Created
August 12, 2013 18:11
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SubmitJob.aspx source
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| <!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2 Final//EN"> | |
| <html xmlns="http://www.w3.org/1999/xhtml"> | |
| <head> | |
| <meta http-equiv="Pragma" content="no-cache" /> | |
| <title>CasJobs</title> | |
| <link href="cjobs.css" rel="stylesheet" /> | |
| <script type="text/javascript" src="scripts/submitjob.js"></script> | |
| <script type="text/javascript" src="scripts/shortcut.js"></script> | |
| <script type="text/javascript" language="JavaScript"> | |
| var queryIsRunning = false; | |
| var editor; | |
| var samplePreview; | |
| var cm; | |
| function completeQuery() { | |
| if (queryIsRunning) { | |
| document.getElementById('message').className = 'happy'; | |
| document.getElementById('message').innerHTML = 'Query complete!'; | |
| showExecButtons(); | |
| setEditorMid(); | |
| queryIsRunning = false; | |
| } | |
| } | |
| function trmenu() { | |
| if (window.frames['resultPane'].document.body.innerHTML.length < 15) | |
| document.getElementById('menuRow').style.display = 'none'; | |
| else { | |
| document.getElementById('menuRow').style.display = ''; | |
| setEditorMid(); | |
| } | |
| } | |
| function onSubmitQueryLoad() { | |
| initEditor(); | |
| initSamplePreview(); | |
| resubmit = document.location.href.indexOf("resubmit") > -1 && document.getElementById('rsqry').innerHTML.length > 0; // || document.location.href.indexOf("sql") > -1; | |
| loadSubmitPage(); | |
| window.onunload = saveSubmitPage; | |
| if (document.getElementById('samples').style.display == 'block') | |
| document.getElementById('sampCheck').checked = true; | |
| editor.focus(); | |
| initHist(); | |
| window.onresize = windowResize; | |
| setSamples(); | |
| initShortCuts(); | |
| } | |
| function initShortCuts() { | |
| shortcut.add("Ctrl+H", setEditorMid); | |
| shortcut.add("Ctrl+J", maxQuery); | |
| shortcut.add("Ctrl+K", maxResults); | |
| shortcut.add("Ctrl+S", checksyntax); | |
| shortcut.add("Ctrl+Q", submitQuickQuery); | |
| shortcut.add("Ctrl+U", submitQuery); | |
| shortcut.add("Ctrl+P", getplan); | |
| shortcut.add("Enter", reindent, { | |
| 'propagate': true | |
| }); | |
| } | |
| function reindent() { | |
| editor.indentLine(editor.getCursor().line); | |
| } | |
| function setSamples() { | |
| var tddl = document.getElementById('targetDDL'); | |
| var context = tddl[tddl.selectedIndex].value; | |
| var tmp = document.getElementById(context.toLowerCase() + "_samples"); | |
| if (!tmp) | |
| tmp = document.getElementById("global_samples"); | |
| document.getElementById('samples').innerHTML = tmp.innerHTML; | |
| } | |
| var lastQry; | |
| var rsThread = null; | |
| var cm; | |
| function windowResize() { | |
| if (rsThread) { | |
| clearTimeout(rsThread); | |
| } else { | |
| lastQry = editor.getValue(); | |
| editor.setValue(''); | |
| cm.style.height = '100%'; | |
| cm.style.width = 'auto'; | |
| } | |
| rsThread = setTimeout(completeResize, 500); | |
| } | |
| function completeResize() { | |
| var osh = cm.offsetHeight; | |
| var osw = cm.offsetWidth; | |
| cm.style.height = osh; | |
| cm.style.width = osw; | |
| editor.setValue(lastQry); | |
| lastQry = null; | |
| rsThread = null; | |
| } | |
| function initEditor() { | |
| var qc = document.getElementById('queryCell'); | |
| editor = CodeMirror(qc, { | |
| lineNumbers: true, | |
| matchBrackets: true, | |
| onCursorActivity: hfloats, | |
| //tabMode: "shift", | |
| tabMode: "indent", | |
| mode: "text/x-tsql" | |
| }); | |
| cm = qc.childNodes[0]; | |
| if (!cm.style) cm = qc.childNodes[1]; | |
| cm.style.height = '100%'; | |
| cm.style.width = 'auto'; | |
| cm.style.padding = '0 0 0 0'; | |
| cm.style.margin = '0 0 0 0'; | |
| cm.style.overflow = 'hidden'; | |
| cm.style.border = 'none'; | |
| windowResize(); | |
| //cm.style.height = cm.offsetHeight - 5; | |
| } | |
| function hfloats() { | |
| hideFloats(); | |
| } | |
| function initSamplePreview() { | |
| var qc = document.getElementById('samplePreviewPane'); | |
| samplePreview = CodeMirror(qc, { | |
| lineNumbers: false, | |
| matchBrackets: false, | |
| readOnly: true, | |
| mode: "text/x-tsql" | |
| }); | |
| } | |
| </script> | |
| <style type="text/css"> | |
| table | |
| { | |
| padding: 0 0 0 0; | |
| margin: 0 0 0 0; | |
| } | |
| </style> | |
| <script src="scripts/codemirror.js"></script> | |
| <script src="scripts/tsql.js"></script> | |
| </head> | |
| <body style="padding: 0 0 0 0; margin: 0 0 0 0" onload="onSubmitQueryLoad();"> | |
| <form name="SubmitJob" id="SubmitJob" action="SubmitJob.aspx" method="post" target="_top" | |
| style="padding: 0 0 0 0; margin: 0 0 0 0"> | |
| <textarea id="rsqry" style="display:none"></textarea> | |
| <input type="hidden" id="queue" name="queue" value="1" style="display: none;" /> | |
| <table cellspacing="0" cellpadding="0" id="mostEverything" style="width: 100%; height: 100%"> | |
| <tr> | |
| <td> | |
| <style type="text/css"> | |
| img { | |
| behavior: url("pngbehavior.htc"); | |
| } | |
| </style> | |
| <link rel="shortcut icon" href="favicon.ico"/> | |
| <div id="div_title" style="background-image: url(img/sdss_back.jpg); background-position: right; | |
| background-repeat: no-repeat; background-color: Black;"> | |
| <table cellpadding="0" cellspacing="0" border="0" width="100%"> | |
| <tr height="73"> | |
| <td> | |
| <a href="http://www.sdss3.org"> | |
| <img border="0" style="width:73;height:60" src="img/sdss3_logo.png"></a></td> | |
| <td height="73" width="100%"> | |
| <a href="default.aspx"> | |
| <img style="border-style: none" src="img/titlebar_left.png" height="73" width="247"></a></td> | |
| <td style="text-align: right;"> | |
| | |
| </td> | |
| </tr> | |
| </table> | |
| </div> | |
| <div id="div_nav"> | |
| <table border="0" cellpadding="0" cellspacing="0" width="100%" style="width: 100%;"> | |
| <tr> | |
| <td align="center"> | |
| <a target="_parent" href="Guide.aspx">Help</a></td> | |
| <td width="60" align="center"> | |
| <a target="_parent" href="casjobscl.aspx">Tools</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="SubmitJob.aspx">Query</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="ViewJobs.aspx">History</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="MyDB.aspx">MyDB</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="TableImport.aspx">Import</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="Groups.aspx">Groups</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="Output.aspx">Output</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="ChangeDetails.aspx">Profile</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="admin.aspx">Queues</a></td> | |
| <td align="center"> | |
| <a target="_blank" href="http://skyserver.sdss3.org">SkyServer</a></td> | |
| <td align="center"> | |
| <a target="_parent" href="logout.aspx">Logout</a></td> | |
| <td style="width: 100%;"> | |
| </td> | |
| <td align="center" style="border-left: none;"> | |
| dstn | |
| </td> | |
| </tr> | |
| </table> | |
| </div> | |
| </td> | |
| </tr> | |
| <tr> | |
| <td> | |
| <table style="width: 100%"> | |
| <tr> | |
| <th class="mover"> | |
| <a href="#" onmouseover="showqsnode('contextHelpDiv');" onmouseout="hideqsnode();">Context</a> | |
| </th> | |
| <th class="mover" style="white-space: nowrap"> | |
| <a href="#" onmouseover="showqsnode('tableHelpDiv');" onmouseout="hideqsnode();">Table | |
| <span style="font-weight: normal" size="-2">(optional)</span></a> | |
| </th> | |
| <th class="mover" style="width: 100%"> | |
| <a href="#" onmouseover="showqsnode('taskNameHelpDiv');" onmouseout="hideqsnode();"> | |
| Task Name</a> | |
| </th> | |
| </tr> | |
| <tr> | |
| <td align="center"> | |
| <select name="targest" id="targetDDL" onchange="setSamples();"> | |
| <option > | |
| MyDB | |
| </option> | |
| <option > | |
| DR10 | |
| </option> | |
| <option > | |
| DR10Collab | |
| </option> | |
| <option > | |
| DR9 | |
| </option> | |
| <option > | |
| TestDR10 | |
| </option> | |
| <option > | |
| DR8 | |
| </option> | |
| <option > | |
| DR7 | |
| </option> | |
| <option > | |
| SEGUE2 | |
| </option> | |
| <option > | |
| GalexGR6 | |
| </option> | |
| <option > | |
| Match2 | |
| </option> | |
| <option > | |
| MatchDB | |
| </option> | |
| <option > | |
| DR4 | |
| </option> | |
| <option > | |
| DR3 | |
| </option> | |
| <option > | |
| DR2 | |
| </option> | |
| <option > | |
| DR1 | |
| </option> | |
| <option > | |
| GalexGR5 | |
| </option> | |
| <option > | |
| DR6 | |
| </option> | |
| <option > | |
| sensor4 | |
| </option> | |
| <option > | |
| sensor | |
| </option> | |
| <option > | |
| 2MASS | |
| </option> | |
| <option > | |
| GalexGR2 | |
| </option> | |
| <option > | |
| GalexGR3 | |
| </option> | |
| <option > | |
| FIRST | |
| </option> | |
| <option > | |
| DR5 | |
| </option> | |
| <option > | |
| ROSAT | |
| </option> | |
| <option > | |
| TestDR9 | |
| </option> | |
| <option > | |
| 2DF | |
| </option> | |
| </select> | |
| </td> | |
| <td align="center" style="width: 100px"> | |
| <input type="text" style="width: 100%" id="table" name="table" value="MyTable_0" /> | |
| </td> | |
| <td align="center"> | |
| <input type="text" name="taskname" style="width: 100%" value="My Query" /> | |
| </td> | |
| </tr> | |
| </table> | |
| </td> | |
| </tr> | |
| <tr> | |
| <td> | |
| <table id="querypane" cellspacing="1" cellpadding="0" class="bar" style="padding: 0 0 0 0; | |
| width: 100%;"> | |
| <tr> | |
| <td style="text-align: center;"> | |
| <input id="sampCheck" type="button" value="Samples" onclick="toggleSamples();" /> | |
| </td> | |
| <td style="text-align: center;"> | |
| <input id="histCheck" type="button" value="Recent" onclick="toggleHist();" /> | |
| </td> | |
| <td style="text-align: center;"> | |
| <input id="clearButton" type="button" onclick="clearQry();" value="Clear" /> | |
| </td> | |
| <td> | |
| </td> | |
| <td style="padding: 0 5 0 5; width: 25;"> | |
| <div style="white-space: nowrap" id="timer"> | |
| </div> | |
| </td> | |
| <td width="100%"> | |
| <div class="message" style="text-align: right; padding-right: 5; height: 15px; overflow: hidden;" | |
| onmouseover="cjshowqsM();" onmouseout="cjhideqsM();" id="message"> | |
| </div> | |
| <div style="visibility: hidden; z-index: 100; position: absolute;" id="mmessage"> | |
| </div> | |
| </td> | |
| <td style="text-align: center;"> | |
| <input type="hidden" id="syntax" name="syntax" value="false" /> | |
| <input id="syntaxButton" title="Check query syntax. (CTRL-S)" type="button" value="Syntax" | |
| onclick="checksyntax()" /> | |
| </td> | |
| <td style="text-align: center;"> | |
| <input id="planButton" title="Show estimated query plan. (CTRL-P)" type="button" value="Plan" | |
| onclick="getplan();" /> | |
| </td> | |
| <td style="text-align: center;"> | |
| <input id="quickButton" title="Runs the query instantaneously. Short duration and data limit. (CTRL-Q)" | |
| value="Quick" type="button" onclick="submitQuickQuery();" /> | |
| </td> | |
| <td style="text-align: center"> | |
| <input id="submitButton" value="Submit" title="Submits your query. Longest duration. (CTRL-U)" | |
| type="button" onclick="submitQuery();" /> | |
| </td> | |
| </tr> | |
| </table> | |
| </td> | |
| </tr> | |
| <tr id="queryRow"> | |
| <td id="queryCell" height="100%" style="padding: 0 1 1 0;"> | |
| </td> | |
| </tr> | |
| <tr id="resultsRow" style="display: none;"> | |
| <td id="resultsCell" width="100%" height="65%"> | |
| <iframe name="resultPane" id="resultPane" height="100%" style="height: 100%; width: 100%" | |
| src="output/vodataclean.aspx" frameborder="0" onload="trmenu();" scrolling="auto"> | |
| </iframe> | |
| </td> | |
| </tr> | |
| <tr id="menuRow"> | |
| <td> | |
| <table class="bar" id="windowMenu" cellpadding="0" cellspacing="1" border="0" style="width: 100%;"> | |
| <tr> | |
| <td style="font-variant: small-caps; padding: 0 10 0 10"> | |
| Results | |
| </td> | |
| <td> | |
| <input type="button" value="Plot" onclick="window.open('output/voplot/loadjvt.aspx','plot','');" /> | |
| </td> | |
| <td> | |
| <input type="button" value="Save As" onclick="save();" /> | |
| </td> | |
| <td> | |
| <select id="ddl"> | |
| <option>HTML</option> | |
| <option>CSV</option> | |
| <option>VOTable</option> | |
| <option>DataSet</option> | |
| </select> | |
| </td> | |
| <td width="100%"> | |
| | |
| </td> | |
| <td style="padding-right: 5;"> | |
| </td> | |
| <td style="font-variant: small-caps; padding: 0 10 0 10"> | |
| Display | |
| </td> | |
| <td> | |
| <input type="button" title="CTRL-J" value="Query" onclick="maxQuery();" /> | |
| </td> | |
| <td> | |
| <input type="button" title="CTRL-K" value="Results" onclick="maxResults();" /> | |
| </td> | |
| <td> | |
| <input type="button" title="CTRL-H" value="Both" onclick="setEditorMid();" /> | |
| </td> | |
| </tr> | |
| </table> | |
| </td> | |
| </tr> | |
| <tr> | |
| <td style=""> | |
| <p class="footer" style="padding:2 2 2 2;margin:0 0 0 0;"> | |
| <a href="http://skyserver.sdss3.org/contact/default.asp?subject=CasJobs+Issue:+&smtp=mail.pha.jhu.edu&helpdesk=helpdesk@sdss3.org&url=http%3a%2f%2fskyservice.pha.jhu.edu%2fcasjobs%2fSubmitJob.aspx&username=Dustin+Lang&userid=dstn &email=dstn@astro.princeton.edu">Contact</a> | |
| <br/> | |
| v3_8_4 | |
| </p> | |
| </td> | |
| </tr> | |
| </table> | |
| </form> | |
| <form name="svqry" id="Form1" action="output/svqry.aspx" method="post" target="hidden" | |
| style="display: none;"> | |
| <input type="hidden" name="USQL" id="USQL" value="" /> | |
| <input type="hidden" name="UCONTEXT" id="UCONTEXT" value="" /> | |
| </form> | |
| <iframe name="hidden" style="display: none"></iframe> | |
| <input type="hidden" id="wsid" value="2092080249" /> | |
| <div id="samples" style="position: absolute; display: none; width: 200; vertical-align: text-top; | |
| overflow: auto; z-index: 100; padding: 2 2 2 2;" class="transparent" > | |
| </div> | |
| <div id="all_samples" style="display:none;"> | |
| <div id="global_samples"> | |
| <div><a href="#" onclick="setQuery('q_377384944');" onmouseover="showSample('q_377384944',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_1917342500');" onmouseover="showSample('q_1917342500',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_199934847');" onmouseover="showSample('q_199934847',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1794636122');" onmouseover="showSample('q_1794636122',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_2053263464');" onmouseover="showSample('q_2053263464',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_610026851');" onmouseover="showSample('q_610026851',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_347053935');" onmouseover="showSample('q_347053935',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1503241840');" onmouseover="showSample('q_1503241840',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1093157909');" onmouseover="showSample('q_1093157909',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1182730545');" onmouseover="showSample('q_1182730545',this);" onmouseout="cjhideqs();">Galaxies By Emission Lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1884957360');" onmouseover="showSample('q_1884957360',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_1314337809');" onmouseover="showSample('q_1314337809',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_453086348');" onmouseover="showSample('q_453086348',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_704206862');" onmouseover="showSample('q_704206862',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_689961383');" onmouseover="showSample('q_689961383',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_410365955');" onmouseover="showSample('q_410365955',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1684523170');" onmouseover="showSample('q_1684523170',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1823934513');" onmouseover="showSample('q_1823934513',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_348348979');" onmouseover="showSample('q_348348979',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_569145814');" onmouseover="showSample('q_569145814',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1687216546');" onmouseover="showSample('q_1687216546',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_113893222');" onmouseover="showSample('q_113893222',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1471444940');" onmouseover="showSample('q_1471444940',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1092529461');" onmouseover="showSample('q_1092529461',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1476423508');" onmouseover="showSample('q_1476423508',this);" onmouseout="cjhideqs();">Spectra of Red Stars</a></div> | |
| <div><a href="#" onclick="setQuery('q_1964088379');" onmouseover="showSample('q_1964088379',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1609807292');" onmouseover="showSample('q_1609807292',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_949416951');" onmouseover="showSample('q_949416951',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_1820036051');" onmouseover="showSample('q_1820036051',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_2086102066');" onmouseover="showSample('q_2086102066',this);" onmouseout="cjhideqs();">Multiple Detections and Time Series</a></div> | |
| </div> | |
| <div id="batchadmin_samples"> | |
| <div><a href="#" onclick="setQuery('q_1342567403');" onmouseover="showSample('q_1342567403',this);" onmouseout="cjhideqs();">Queries longer than 10min</a></div> | |
| <div><a href="#" onclick="setQuery('q_1185292591');" onmouseover="showSample('q_1185292591',this);" onmouseout="cjhideqs();">Accounts created monthly</a></div> | |
| </div> | |
| <div id="dr1_samples"> | |
| <div><a href="#" onclick="setQuery('q_2127032053');" onmouseover="showSample('q_2127032053',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_1822251911');" onmouseover="showSample('q_1822251911',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_2112964880');" onmouseover="showSample('q_2112964880',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1876103269');" onmouseover="showSample('q_1876103269',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1604660031');" onmouseover="showSample('q_1604660031',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1209894154');" onmouseover="showSample('q_1209894154',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1732295176');" onmouseover="showSample('q_1732295176',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_2122410695');" onmouseover="showSample('q_2122410695',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_162421342');" onmouseover="showSample('q_162421342',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1947188265');" onmouseover="showSample('q_1947188265',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_1076082999');" onmouseover="showSample('q_1076082999',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_362452986');" onmouseover="showSample('q_362452986',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_2140829941');" onmouseover="showSample('q_2140829941',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1307734809');" onmouseover="showSample('q_1307734809',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_699861840');" onmouseover="showSample('q_699861840',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1448724282');" onmouseover="showSample('q_1448724282',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1373505727');" onmouseover="showSample('q_1373505727',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_203899950');" onmouseover="showSample('q_203899950',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_160825834');" onmouseover="showSample('q_160825834',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_1984607857');" onmouseover="showSample('q_1984607857',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_2071057527');" onmouseover="showSample('q_2071057527',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1616963259');" onmouseover="showSample('q_1616963259',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1224142175');" onmouseover="showSample('q_1224142175',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_733458258');" onmouseover="showSample('q_733458258',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1195635002');" onmouseover="showSample('q_1195635002',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_792880405');" onmouseover="showSample('q_792880405',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1564994359');" onmouseover="showSample('q_1564994359',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_491051768');" onmouseover="showSample('q_491051768',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_453518089');" onmouseover="showSample('q_453518089',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_1011044940');" onmouseover="showSample('q_1011044940',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1835462071');" onmouseover="showSample('q_1835462071',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_715981218');" onmouseover="showSample('q_715981218',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1104283183');" onmouseover="showSample('q_1104283183',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_1837021711');" onmouseover="showSample('q_1837021711',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_2135502459');" onmouseover="showSample('q_2135502459',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_114193719');" onmouseover="showSample('q_114193719',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr10_samples"> | |
| <div><a href="#" onclick="setQuery('q_318573181');" onmouseover="showSample('q_318573181',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_2121526033');" onmouseover="showSample('q_2121526033',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1702999202');" onmouseover="showSample('q_1702999202',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_807954861');" onmouseover="showSample('q_807954861',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_1601839065');" onmouseover="showSample('q_1601839065',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1407015576');" onmouseover="showSample('q_1407015576',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_810186038');" onmouseover="showSample('q_810186038',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_446289279');" onmouseover="showSample('q_446289279',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_832506840');" onmouseover="showSample('q_832506840',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1549577480');" onmouseover="showSample('q_1549577480',this);" onmouseout="cjhideqs();">Galaxies By Emission Lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1075597663');" onmouseover="showSample('q_1075597663',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_387047336');" onmouseover="showSample('q_387047336',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_464249349');" onmouseover="showSample('q_464249349',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1257775135');" onmouseover="showSample('q_1257775135',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1773962834');" onmouseover="showSample('q_1773962834',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1890051708');" onmouseover="showSample('q_1890051708',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_2042342521');" onmouseover="showSample('q_2042342521',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1271476914');" onmouseover="showSample('q_1271476914',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_162268584');" onmouseover="showSample('q_162268584',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_200158383');" onmouseover="showSample('q_200158383',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_220572073');" onmouseover="showSample('q_220572073',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_454660149');" onmouseover="showSample('q_454660149',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1221376687');" onmouseover="showSample('q_1221376687',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_663779516');" onmouseover="showSample('q_663779516',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_338186821');" onmouseover="showSample('q_338186821',this);" onmouseout="cjhideqs();">Spectra of Red Stars</a></div> | |
| <div><a href="#" onclick="setQuery('q_284125386');" onmouseover="showSample('q_284125386',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1363234497');" onmouseover="showSample('q_1363234497',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_911927524');" onmouseover="showSample('q_911927524',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_2046113808');" onmouseover="showSample('q_2046113808',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1348920221');" onmouseover="showSample('q_1348920221',this);" onmouseout="cjhideqs();">Multiple Detections and Time Series</a></div> | |
| <div><a href="#" onclick="setQuery('q_619277145');" onmouseover="showSample('q_619277145',this);" onmouseout="cjhideqs();">All APOGEE Plate Visits</a></div> | |
| <div><a href="#" onclick="setQuery('q_1575944052');" onmouseover="showSample('q_1575944052',this);" onmouseout="cjhideqs();">ASPCAP Parameters and Errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_873427785');" onmouseover="showSample('q_873427785',this);" onmouseout="cjhideqs();">APOGEE Stars No BAD Flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_509946294');" onmouseover="showSample('q_509946294',this);" onmouseout="cjhideqs();">ASPCAP Params for Cluster Mbrs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1886714918');" onmouseover="showSample('q_1886714918',this);" onmouseout="cjhideqs();">APOGEE Proper Motions</a></div> | |
| <div><a href="#" onclick="setQuery('q_214541362');" onmouseover="showSample('q_214541362',this);" onmouseout="cjhideqs();">APOGEE Stars Near Cluster Ctr</a></div> | |
| <div><a href="#" onclick="setQuery('q_114253696');" onmouseover="showSample('q_114253696',this);" onmouseout="cjhideqs();">RVs for Individual APOGEE Visits</a></div> | |
| <div><a href="#" onclick="setQuery('q_286757891');" onmouseover="showSample('q_286757891',this);" onmouseout="cjhideqs();">APOGEE and SEGUE Spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_251526975');" onmouseover="showSample('q_251526975',this);" onmouseout="cjhideqs();">SDSS Photometry for APOGEE Stars</a></div> | |
| </div> | |
| <div id="dr10collab_samples"> | |
| <div><a href="#" onclick="setQuery('q_341160974');" onmouseover="showSample('q_341160974',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_2088747594');" onmouseover="showSample('q_2088747594',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_326961301');" onmouseover="showSample('q_326961301',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1559254220');" onmouseover="showSample('q_1559254220',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_364596238');" onmouseover="showSample('q_364596238',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1145250273');" onmouseover="showSample('q_1145250273',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_965086605');" onmouseover="showSample('q_965086605',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_893526326');" onmouseover="showSample('q_893526326',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1359629897');" onmouseover="showSample('q_1359629897',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_2046520797');" onmouseover="showSample('q_2046520797',this);" onmouseout="cjhideqs();">Galaxies By Emission Lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1722069906');" onmouseover="showSample('q_1722069906',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_504267227');" onmouseover="showSample('q_504267227',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_273521898');" onmouseover="showSample('q_273521898',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1145880200');" onmouseover="showSample('q_1145880200',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1019525219');" onmouseover="showSample('q_1019525219',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_891488825');" onmouseover="showSample('q_891488825',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1456890876');" onmouseover="showSample('q_1456890876',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1683900573');" onmouseover="showSample('q_1683900573',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_538248463');" onmouseover="showSample('q_538248463',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_2107503000');" onmouseover="showSample('q_2107503000',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1724772452');" onmouseover="showSample('q_1724772452',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_34323696');" onmouseover="showSample('q_34323696',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_357369514');" onmouseover="showSample('q_357369514',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_2085753961');" onmouseover="showSample('q_2085753961',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1598688566');" onmouseover="showSample('q_1598688566',this);" onmouseout="cjhideqs();">Spectra of Red Stars</a></div> | |
| <div><a href="#" onclick="setQuery('q_1031426103');" onmouseover="showSample('q_1031426103',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_907308906');" onmouseover="showSample('q_907308906',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1246974053');" onmouseover="showSample('q_1246974053',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_1446002135');" onmouseover="showSample('q_1446002135',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_45055564');" onmouseover="showSample('q_45055564',this);" onmouseout="cjhideqs();">Multiple Detections and Time Series</a></div> | |
| <div><a href="#" onclick="setQuery('q_1674347198');" onmouseover="showSample('q_1674347198',this);" onmouseout="cjhideqs();">All APOGEE Plate Visits</a></div> | |
| <div><a href="#" onclick="setQuery('q_29000041');" onmouseover="showSample('q_29000041',this);" onmouseout="cjhideqs();">ASPCAP Parameters and Errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1193882752');" onmouseover="showSample('q_1193882752',this);" onmouseout="cjhideqs();">APOGEE Stars No BAD Flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_1745805745');" onmouseover="showSample('q_1745805745',this);" onmouseout="cjhideqs();">ASPCAP Params for Cluster Mbrs</a></div> | |
| <div><a href="#" onclick="setQuery('q_111582421');" onmouseover="showSample('q_111582421',this);" onmouseout="cjhideqs();">APOGEE Proper Motions</a></div> | |
| <div><a href="#" onclick="setQuery('q_1441850959');" onmouseover="showSample('q_1441850959',this);" onmouseout="cjhideqs();">APOGEE Stars Near Cluster Ctr</a></div> | |
| <div><a href="#" onclick="setQuery('q_988146083');" onmouseover="showSample('q_988146083',this);" onmouseout="cjhideqs();">RVs for Individual APOGEE Visits</a></div> | |
| <div><a href="#" onclick="setQuery('q_197092168');" onmouseover="showSample('q_197092168',this);" onmouseout="cjhideqs();">APOGEE and SEGUE Spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_871745526');" onmouseover="showSample('q_871745526',this);" onmouseout="cjhideqs();">SDSS Photometry for APOGEE Stars</a></div> | |
| </div> | |
| <div id="dr2_samples"> | |
| <div><a href="#" onclick="setQuery('q_658663612');" onmouseover="showSample('q_658663612',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_2046242728');" onmouseover="showSample('q_2046242728',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_100466571');" onmouseover="showSample('q_100466571',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_473336052');" onmouseover="showSample('q_473336052',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1038272356');" onmouseover="showSample('q_1038272356',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1673976505');" onmouseover="showSample('q_1673976505',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1262886835');" onmouseover="showSample('q_1262886835',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1206688596');" onmouseover="showSample('q_1206688596',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1341462147');" onmouseover="showSample('q_1341462147',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1497461636');" onmouseover="showSample('q_1497461636',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_166620452');" onmouseover="showSample('q_166620452',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_605771979');" onmouseover="showSample('q_605771979',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_384152764');" onmouseover="showSample('q_384152764',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_239583990');" onmouseover="showSample('q_239583990',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_513883755');" onmouseover="showSample('q_513883755',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_123633451');" onmouseover="showSample('q_123633451',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_964285562');" onmouseover="showSample('q_964285562',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1428429823');" onmouseover="showSample('q_1428429823',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1014719417');" onmouseover="showSample('q_1014719417',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_955083894');" onmouseover="showSample('q_955083894',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_2067166502');" onmouseover="showSample('q_2067166502',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1081925782');" onmouseover="showSample('q_1081925782',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1379940380');" onmouseover="showSample('q_1379940380',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_5571651');" onmouseover="showSample('q_5571651',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_284612279');" onmouseover="showSample('q_284612279',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1514959216');" onmouseover="showSample('q_1514959216',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1269992360');" onmouseover="showSample('q_1269992360',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1619536327');" onmouseover="showSample('q_1619536327',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_234499396');" onmouseover="showSample('q_234499396',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_386537157');" onmouseover="showSample('q_386537157',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_506396296');" onmouseover="showSample('q_506396296',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1230693149');" onmouseover="showSample('q_1230693149',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_2026053022');" onmouseover="showSample('q_2026053022',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_643163052');" onmouseover="showSample('q_643163052',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1483607040');" onmouseover="showSample('q_1483607040',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_1458312124');" onmouseover="showSample('q_1458312124',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr3_samples"> | |
| <div><a href="#" onclick="setQuery('q_998698239');" onmouseover="showSample('q_998698239',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_324753475');" onmouseover="showSample('q_324753475',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_638887334');" onmouseover="showSample('q_638887334',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1942123503');" onmouseover="showSample('q_1942123503',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1122950537');" onmouseover="showSample('q_1122950537',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_203970260');" onmouseover="showSample('q_203970260',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_155362706');" onmouseover="showSample('q_155362706',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_2008048623');" onmouseover="showSample('q_2008048623',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_468185944');" onmouseover="showSample('q_468185944',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1741581729');" onmouseover="showSample('q_1741581729',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_293030657');" onmouseover="showSample('q_293030657',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_50066576');" onmouseover="showSample('q_50066576',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_1227312257');" onmouseover="showSample('q_1227312257',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1009123441');" onmouseover="showSample('q_1009123441',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_97947386');" onmouseover="showSample('q_97947386',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1715812784');" onmouseover="showSample('q_1715812784',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1301593803');" onmouseover="showSample('q_1301593803',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1729284068');" onmouseover="showSample('q_1729284068',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1709778956');" onmouseover="showSample('q_1709778956',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_1346173317');" onmouseover="showSample('q_1346173317',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_874416063');" onmouseover="showSample('q_874416063',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1426553339');" onmouseover="showSample('q_1426553339',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_2092933015');" onmouseover="showSample('q_2092933015',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_2046005064');" onmouseover="showSample('q_2046005064',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1937139908');" onmouseover="showSample('q_1937139908',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1071911477');" onmouseover="showSample('q_1071911477',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1639576493');" onmouseover="showSample('q_1639576493',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_2052665602');" onmouseover="showSample('q_2052665602',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1227456513');" onmouseover="showSample('q_1227456513',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_1795100394');" onmouseover="showSample('q_1795100394',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1993463533');" onmouseover="showSample('q_1993463533',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_477859480');" onmouseover="showSample('q_477859480',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1558845305');" onmouseover="showSample('q_1558845305',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_30651545');" onmouseover="showSample('q_30651545',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_598412421');" onmouseover="showSample('q_598412421',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_834106047');" onmouseover="showSample('q_834106047',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr4_samples"> | |
| <div><a href="#" onclick="setQuery('q_190266330');" onmouseover="showSample('q_190266330',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_399748022');" onmouseover="showSample('q_399748022',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_168487273');" onmouseover="showSample('q_168487273',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1315505534');" onmouseover="showSample('q_1315505534',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1675888762');" onmouseover="showSample('q_1675888762',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1650901083');" onmouseover="showSample('q_1650901083',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_763893289');" onmouseover="showSample('q_763893289',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1725633998');" onmouseover="showSample('q_1725633998',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1178472613');" onmouseover="showSample('q_1178472613',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_828709702');" onmouseover="showSample('q_828709702',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_1055252390');" onmouseover="showSample('q_1055252390',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_791936939');" onmouseover="showSample('q_791936939',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_224126374');" onmouseover="showSample('q_224126374',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_388139904');" onmouseover="showSample('q_388139904',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_915208631');" onmouseover="showSample('q_915208631',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_98652983');" onmouseover="showSample('q_98652983',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_2027172584');" onmouseover="showSample('q_2027172584',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_730255691');" onmouseover="showSample('q_730255691',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1691326363');" onmouseover="showSample('q_1691326363',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_1324808024');" onmouseover="showSample('q_1324808024',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_51406064');" onmouseover="showSample('q_51406064',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1713458572');" onmouseover="showSample('q_1713458572',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_70783942');" onmouseover="showSample('q_70783942',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1804705991');" onmouseover="showSample('q_1804705991',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_167002323');" onmouseover="showSample('q_167002323',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_834596942');" onmouseover="showSample('q_834596942',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1424444742');" onmouseover="showSample('q_1424444742',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_175511087');" onmouseover="showSample('q_175511087',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1053909050');" onmouseover="showSample('q_1053909050',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_622853371');" onmouseover="showSample('q_622853371',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_510380354');" onmouseover="showSample('q_510380354',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_963813061');" onmouseover="showSample('q_963813061',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_23925016');" onmouseover="showSample('q_23925016',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_1398357282');" onmouseover="showSample('q_1398357282',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1944663326');" onmouseover="showSample('q_1944663326',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_166816670');" onmouseover="showSample('q_166816670',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr5_samples"> | |
| <div><a href="#" onclick="setQuery('q_314022943');" onmouseover="showSample('q_314022943',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_2121237275');" onmouseover="showSample('q_2121237275',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_706908036');" onmouseover="showSample('q_706908036',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1510674311');" onmouseover="showSample('q_1510674311',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_342684245');" onmouseover="showSample('q_342684245',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1821885322');" onmouseover="showSample('q_1821885322',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_654356252');" onmouseover="showSample('q_654356252',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_420853709');" onmouseover="showSample('q_420853709',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_631175478');" onmouseover="showSample('q_631175478',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1165868693');" onmouseover="showSample('q_1165868693',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_1514903499');" onmouseover="showSample('q_1514903499',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_214576614');" onmouseover="showSample('q_214576614',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_619033119');" onmouseover="showSample('q_619033119',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1653404421');" onmouseover="showSample('q_1653404421',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1527039772');" onmouseover="showSample('q_1527039772',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1055015502');" onmouseover="showSample('q_1055015502',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1131150381');" onmouseover="showSample('q_1131150381',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_859289958');" onmouseover="showSample('q_859289958',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1033172010');" onmouseover="showSample('q_1033172010',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_976449187');" onmouseover="showSample('q_976449187',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1404790795');" onmouseover="showSample('q_1404790795',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1368831015');" onmouseover="showSample('q_1368831015',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_642208693');" onmouseover="showSample('q_642208693',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_674238270');" onmouseover="showSample('q_674238270',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1020817074');" onmouseover="showSample('q_1020817074',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1695980969');" onmouseover="showSample('q_1695980969',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1794028875');" onmouseover="showSample('q_1794028875',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_875447540');" onmouseover="showSample('q_875447540',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_408046859');" onmouseover="showSample('q_408046859',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_2023911456');" onmouseover="showSample('q_2023911456',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1739829469');" onmouseover="showSample('q_1739829469',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1716646730');" onmouseover="showSample('q_1716646730',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_856840643');" onmouseover="showSample('q_856840643',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_211714083');" onmouseover="showSample('q_211714083',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_137356135');" onmouseover="showSample('q_137356135',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_1480779043');" onmouseover="showSample('q_1480779043',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr6_samples"> | |
| <div><a href="#" onclick="setQuery('q_1195248688');" onmouseover="showSample('q_1195248688',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_1747257364');" onmouseover="showSample('q_1747257364',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1374627809');" onmouseover="showSample('q_1374627809',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1381525768');" onmouseover="showSample('q_1381525768',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_909071920');" onmouseover="showSample('q_909071920',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1357802971');" onmouseover="showSample('q_1357802971',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1954141537');" onmouseover="showSample('q_1954141537',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_545014296');" onmouseover="showSample('q_545014296',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_547865327');" onmouseover="showSample('q_547865327',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_716142064');" onmouseover="showSample('q_716142064',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_272200048');" onmouseover="showSample('q_272200048',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_753648351');" onmouseover="showSample('q_753648351',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_1150951472');" onmouseover="showSample('q_1150951472',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_106085622');" onmouseover="showSample('q_106085622',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1713017857');" onmouseover="showSample('q_1713017857',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_270075329');" onmouseover="showSample('q_270075329',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1540370546');" onmouseover="showSample('q_1540370546',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_365239915');" onmouseover="showSample('q_365239915',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_179278427');" onmouseover="showSample('q_179278427',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_2005973150');" onmouseover="showSample('q_2005973150',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1400899770');" onmouseover="showSample('q_1400899770',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1330058026');" onmouseover="showSample('q_1330058026',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1048676048');" onmouseover="showSample('q_1048676048',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_53648337');" onmouseover="showSample('q_53648337',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1793902941');" onmouseover="showSample('q_1793902941',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1876907516');" onmouseover="showSample('q_1876907516',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1499026876');" onmouseover="showSample('q_1499026876',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_253037019');" onmouseover="showSample('q_253037019',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_627065552');" onmouseover="showSample('q_627065552',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_873473743');" onmouseover="showSample('q_873473743',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1226072052');" onmouseover="showSample('q_1226072052',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1201934799');" onmouseover="showSample('q_1201934799',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1778610482');" onmouseover="showSample('q_1778610482',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_2026496616');" onmouseover="showSample('q_2026496616',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_813213932');" onmouseover="showSample('q_813213932',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_1470069848');" onmouseover="showSample('q_1470069848',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr7_samples"> | |
| <div><a href="#" onclick="setQuery('q_1442356757');" onmouseover="showSample('q_1442356757',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_25768111');" onmouseover="showSample('q_25768111',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_836207046');" onmouseover="showSample('q_836207046',this);" onmouseout="cjhideqs();">Unclassified spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_1444654077');" onmouseover="showSample('q_1444654077',this);" onmouseout="cjhideqs();">Galaxies multiple criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_824393739');" onmouseover="showSample('q_824393739',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1467158080');" onmouseover="showSample('q_1467158080',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_922576218');" onmouseover="showSample('q_922576218',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_256345731');" onmouseover="showSample('q_256345731',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1261782764');" onmouseover="showSample('q_1261782764',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1772065995');" onmouseover="showSample('q_1772065995',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_731851157');" onmouseover="showSample('q_731851157',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_197942948');" onmouseover="showSample('q_197942948',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_307791979');" onmouseover="showSample('q_307791979',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_663453829');" onmouseover="showSample('q_663453829',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1970118298');" onmouseover="showSample('q_1970118298',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1322104004');" onmouseover="showSample('q_1322104004',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_488717385');" onmouseover="showSample('q_488717385',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_666094160');" onmouseover="showSample('q_666094160',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1391190496');" onmouseover="showSample('q_1391190496',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_12263065');" onmouseover="showSample('q_12263065',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1540682795');" onmouseover="showSample('q_1540682795',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1674685583');" onmouseover="showSample('q_1674685583',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_335683413');" onmouseover="showSample('q_335683413',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1986785076');" onmouseover="showSample('q_1986785076',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_279312168');" onmouseover="showSample('q_279312168',this);" onmouseout="cjhideqs();">Galaxies by spectra</a></div> | |
| <div><a href="#" onclick="setQuery('q_168810913');" onmouseover="showSample('q_168810913',this);" onmouseout="cjhideqs();">Galaxies by spectra2</a></div> | |
| <div><a href="#" onclick="setQuery('q_1868611009');" onmouseover="showSample('q_1868611009',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_686166294');" onmouseover="showSample('q_686166294',this);" onmouseout="cjhideqs();">QSOs broadlines near galaxy</a></div> | |
| <div><a href="#" onclick="setQuery('q_2089021461');" onmouseover="showSample('q_2089021461',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_535089494');" onmouseover="showSample('q_535089494',this);" onmouseout="cjhideqs();">Ellipticals odd lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1581828007');" onmouseover="showSample('q_1581828007',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1954768468');" onmouseover="showSample('q_1954768468',this);" onmouseout="cjhideqs();">Broadest spectral lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_1311402765');" onmouseover="showSample('q_1311402765',this);" onmouseout="cjhideqs();">Gridded galaxy counts</a></div> | |
| <div><a href="#" onclick="setQuery('q_1594656083');" onmouseover="showSample('q_1594656083',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1399733903');" onmouseover="showSample('q_1399733903',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_532479277');" onmouseover="showSample('q_532479277',this);" onmouseout="cjhideqs();">Checking SDSS footprint</a></div> | |
| </div> | |
| <div id="dr8_samples"> | |
| <div><a href="#" onclick="setQuery('q_1774811490');" onmouseover="showSample('q_1774811490',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_1950906038');" onmouseover="showSample('q_1950906038',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_118442681');" onmouseover="showSample('q_118442681',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_1087655456');" onmouseover="showSample('q_1087655456',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_1315557362');" onmouseover="showSample('q_1315557362',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_671661625');" onmouseover="showSample('q_671661625',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_474354453');" onmouseover="showSample('q_474354453',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_765492618');" onmouseover="showSample('q_765492618',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_453245167');" onmouseover="showSample('q_453245167',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1745962591');" onmouseover="showSample('q_1745962591',this);" onmouseout="cjhideqs();">Galaxies By Emission Lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_23566870');" onmouseover="showSample('q_23566870',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_225105383');" onmouseover="showSample('q_225105383',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_834528110');" onmouseover="showSample('q_834528110',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_245836436');" onmouseover="showSample('q_245836436',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1952789469');" onmouseover="showSample('q_1952789469',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1577813389');" onmouseover="showSample('q_1577813389',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1362554404');" onmouseover="showSample('q_1362554404',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1335992021');" onmouseover="showSample('q_1335992021',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_999622185');" onmouseover="showSample('q_999622185',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_416441924');" onmouseover="showSample('q_416441924',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_2043177420');" onmouseover="showSample('q_2043177420',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_538360056');" onmouseover="showSample('q_538360056',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1596667058');" onmouseover="showSample('q_1596667058',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1317231909');" onmouseover="showSample('q_1317231909',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1838668250');" onmouseover="showSample('q_1838668250',this);" onmouseout="cjhideqs();">Spectra of Red Stars</a></div> | |
| <div><a href="#" onclick="setQuery('q_2014769771');" onmouseover="showSample('q_2014769771',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1687012106');" onmouseover="showSample('q_1687012106',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1632881509');" onmouseover="showSample('q_1632881509',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_103654135');" onmouseover="showSample('q_103654135',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_675428088');" onmouseover="showSample('q_675428088',this);" onmouseout="cjhideqs();">Multiple Detections and Time Series</a></div> | |
| </div> | |
| <div id="dr9_samples"> | |
| <div><a href="#" onclick="setQuery('q_1651054877');" onmouseover="showSample('q_1651054877',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_229416785');" onmouseover="showSample('q_229416785',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_639018260');" onmouseover="showSample('q_639018260',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_906922939');" onmouseover="showSample('q_906922939',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_1646205417');" onmouseover="showSample('q_1646205417',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_150519266');" onmouseover="showSample('q_150519266',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_943895088');" onmouseover="showSample('q_943895088',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1380995089');" onmouseover="showSample('q_1380995089',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_2032074038');" onmouseover="showSample('q_2032074038',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_77418842');" onmouseover="showSample('q_77418842',this);" onmouseout="cjhideqs();">Galaxies By Emission Lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_436084239');" onmouseover="showSample('q_436084239',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_352254942');" onmouseover="showSample('q_352254942',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_1677687603');" onmouseover="showSample('q_1677687603',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1019428081');" onmouseover="showSample('q_1019428081',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_1340958328');" onmouseover="showSample('q_1340958328',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1563485422');" onmouseover="showSample('q_1563485422',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_466532201');" onmouseover="showSample('q_466532201',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1381126224');" onmouseover="showSample('q_1381126224',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_570846738');" onmouseover="showSample('q_570846738',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_1884815287');" onmouseover="showSample('q_1884815287',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_689792689');" onmouseover="showSample('q_689792689',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_193732499');" onmouseover="showSample('q_193732499',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_883674423');" onmouseover="showSample('q_883674423',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_498791126');" onmouseover="showSample('q_498791126',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_620022539');" onmouseover="showSample('q_620022539',this);" onmouseout="cjhideqs();">Spectra of Red Stars</a></div> | |
| <div><a href="#" onclick="setQuery('q_1606095120');" onmouseover="showSample('q_1606095120',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_2056596239');" onmouseover="showSample('q_2056596239',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1200129878');" onmouseover="showSample('q_1200129878',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_1036893522');" onmouseover="showSample('q_1036893522',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_1368842829');" onmouseover="showSample('q_1368842829',this);" onmouseout="cjhideqs();">Multiple Detections and Time Series</a></div> | |
| </div> | |
| <div id="dr9collab_samples"> | |
| <div><a href="#" onclick="setQuery('q_442485668');" onmouseover="showSample('q_442485668',this);" onmouseout="cjhideqs();">Basic SELECT FROM WHERE</a></div> | |
| <div><a href="#" onclick="setQuery('q_2039614472');" onmouseover="showSample('q_2039614472',this);" onmouseout="cjhideqs();">Galaxies two criteria</a></div> | |
| <div><a href="#" onclick="setQuery('q_1763264299');" onmouseover="showSample('q_1763264299',this);" onmouseout="cjhideqs();">QSOs in spectroscopy</a></div> | |
| <div><a href="#" onclick="setQuery('q_2013120862');" onmouseover="showSample('q_2013120862',this);" onmouseout="cjhideqs();">Using BETWEEN</a></div> | |
| <div><a href="#" onclick="setQuery('q_930225692');" onmouseover="showSample('q_930225692',this);" onmouseout="cjhideqs();">Spatial unit vectors</a></div> | |
| <div><a href="#" onclick="setQuery('q_129227591');" onmouseover="showSample('q_129227591',this);" onmouseout="cjhideqs();">CVs using colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1795754421');" onmouseover="showSample('q_1795754421',this);" onmouseout="cjhideqs();">Data subsample</a></div> | |
| <div><a href="#" onclick="setQuery('q_787192452');" onmouseover="showSample('q_787192452',this);" onmouseout="cjhideqs();">Low z QSOs by colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_268548153');" onmouseover="showSample('q_268548153',this);" onmouseout="cjhideqs();">Velocities and errors</a></div> | |
| <div><a href="#" onclick="setQuery('q_1047280483');" onmouseover="showSample('q_1047280483',this);" onmouseout="cjhideqs();">Galaxies By Emission Lines</a></div> | |
| <div><a href="#" onclick="setQuery('q_191604836');" onmouseover="showSample('q_191604836',this);" onmouseout="cjhideqs();">Moving asteroids</a></div> | |
| <div><a href="#" onclick="setQuery('q_1893814627');" onmouseover="showSample('q_1893814627',this);" onmouseout="cjhideqs();">Quasars in imaging</a></div> | |
| <div><a href="#" onclick="setQuery('q_1199374736');" onmouseover="showSample('q_1199374736',this);" onmouseout="cjhideqs();">Object counts and logic</a></div> | |
| <div><a href="#" onclick="setQuery('q_1733737046');" onmouseover="showSample('q_1733737046',this);" onmouseout="cjhideqs();">Galaxy star blends</a></div> | |
| <div><a href="#" onclick="setQuery('q_317286293');" onmouseover="showSample('q_317286293',this);" onmouseout="cjhideqs();">Stars in specific fields</a></div> | |
| <div><a href="#" onclick="setQuery('q_1874540969');" onmouseover="showSample('q_1874540969',this);" onmouseout="cjhideqs();">Using three tables</a></div> | |
| <div><a href="#" onclick="setQuery('q_1435232814');" onmouseover="showSample('q_1435232814',this);" onmouseout="cjhideqs();">Objects close pairs</a></div> | |
| <div><a href="#" onclick="setQuery('q_2060639971');" onmouseover="showSample('q_2060639971',this);" onmouseout="cjhideqs();">Stars multiply measured</a></div> | |
| <div><a href="#" onclick="setQuery('q_1200416665');" onmouseover="showSample('q_1200416665',this);" onmouseout="cjhideqs();">Errors using flags</a></div> | |
| <div><a href="#" onclick="setQuery('q_1563979474');" onmouseover="showSample('q_1563979474',this);" onmouseout="cjhideqs();">Elliptical galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_673740146');" onmouseover="showSample('q_673740146',this);" onmouseout="cjhideqs();">Galaxies blue centers</a></div> | |
| <div><a href="#" onclick="setQuery('q_1080565066');" onmouseover="showSample('q_1080565066',this);" onmouseout="cjhideqs();">Diameter limited galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1549277712');" onmouseover="showSample('q_1549277712',this);" onmouseout="cjhideqs();">Extremely red galaxies</a></div> | |
| <div><a href="#" onclick="setQuery('q_1688445031');" onmouseover="showSample('q_1688445031',this);" onmouseout="cjhideqs();">LRG sample</a></div> | |
| <div><a href="#" onclick="setQuery('q_1276987864');" onmouseover="showSample('q_1276987864',this);" onmouseout="cjhideqs();">Spectra of Red Stars</a></div> | |
| <div><a href="#" onclick="setQuery('q_1804992033');" onmouseover="showSample('q_1804992033',this);" onmouseout="cjhideqs();">Galaxy counts HTM grid</a></div> | |
| <div><a href="#" onclick="setQuery('q_1055302504');" onmouseover="showSample('q_1055302504',this);" onmouseout="cjhideqs();">Binary stars colors</a></div> | |
| <div><a href="#" onclick="setQuery('q_183659941');" onmouseover="showSample('q_183659941',this);" onmouseout="cjhideqs();">Galaxies unsaturated near coord</a></div> | |
| <div><a href="#" onclick="setQuery('q_2000917639');" onmouseover="showSample('q_2000917639',this);" onmouseout="cjhideqs();">Search near BCGs</a></div> | |
| <div><a href="#" onclick="setQuery('q_359595534');" onmouseover="showSample('q_359595534',this);" onmouseout="cjhideqs();">Multiple Detections and Time Series</a></div> | |
| </div> | |
| <div id="weblog_samples"> | |
| <div><a href="#" onclick="setQuery('q_752833322');" onmouseover="showSample('q_752833322',this);" onmouseout="cjhideqs();">Monthly SQL Usage</a></div> | |
| <div><a href="#" onclick="setQuery('q_652519058');" onmouseover="showSample('q_652519058',this);" onmouseout="cjhideqs();">Monthly GB Returned</a></div> | |
| <div><a href="#" onclick="setQuery('q_518325890');" onmouseover="showSample('q_518325890',this);" onmouseout="cjhideqs();">Quarterly SQL Usage</a></div> | |
| <div><a href="#" onclick="setQuery('q_1785185606');" onmouseover="showSample('q_1785185606',this);" onmouseout="cjhideqs();">Quarterly Web Hits</a></div> | |
| </div> | |
| </div> | |
| <div id="hist" style="position: absolute; display: none; vertical-align: text-top; | |
| overflow: auto; z-index: 100; padding: 2 2 2 2;" class="transparent"> | |
| </div> | |
| <div style=""> | |
| <textarea style="display:none" id="q_377384944">-- Find unique objects in an RA/Dec box. | |
| -- PhotoPrimary is a view which selects only unique objects. | |
| -- The full list of good detections including duplicates is in PhotoObj | |
| -- A basic SELECT-FROM-WHERE query. | |
| SELECT TOP 100 objID, -- Get the unique object ID, | |
| field, ra, dec -- the field number, and coordinates | |
| FROM PhotoPrimary -- From the photometric data | |
| WHERE | |
| ra > 185. and ra < 185.1 and dec > 15. and dec < 15.1 </textarea><textarea style="display:none" id="q_1917342500">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 22, where the local | |
| -- extinction is > 0.175. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| SELECT TOP 10 objID | |
| FROM Galaxy | |
| WHERE | |
| r < 22 -- r IS NOT deredenned | |
| and extinction_r > 0.175 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_199934847">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1794636122">-- Using the BETWEEN syntax. | |
| -- Find all galaxies in a certain area of the sky that also meet other | |
| -- criteria in their measured parameters. This query intriduces the | |
| -- BETWEEN construct to specify a range of values. | |
| SELECT TOP 100 objID, ra, dec, cModelMag_g | |
| FROM Galaxy | |
| WHERE ra BETWEEN 178 AND 180 | |
| AND dec < 0 | |
| AND cModelMag_g BETWEEN 18 AND 19 | |
| </textarea><textarea style="display:none" id="q_2053263464">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- NOTE: This query must be run in batch mode, i.e. using the Submit button | |
| -- because it takes too long to execute in Quick mode. | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_610026851">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_347053935">-- Getting a subsample of the data. | |
| -- | |
| -- Uses the integer short object id (obj) - which is the least significant bits | |
| -- of the long objID - and the '%' operator (remainder) to get every 1000th | |
| -- object. | |
| -- NOTE: THIS IS NOT A TRULY RANDOM SAMPLE! | |
| SELECT TOP 100 u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_1503241840">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_1093157909">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 10 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1182730545">-- Finding galaxies by their emission lines: | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Spectra of Red | |
| -- Stars" sample query for an example of using stellar spectra. | |
| -- | |
| -- Spectral lines for galaxies are calculated using the MPA-JHU | |
| -- spectroscopic reanalysis (Tremonti et al. 2004; Brinchmann et al. 2004) | |
| -- and are stored in the galSpecLine table. For more on how spectral lines | |
| -- of galaxies are found, see the Galspec page of the sdss3.org website. | |
| -- | |
| -- This query selects galaxy spectra with high internal reddening, | |
| -- as measured by the standard Balmer decrement technique. It | |
| -- makes use of the galSpec tables for the measurements of | |
| -- galaxy lines. In this case we use galSpecLine, which has | |
| -- emission line measurements. | |
| SELECT | |
| s.plate, s.fiberid, s.mjd, s.z, s.zwarning, | |
| g.h_beta_flux, g.h_beta_flux_err, | |
| g.h_alpha_flux, g.h_alpha_flux_err | |
| FROM GalSpecLine AS g | |
| JOIN dbo.SpecObj AS s ON s.specobjid = g.specobjid | |
| WHERE | |
| h_alpha_flux > h_alpha_flux_err*5 | |
| AND h_beta_flux > h_beta_flux_err*5 | |
| AND h_beta_flux_err > 0 | |
| AND h_alpha_flux > 10.*h_beta_flux | |
| AND s.class = 'GALAXY' | |
| AND s.zwarning = 0 | |
| </textarea><textarea style="display:none" id="q_1884957360">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| -- NOTE: Since asteroids are rare objects in the SDSS data, this query will | |
| -- take a long time to run without the "TOP 10" and should be executed | |
| -- in batch mode (with the Submit button). | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_1314337809">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_453086348">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| -- An area restriction is added so the query will run in the Quick queue. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE | |
| (ra between 180 and 190) and (dec between -5 and 5) | |
| and (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_704206862">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you must specify which table each quantity in the SELECT | |
| -- clause comes from. The query illustrates the JOIN syntax between | |
| -- the two tables, which requires that a common quantity that is present in | |
| -- both tables be equal, in this case their common parent object. | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z | |
| FROM Galaxy G -- compare Galaxy and Star | |
| JOIN Star S ON G.parentID = S.parentID -- using the same parent | |
| WHERE | |
| G.parentID > 0 -- if the galaxy has a "parent", this object was deblended | |
| </textarea><textarea style="display:none" id="q_689961383">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s | |
| JOIN Field f ON s.fieldID = f.fieldID | |
| WHERE | |
| s.psfMag_g < 20 | |
| and f.pspStatus = 2 | |
| </textarea><textarea style="display:none" id="q_410365955">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r, | |
| r.stripe, | |
| r.strip | |
| FROM | |
| photoObj p | |
| JOIN field f ON f.fieldid = p.fieldid | |
| JOIN run r ON r.run=f.run | |
| WHERE | |
| f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1684523170">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. This query introduces the | |
| -- Neighbors table, which is a pre-computed list of the nearest | |
| -- neighbors of each object within 30 arcseconds. | |
| SELECT TOP 10 P.ObjID as objid1, L.ObjID as objid2, N.distance | |
| FROM PhotoPrimary P -- P is the primary object | |
| JOIN Neighbors N ON P.ObjID = N.ObjID -- N is the neighbor link | |
| JOIN PhotoPrimary L ON L.ObjID = N.NeighborObjID -- L is the lens candidate of P | |
| WHERE | |
| P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1823934513">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_348348979">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or that their sum is zero. | |
| -- (From Gordon Richards) | |
| -- | |
| -- NOTE: A caveat about using functons (like fPhotoFlags) is that if your | |
| -- query is selecting a very large number of rows (e.g. hundreds of | |
| -- thousands or millions) then it's that many function calls, and | |
| -- this will slow down the query execution significantly. In that | |
| -- case, you should replace the function call with its equivalent | |
| -- binary bitmask, e.g. if you run the query (with Quick button) | |
| -- SELECT (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT')) | |
| -- you will get the value 36507222016, which you can substitute in | |
| -- first line of the WHERE clause below as: | |
| -- (flags & 36507222016) > 0 | |
| -- to avoid zillions of function calls. | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr) | |
| </textarea><textarea style="display:none" id="q_569145814">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. | |
| -- This query has many conditions, and also shows more of the | |
| -- bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_1687216546">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_113893222">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| -- Another query that makes extensive use of photo flags to get a sample | |
| -- of galaxies within a size range as specified by their i-band Petrosian | |
| -- radius. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1471444940">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query but selects galaxies that | |
| -- are red (i-z color greater than a certain threshold). | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) | |
| </textarea><textarea style="display:none" id="q_1092529461">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests that selects Luminous | |
| -- Red Galaxies (LRGs). | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) ) | |
| </textarea><textarea style="display:none" id="q_1476423508">-- Spectra of Red Stars | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Galaxies with | |
| -- Emission Lines" sample query for an example of using galaxy spectra. | |
| -- | |
| -- Spectral lines for stars are calculated using the SEGUE Stellar Parameter | |
| -- Pipeline (SSPP; Lee et al. 2008) and are stored in the sppLines | |
| -- table. For more on how spectral lines of stars are found, see | |
| -- the SSPP page of the sdss3.org website. | |
| -- This query selects red stars (spectral type K), with large | |
| -- CaII triplet eq widths, with low errors on the CaII triplet | |
| -- equivalent widths. | |
| SELECT | |
| sl.plate,sl.mjd,sl.fiber, | |
| sl.caIIKside,sl.caIIKerr,sl.caIIKmask, | |
| sp.fehadop,sp.fehadopunc,sp.fehadopn, | |
| sp.loggadopn,sp.loggadopunc | |
| FROM sppLines AS sl | |
| JOIN sppParams AS sp ON sl.specobjid = sp.specobjid | |
| WHERE | |
| fehadop < -3.5 | |
| AND fehadopunc between 0.01 | |
| and 0.5 and fehadopn > 3 | |
| </textarea><textarea style="display:none" id="q_1964088379">-- Galaxy counts on HTM grid. | |
| -- | |
| -- Create a count of galaxies for each of the Hierarchical Triangular Mesh (HTM) triangles. | |
| -- Galaxies should satisfy a certain color cut like 0.7u-0.5g-0.2i<1.25 && r<21.75, output | |
| -- it in a form adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE | |
| -- RA/dec cut added to make query run in Quick mode | |
| (ra between 180 and 181 and dec between -1 and 1) and | |
| (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1609807292">-- Binary Stars Colors. | |
| -- | |
| -- Find binary stars with specific colors. | |
| -- At least one of them should have the colors (meets Paul Szkody's color cut) of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1 -- S1 is the white dwarf | |
| JOIN Neighbors N ON S1.objID = N. objID -- N is the precomputed neighbors link | |
| JOIN Star S2 ON S2.objID = N.NeighborObjID -- S2 is the second star | |
| WHERE | |
| N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets the color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_949416951">-- Galaxies unsaturated near (given) coordinates. | |
| -- | |
| -- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'ORDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy AS G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) AS GN -- this function outputs a table, so we have to do a join | |
| ON G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE | |
| (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_1820036051">-- Search near BCG galaxies. | |
| -- | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- This query has a very complex WHERE clause. | |
| SELECT TOP 1000 G.objID, COUNT(N.NeighborObjID) AS pop | |
| FROM Galaxy AS G -- first gravitational lens candidate | |
| JOIN Neighbors AS N ON G.objID = N.objID -- precomputed list of neighbors | |
| JOIN Galaxy AS U ON U.objID = N.neighborObjID -- a neighbor galaxy of G | |
| JOIN photoZ AS Gpz ON G.objID = Gpz.objID -- photoZ of G. | |
| JOIN photoZ AS Npz ON U.objID = Npz.objID -- neighbor photoZ | |
| WHERE | |
| G.ra BETWEEN 160 AND 170 | |
| AND G.dec BETWEEN -5 AND 5 | |
| AND N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| AND ABS(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| AND (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| AND (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| AND (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| AND G.petroMag_i > 17.5 | |
| AND (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| AND (G.petroMag_r < 30 AND G.g < 30 AND G.r < 30 AND G.i < 30) | |
| AND (G.r < 19.2 | |
| AND ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| AND (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 AND 0.2 ) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| AND (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| AND ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| GROUP BY G.objID | |
| </textarea><textarea style="display:none" id="q_2086102066">-- The detectionIndex table contains all detections of a given physical object, | |
| -- which is uniquely identified by the "thingid". In order to extract photometry, | |
| -- you need a join with the PhotoObjAll table, using the objid. | |
| -- There is also a flag field called isPrimary, which is 1 for the object that | |
| -- is found on a primary polygon/field, all the other detections have 0 in this field. | |
| -- Here is a compound query to find all time series around a certain object with a thingid= 97423000 | |
| SELECT | |
| LTRIM(STR(mjd_r,20,2)) AS MJD, | |
| dbo.fSDSS(p.objId) AS ID, | |
| modelMag_g, modelMagErr_g, | |
| modelMag_r, modelMagErr_r, | |
| modelMag_i, modelMagErr_i, p.ra, p.dec | |
| INTO #list | |
| FROM detectionindex d | |
| JOIN PhotoObjAll p ON d.objid=p.objid | |
| JOIN Field f ON p.fieldid=f.fieldid | |
| WHERE d.thingid=97423000 | |
| ORDER BY 1 | |
| GO | |
| -- | |
| -- Now find objects near each of the detections | |
| -- | |
| SELECT a.*, b.* | |
| FROM #list a | |
| CROSS APPLY dbo.fGetNearbyObjEq(a.ra, a.dec, 0.1) b | |
| </textarea> | |
| <textarea style="display:none" id="q_1342567403">-- Here's a query that looks at average query time by month, for all queries that took longer then 10 minutes. | |
| select | |
| ( | |
| convert(varchar, datepart(year, timestart))+'_'+ | |
| right('00'+convert(varchar,datepart(month, timestart)),2) | |
| ) as yymm, | |
| avg ( | |
| datepart(hour, (timeend - timestart)) * 360 + | |
| datepart(minute, (timeend - timestart)) * 60 + | |
| datepart(second, (timeend - timestart)) | |
| ) as avgseconds | |
| from jobs | |
| where | |
| timeend - timestart > 0 | |
| and timeend is not null | |
| and ( | |
| datepart(hour, (timeend - timestart)) * 60 + | |
| datepart(minute, (timeend - timestart)) | |
| ) >= 10 | |
| and taskname not like '%__SYSTEM__%' | |
| and estimate > 1 | |
| group by | |
| convert(varchar, datepart(year, timestart))+'_'+ | |
| right('00'+convert(varchar,datepart(month, timestart)),2) | |
| order by | |
| convert(varchar, datepart(year, timestart))+'_'+ | |
| right('00'+convert(varchar,datepart(month, timestart)),2) | |
| </textarea><textarea style="display:none" id="q_1185292591">-- Accounts created, monthly. This is not cumulative. | |
| select | |
| ( | |
| convert(varchar, datepart(year, timecreated))+'_'+ | |
| right('00'+convert(varchar,datepart(month, timecreated)),2) | |
| ) as yymm, | |
| count(*) as ucnt | |
| from users | |
| group by | |
| convert(varchar, datepart(year, timecreated))+'_'+ | |
| right('00'+convert(varchar,datepart(month, timecreated)),2) | |
| order by | |
| convert(varchar, datepart(year, timecreated))+'_'+ | |
| right('00'+convert(varchar,datepart(month, timecreated)),2)</textarea> | |
| <textarea style="display:none" id="q_2127032053">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_1822251911">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_2112964880">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_1876103269">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_1604660031">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1209894154">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_1732295176">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_2122410695">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_162421342">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1947188265">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_1076082999">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_362452986">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_2140829941">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1307734809">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_699861840">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_1448724282">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1373505727">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_203899950">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_160825834">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_1984607857">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_2071057527">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1616963259">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1224142175">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_733458258">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_1195635002">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_792880405">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1564994359">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_491051768">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_453518089">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_1011044940">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_1835462071">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_715981218">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_1104283183">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_1837021711">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_2135502459">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_114193719">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_318573181">-- Find unique objects in an RA/Dec box. | |
| -- PhotoPrimary is a view which selects only unique objects. | |
| -- The full list of good detections including duplicates is in PhotoObj | |
| -- A basic SELECT-FROM-WHERE query. | |
| SELECT TOP 100 objID, -- Get the unique object ID, | |
| field, ra, dec -- the field number, and coordinates | |
| FROM PhotoPrimary -- From the photometric data | |
| WHERE | |
| ra > 185. and ra < 185.1 and dec > 15. and dec < 15.1 </textarea><textarea style="display:none" id="q_2121526033">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 22, where the local | |
| -- extinction is > 0.175. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| SELECT TOP 10 objID | |
| FROM Galaxy | |
| WHERE | |
| r < 22 -- r IS NOT deredenned | |
| and extinction_r > 0.175 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_1702999202">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_807954861">-- Using the BETWEEN syntax. | |
| -- Find all galaxies in a certain area of the sky that also meet other | |
| -- criteria in their measured parameters. This query intriduces the | |
| -- BETWEEN construct to specify a range of values. | |
| SELECT TOP 100 objID, ra, dec, cModelMag_g | |
| FROM Galaxy | |
| WHERE ra BETWEEN 178 AND 180 | |
| AND dec < 0 | |
| AND cModelMag_g BETWEEN 18 AND 19 | |
| </textarea><textarea style="display:none" id="q_1601839065">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- NOTE: This query must be run in batch mode, i.e. using the Submit button | |
| -- because it takes too long to execute in Quick mode. | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1407015576">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_810186038">-- Getting a subsample of the data. | |
| -- | |
| -- Uses the integer short object id (obj) - which is the least significant bits | |
| -- of the long objID - and the '%' operator (remainder) to get every 1000th | |
| -- object. | |
| -- NOTE: THIS IS NOT A TRULY RANDOM SAMPLE! | |
| SELECT TOP 100 u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_446289279">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_832506840">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 10 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1549577480">-- Finding galaxies by their emission lines: | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Spectra of Red | |
| -- Stars" sample query for an example of using stellar spectra. | |
| -- | |
| -- Spectral lines for galaxies are calculated using the MPA-JHU | |
| -- spectroscopic reanalysis (Tremonti et al. 2004; Brinchmann et al. 2004) | |
| -- and are stored in the galSpecLine table. For more on how spectral lines | |
| -- of galaxies are found, see the Galspec page of the sdss3.org website. | |
| -- | |
| -- This query selects galaxy spectra with high internal reddening, | |
| -- as measured by the standard Balmer decrement technique. It | |
| -- makes use of the galSpec tables for the measurements of | |
| -- galaxy lines. In this case we use galSpecLine, which has | |
| -- emission line measurements. | |
| SELECT | |
| s.plate, s.fiberid, s.mjd, s.z, s.zwarning, | |
| g.h_beta_flux, g.h_beta_flux_err, | |
| g.h_alpha_flux, g.h_alpha_flux_err | |
| FROM GalSpecLine AS g | |
| JOIN dbo.SpecObj AS s ON s.specobjid = g.specobjid | |
| WHERE | |
| h_alpha_flux > h_alpha_flux_err*5 | |
| AND h_beta_flux > h_beta_flux_err*5 | |
| AND h_beta_flux_err > 0 | |
| AND h_alpha_flux > 10.*h_beta_flux | |
| AND s.class = 'GALAXY' | |
| AND s.zwarning = 0 | |
| </textarea><textarea style="display:none" id="q_1075597663">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| -- NOTE: Since asteroids are rare objects in the SDSS data, this query will | |
| -- take a long time to run without the "TOP 10" and should be executed | |
| -- in batch mode (with the Submit button). | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_387047336">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_464249349">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| -- An area restriction is added so the query will run in the Quick queue. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE | |
| (ra between 180 and 190) and (dec between -5 and 5) | |
| and (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1257775135">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you must specify which table each quantity in the SELECT | |
| -- clause comes from. The query illustrates the JOIN syntax between | |
| -- the two tables, which requires that a common quantity that is present in | |
| -- both tables be equal, in this case their common parent object. | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z | |
| FROM Galaxy G -- compare Galaxy and Star | |
| JOIN Star S ON G.parentID = S.parentID -- using the same parent | |
| WHERE | |
| G.parentID > 0 -- if the galaxy has a "parent", this object was deblended | |
| </textarea><textarea style="display:none" id="q_1773962834">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s | |
| JOIN Field f ON s.fieldID = f.fieldID | |
| WHERE | |
| s.psfMag_g < 20 | |
| and f.pspStatus = 2 | |
| </textarea><textarea style="display:none" id="q_1890051708">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r, | |
| r.stripe, | |
| r.strip | |
| FROM | |
| photoObj p | |
| JOIN field f ON f.fieldid = p.fieldid | |
| JOIN run r ON r.run=f.run | |
| WHERE | |
| f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_2042342521">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. This query introduces the | |
| -- Neighbors table, which is a pre-computed list of the nearest | |
| -- neighbors of each object within 30 arcseconds. | |
| SELECT TOP 10 P.ObjID as objid1, L.ObjID as objid2, N.distance | |
| FROM PhotoPrimary P -- P is the primary object | |
| JOIN Neighbors N ON P.ObjID = N.ObjID -- N is the neighbor link | |
| JOIN PhotoPrimary L ON L.ObjID = N.NeighborObjID -- L is the lens candidate of P | |
| WHERE | |
| P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1271476914">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_162268584">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or that their sum is zero. | |
| -- (From Gordon Richards) | |
| -- | |
| -- NOTE: A caveat about using functons (like fPhotoFlags) is that if your | |
| -- query is selecting a very large number of rows (e.g. hundreds of | |
| -- thousands or millions) then it's that many function calls, and | |
| -- this will slow down the query execution significantly. In that | |
| -- case, you should replace the function call with its equivalent | |
| -- binary bitmask, e.g. if you run the query (with Quick button) | |
| -- SELECT (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT')) | |
| -- you will get the value 36507222016, which you can substitute in | |
| -- first line of the WHERE clause below as: | |
| -- (flags & 36507222016) > 0 | |
| -- to avoid zillions of function calls. | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr) | |
| </textarea><textarea style="display:none" id="q_200158383">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. | |
| -- This query has many conditions, and also shows more of the | |
| -- bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_220572073">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_454660149">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| -- Another query that makes extensive use of photo flags to get a sample | |
| -- of galaxies within a size range as specified by their i-band Petrosian | |
| -- radius. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1221376687">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query but selects galaxies that | |
| -- are red (i-z color greater than a certain threshold). | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) | |
| </textarea><textarea style="display:none" id="q_663779516">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests that selects Luminous | |
| -- Red Galaxies (LRGs). | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) ) | |
| </textarea><textarea style="display:none" id="q_338186821">-- Spectra of Red Stars | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Galaxies with | |
| -- Emission Lines" sample query for an example of using galaxy spectra. | |
| -- | |
| -- Spectral lines for stars are calculated using the SEGUE Stellar Parameter | |
| -- Pipeline (SSPP; Lee et al. 2008) and are stored in the sppLines | |
| -- table. For more on how spectral lines of stars are found, see | |
| -- the SSPP page of the sdss3.org website. | |
| -- This query selects red stars (spectral type K), with large | |
| -- CaII triplet eq widths, with low errors on the CaII triplet | |
| -- equivalent widths. | |
| SELECT | |
| sl.plate,sl.mjd,sl.fiber, | |
| sl.caIIKside,sl.caIIKerr,sl.caIIKmask, | |
| sp.fehadop,sp.fehadopunc,sp.fehadopn, | |
| sp.loggadopn,sp.loggadopunc | |
| FROM sppLines AS sl | |
| JOIN sppParams AS sp ON sl.specobjid = sp.specobjid | |
| WHERE | |
| fehadop < -3.5 | |
| AND fehadopunc between 0.01 | |
| and 0.5 and fehadopn > 3 | |
| </textarea><textarea style="display:none" id="q_284125386">-- Galaxy counts on HTM grid. | |
| -- | |
| -- Create a count of galaxies for each of the Hierarchical Triangular Mesh (HTM) triangles. | |
| -- Galaxies should satisfy a certain color cut like 0.7u-0.5g-0.2i<1.25 && r<21.75, output | |
| -- it in a form adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE | |
| -- RA/dec cut added to make query run in Quick mode | |
| (ra between 180 and 181 and dec between -1 and 1) and | |
| (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1363234497">-- Binary Stars Colors. | |
| -- | |
| -- Find binary stars with specific colors. | |
| -- At least one of them should have the colors (meets Paul Szkody's color cut) of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1 -- S1 is the white dwarf | |
| JOIN Neighbors N ON S1.objID = N. objID -- N is the precomputed neighbors link | |
| JOIN Star S2 ON S2.objID = N.NeighborObjID -- S2 is the second star | |
| WHERE | |
| N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets the color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_911927524">-- Galaxies unsaturated near (given) coordinates. | |
| -- | |
| -- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'ORDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy AS G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) AS GN -- this function outputs a table, so we have to do a join | |
| ON G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE | |
| (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_2046113808">-- Search near BCG galaxies. | |
| -- | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- This query has a very complex WHERE clause. | |
| SELECT TOP 1000 G.objID, COUNT(N.NeighborObjID) AS pop | |
| FROM Galaxy AS G -- first gravitational lens candidate | |
| JOIN Neighbors AS N ON G.objID = N.objID -- precomputed list of neighbors | |
| JOIN Galaxy AS U ON U.objID = N.neighborObjID -- a neighbor galaxy of G | |
| JOIN photoZ AS Gpz ON G.objID = Gpz.objID -- photoZ of G. | |
| JOIN photoZ AS Npz ON U.objID = Npz.objID -- neighbor photoZ | |
| WHERE | |
| G.ra BETWEEN 160 AND 170 | |
| AND G.dec BETWEEN -5 AND 5 | |
| AND N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| AND ABS(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| AND (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| AND (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| AND (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| AND G.petroMag_i > 17.5 | |
| AND (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| AND (G.petroMag_r < 30 AND G.g < 30 AND G.r < 30 AND G.i < 30) | |
| AND (G.r < 19.2 | |
| AND ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| AND (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 AND 0.2 ) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| AND (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| AND ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| GROUP BY G.objID | |
| </textarea><textarea style="display:none" id="q_1348920221">-- The detectionIndex table contains all detections of a given physical object, | |
| -- which is uniquely identified by the "thingid". In order to extract photometry, | |
| -- you need a join with the PhotoObjAll table, using the objid. | |
| -- There is also a flag field called isPrimary, which is 1 for the object that | |
| -- is found on a primary polygon/field, all the other detections have 0 in this field. | |
| -- Here is a compound query to find all time series around a certain object with a thingid= 97423000 | |
| SELECT | |
| LTRIM(STR(mjd_r,20,2)) AS MJD, | |
| dbo.fSDSS(p.objId) AS ID, | |
| modelMag_g, modelMagErr_g, | |
| modelMag_r, modelMagErr_r, | |
| modelMag_i, modelMagErr_i, p.ra, p.dec | |
| INTO #list | |
| FROM detectionindex d | |
| JOIN PhotoObjAll p ON d.objid=p.objid | |
| JOIN Field f ON p.fieldid=f.fieldid | |
| WHERE d.thingid=97423000 | |
| ORDER BY 1 | |
| GO | |
| -- | |
| -- Now find objects near each of the detections | |
| -- | |
| SELECT a.*, b.* | |
| FROM #list a | |
| CROSS APPLY dbo.fGetNearbyObjEq(a.ra, a.dec, 0.1) b | |
| </textarea><textarea style="display:none" id="q_619277145">-- The APOGEE survey is conducted along a number of different lines of sight, | |
| -- each referred to as as a "field" or "location" (interchangeably). Each | |
| -- field has a name and an id number (LOCATION_ID). The stars in each field | |
| -- are observed multiple times on multiple visits, on different MJDs. These | |
| -- may involve one or more physical plug plates. | |
| -- To find all the plate visits, one can search as follows (for LOCATION_ID | |
| -- 4105): | |
| SELECT plate, mjd FROM apogeePlate WHERE location_id=4105 | |
| -- The same field can be searched by its name (in this case 'M13'): | |
| SELECT plate, mjd FROM apogeePlate WHERE name = 'M13' | |
| </textarea><textarea style="display:none" id="q_1575944052">-- Get ASPCAP parameters and errors for all stars that were targeted as part | |
| -- of the main APOGEE survey: | |
| -- The stellar parameters are available for all stars that had ASPCAP run | |
| -- on them. However, this includes some spectra known to be bad as well as | |
| -- stars targeted as part of ancillary programs of various | |
| -- sorts. Restricting to the good, main survey targets requires checking on | |
| -- target and catalog flags, as in the examples below: | |
| SELECT TOP 100 | |
| s.apogee_id,s.ra, s.dec, s.glon, s.glat, | |
| s.vhelio_avg,s.vscatter, | |
| a.teff, a.teff_err, a.logg, a.logg_err, a.metals, a.metals_err, | |
| a.alphafe, a.alphafe_err, | |
| dbo.fApogeeAspcapFlagN(a.aspcapflag), | |
| dbo.fApogeeStarFlagN(s.starflag) | |
| FROM apogeeStar s | |
| JOIN aspcapStar a on a.apstar_id = s.apstar_id | |
| WHERE (a.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and | |
| s.commiss = 0 and | |
| (s.apogee_target1 & | |
| (dbo.fApogeeTarget1('APOGEE_SHORT')+ | |
| dbo.fApogeeTarget1('APOGEE_INTERMEDIATE')+ | |
| dbo.fApogeeTarget1('APOGEE_LONG'))) != 0 | |
| </textarea><textarea style="display:none" id="q_873427785">-- Get parameters for all stars with [Fe/H] < -2 with no BAD FLAGS set: | |
| -- You can also select a subset of the stars based on their | |
| -- properties. This example finds a set of metal-poor stars, without any | |
| -- flags set indicating that the observations or analysis is bad. | |
| SELECT TOP 100 | |
| s.apogee_id,s.ra, s.dec, s.glon, s.glat, | |
| s.vhelio_avg,s.vscatter, | |
| a.teff,a.logg, a.metals, a.alphafe, | |
| dbo.fApogeeAspcapFlagN(a.aspcapflag), | |
| dbo.fApogeeStarFlagN(s.starflag) | |
| FROM apogeeStar s | |
| JOIN aspcapStar a on a.apstar_id = s.apstar_id | |
| WHERE (a.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 | |
| and a.teff > 0 and a.metals < -2 | |
| </textarea><textarea style="display:none" id="q_509946294">-- Get ASPCAP parameters for stars flagged as known cluster members: | |
| -- In addition to selecting main survey targets, you can | |
| -- select other objects according how they were selected. This is | |
| -- an example of selecting objects chosen to be calibrator stars in | |
| -- clusters with known metallicities (APOGEE_CALIB_CLUSTER). | |
| SELECT TOP 100 | |
| s.apogee_id,s.ra, s.dec, s.glon, s.glat, | |
| s.vhelio_avg,s.vscatter, | |
| a.teff, a.teff_err, a.logg, a.logg_err, a.metals, a.metals_err, | |
| a.alphafe, a.alphafe_err, | |
| dbo.fApogeeAspcapFlagN(a.aspcapflag), | |
| dbo.fApogeeStarFlagN(s.starflag) | |
| FROM apogeeStar s | |
| JOIN aspcapStar a on a.apstar_id = s.apstar_id | |
| WHERE (a.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and | |
| s.commiss = 0 and | |
| (s.apogee_target2 & (dbo.fApogeeTarget2('APOGEE_CALIB_CLUSTER')) != 0) | |
| </textarea><textarea style="display:none" id="q_1886714918">-- Get proper motions, JHK mag and errors, K-band extinction and radial | |
| -- velocities, for stars with RVs > 300 km/s (with no BAD flags for RVs): | |
| -- There is photometric data associated with each target, including proper | |
| -- motions and other information. This example looks for such information | |
| -- for larger (heliocentric) radial velocity stars. It restricts to objects | |
| -- with good measured ASPCAP parameters. This requires joining the apogeeStar and | |
| -- aspcapStar tables with the apogeeObject table, which has the target information. | |
| SELECT TOP 100 | |
| star.apogee_id, star.ra, star.dec, star.glon, star.glat, | |
| star.vhelio_avg, star.vscatter, | |
| obj.j, obj.h, obj.k, obj.ak_targ, obj.ak_targ_method, obj.ak_wise, | |
| aspcap.teff, aspcap.logg, aspcap.metals | |
| FROM apogeeStar star | |
| JOIN aspcapStar aspcap on aspcap.apstar_id = star.apstar_id | |
| JOIN apogeeObject obj on aspcap.target_id = obj.target_id | |
| WHERE (aspcap.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and aspcap.teff > 0 | |
| and (star.vhelio_avg > 300) and (star.starflag & | |
| dbo.fApogeeStarFlag('SUSPECT_RV_COMBINATION')) = 0 | |
| and star.nvisits > 2 order by aspcap.apogee_id | |
| </textarea><textarea style="display:none" id="q_214541362">-- Get ASPCAP parameters and targeting flags for all stars with 1 degree of a cluster center: | |
| -- CASJobs allows search for objects near any particular RA and Dec. The | |
| -- following example searches for ASPCAP parameters and targeting flags for | |
| -- the stars observed near M13. | |
| SELECT star.apstar_id, | |
| star.apogee_id, star.ra, star.dec, star.glon, star.glat, | |
| star.apogee_target1, star.apogee_target2, | |
| aspcap.teff,aspcap.logg,aspcap.metals | |
| FROM apogeeStar star | |
| JOIN dbo.fGetNearbyApogeeStarEq(250.423458,36.461306,60) near on | |
| star.apstar_id=near.apstar_id | |
| JOIN aspcapStar aspcap on aspcap.apstar_id = star.apstar_id | |
| </textarea><textarea style="display:none" id="q_114253696"> | |
| -- Get individual RVs from individual visits, the ASPCAP parameters for the combined | |
| -- spectra for stars which have more than 6 visits: | |
| -- Each star is visited several times, and in some case many times, in | |
| -- order to build up signal-to-noise and to detect radial velocity | |
| -- variations. The information about each visit to each star is in the | |
| -- apogeeVisit table. One could join this table with apogeeStar on | |
| -- apogee_id in order to literally find all visits to each star. However, | |
| -- in this example we are interested in just finding those visits that | |
| -- actually contributed to each combined spectrum. In this case, bad visits | |
| -- are excluded and commissioning data and survey data are kept separate | |
| -- (not combined). To find these stars, one may use the apogeeStarVisit | |
| -- table in CAS, or the array visit_pk which exists for each star in the | |
| -- allStar file. Alternatively, if you wanted to find all visits to a | |
| -- particular star, one could replace in the code below apogeeStarVisit | |
| -- with apogeeStarAllVisit and visit_pk with all_visit_pk. | |
| SELECT top 100 | |
| visit.*, aspcap.teff, aspcap.logg, aspcap.metals | |
| FROM apogeeVisit visit | |
| JOIN apogeeStarVisit starvisit on visit.visit_id = starvisit.visit_id | |
| JOIN aspcapStar aspcap on aspcap.apstar_id = starvisit.apstar_id | |
| JOIN apogeeStar star on star.apstar_id = starvisit.apstar_id | |
| WHERE (aspcap.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and aspcap.teff > 0 | |
| and (star.apogee_target1 & dbo.fApogeeTarget1('APOGEE_LONG')) > 0 | |
| and star.nvisits > 6 | |
| ORDER BY visit.apogee_id | |
| </textarea><textarea style="display:none" id="q_286757891">-- Get APOGEE_IDs and SDSS/BOSS plate, mjd, fiberid for all stars that have both APOGEE and SEGUE spectra: | |
| -- A small number of objects have been observed both in the optical with | |
| -- the SDSS and/or BOSS spectrographs and in the infrared with the APOGEE | |
| -- spectrograph. The examples below finds all matches between primary | |
| -- SDSS/BOSS spectra and APOGEE stars with a 3 arcsec tolerance for such | |
| -- cases (note that there are some cases where an entry in one catalog | |
| -- matches multiple entries in the other). | |
| SELECT TOP 50 | |
| specobj.plate as specobj_plate, specobj.mjd as specobj_mjd, | |
| specobj.fiberid as specobj_fiberid, | |
| specobj.ra as specobj_ra, specobj.dec as specobj_dec, | |
| star.apstar_id, star.ra as star_ra, star.dec as star_dec | |
| FROM apogeeStar AS star | |
| CROSS APPLY dbo.fGetNearestSpecObjEq( star.ra, star.dec, 0.05) AS near | |
| JOIN specobj ON near.specobjid=specobj.specobjid | |
| </textarea><textarea style="display:none" id="q_251526975">-- Get SDSS ugriz photometry, errors and flags, ASPCAP parameters for the APOGEE stars with b > 60: | |
| -- In addition to matching to the SDSS spectroscopy, you can also match to | |
| -- the SDSS photometric imaging data. In this case, we only give an example | |
| -- within CAS. To do this purely with flat files requires either | |
| -- downloading the full photometric catalog (about 3 Tbytes) or the | |
| -- "datasweep" files (about 300 Gbytes), both described in the imaging data | |
| -- access documentation, and constructing an efficient flat-file method to | |
| -- do the matching. For most purposes, CAS will be the right way to do this. | |
| SELECT TOP 50 | |
| photoobj.run, photoobj.camcol, photoobj.field, photoobj.obj, | |
| photoobj.psfmag_u, photoobj.psfmag_g, photoobj.psfmag_r, | |
| photoobj.psfmag_i, photoobj.psfmag_z, | |
| photoobj.ra as photoobj_ra, photoobj.dec as photoobj_dec, | |
| star.apstar_id, star.ra as star_ra, star.dec as star_dec, | |
| aspcap.teff, aspcap.metals, aspcap.logg | |
| FROM apogeeStar AS star | |
| CROSS APPLY dbo.fGetNearestObjEq( star.ra, star.dec, 0.05) AS near | |
| JOIN photoobj ON near.objid=photoobj.objid | |
| JOIN aspcapStar as aspcap ON star.apstar_id = aspcap.apstar_id | |
| WHERE star.glat > 60. and aspcap.teff > 0 | |
| </textarea> | |
| <textarea style="display:none" id="q_341160974">-- Find unique objects in an RA/Dec box. | |
| -- PhotoPrimary is a view which selects only unique objects. | |
| -- The full list of good detections including duplicates is in PhotoObj | |
| -- A basic SELECT-FROM-WHERE query. | |
| SELECT TOP 100 objID, -- Get the unique object ID, | |
| field, ra, dec -- the field number, and coordinates | |
| FROM PhotoPrimary -- From the photometric data | |
| WHERE | |
| ra > 185. and ra < 185.1 and dec > 15. and dec < 15.1 </textarea><textarea style="display:none" id="q_2088747594">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 22, where the local | |
| -- extinction is > 0.175. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| SELECT TOP 10 objID | |
| FROM Galaxy | |
| WHERE | |
| r < 22 -- r IS NOT deredenned | |
| and extinction_r > 0.175 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_326961301">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1559254220">-- Using the BETWEEN syntax. | |
| -- Find all galaxies in a certain area of the sky that also meet other | |
| -- criteria in their measured parameters. This query intriduces the | |
| -- BETWEEN construct to specify a range of values. | |
| SELECT TOP 100 objID, ra, dec, cModelMag_g | |
| FROM Galaxy | |
| WHERE ra BETWEEN 178 AND 180 | |
| AND dec < 0 | |
| AND cModelMag_g BETWEEN 18 AND 19 | |
| </textarea><textarea style="display:none" id="q_364596238">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- NOTE: This query must be run in batch mode, i.e. using the Submit button | |
| -- because it takes too long to execute in Quick mode. | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1145250273">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_965086605">-- Getting a subsample of the data. | |
| -- | |
| -- Uses the integer short object id (obj) - which is the least significant bits | |
| -- of the long objID - and the '%' operator (remainder) to get every 1000th | |
| -- object. | |
| -- NOTE: THIS IS NOT A TRULY RANDOM SAMPLE! | |
| SELECT TOP 100 u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_893526326">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_1359629897">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 10 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_2046520797">-- Finding galaxies by their emission lines: | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Spectra of Red | |
| -- Stars" sample query for an example of using stellar spectra. | |
| -- | |
| -- Spectral lines for galaxies are calculated using the MPA-JHU | |
| -- spectroscopic reanalysis (Tremonti et al. 2004; Brinchmann et al. 2004) | |
| -- and are stored in the galSpecLine table. For more on how spectral lines | |
| -- of galaxies are found, see the Galspec page of the sdss3.org website. | |
| -- | |
| -- This query selects galaxy spectra with high internal reddening, | |
| -- as measured by the standard Balmer decrement technique. It | |
| -- makes use of the galSpec tables for the measurements of | |
| -- galaxy lines. In this case we use galSpecLine, which has | |
| -- emission line measurements. | |
| SELECT | |
| s.plate, s.fiberid, s.mjd, s.z, s.zwarning, | |
| g.h_beta_flux, g.h_beta_flux_err, | |
| g.h_alpha_flux, g.h_alpha_flux_err | |
| FROM GalSpecLine AS g | |
| JOIN dbo.SpecObj AS s ON s.specobjid = g.specobjid | |
| WHERE | |
| h_alpha_flux > h_alpha_flux_err*5 | |
| AND h_beta_flux > h_beta_flux_err*5 | |
| AND h_beta_flux_err > 0 | |
| AND h_alpha_flux > 10.*h_beta_flux | |
| AND s.class = 'GALAXY' | |
| AND s.zwarning = 0 | |
| </textarea><textarea style="display:none" id="q_1722069906">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| -- NOTE: Since asteroids are rare objects in the SDSS data, this query will | |
| -- take a long time to run without the "TOP 10" and should be executed | |
| -- in batch mode (with the Submit button). | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_504267227">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_273521898">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| -- An area restriction is added so the query will run in the Quick queue. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE | |
| (ra between 180 and 190) and (dec between -5 and 5) | |
| and (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1145880200">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you must specify which table each quantity in the SELECT | |
| -- clause comes from. The query illustrates the JOIN syntax between | |
| -- the two tables, which requires that a common quantity that is present in | |
| -- both tables be equal, in this case their common parent object. | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z | |
| FROM Galaxy G -- compare Galaxy and Star | |
| JOIN Star S ON G.parentID = S.parentID -- using the same parent | |
| WHERE | |
| G.parentID > 0 -- if the galaxy has a "parent", this object was deblended | |
| </textarea><textarea style="display:none" id="q_1019525219">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s | |
| JOIN Field f ON s.fieldID = f.fieldID | |
| WHERE | |
| s.psfMag_g < 20 | |
| and f.pspStatus = 2 | |
| </textarea><textarea style="display:none" id="q_891488825">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r, | |
| r.stripe, | |
| r.strip | |
| FROM | |
| photoObj p | |
| JOIN field f ON f.fieldid = p.fieldid | |
| JOIN run r ON r.run=f.run | |
| WHERE | |
| f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1456890876">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. This query introduces the | |
| -- Neighbors table, which is a pre-computed list of the nearest | |
| -- neighbors of each object within 30 arcseconds. | |
| SELECT TOP 10 P.ObjID as objid1, L.ObjID as objid2, N.distance | |
| FROM PhotoPrimary P -- P is the primary object | |
| JOIN Neighbors N ON P.ObjID = N.ObjID -- N is the neighbor link | |
| JOIN PhotoPrimary L ON L.ObjID = N.NeighborObjID -- L is the lens candidate of P | |
| WHERE | |
| P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1683900573">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_538248463">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or that their sum is zero. | |
| -- (From Gordon Richards) | |
| -- | |
| -- NOTE: A caveat about using functons (like fPhotoFlags) is that if your | |
| -- query is selecting a very large number of rows (e.g. hundreds of | |
| -- thousands or millions) then it's that many function calls, and | |
| -- this will slow down the query execution significantly. In that | |
| -- case, you should replace the function call with its equivalent | |
| -- binary bitmask, e.g. if you run the query (with Quick button) | |
| -- SELECT (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT')) | |
| -- you will get the value 36507222016, which you can substitute in | |
| -- first line of the WHERE clause below as: | |
| -- (flags & 36507222016) > 0 | |
| -- to avoid zillions of function calls. | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr) | |
| </textarea><textarea style="display:none" id="q_2107503000">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. | |
| -- This query has many conditions, and also shows more of the | |
| -- bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_1724772452">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_34323696">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| -- Another query that makes extensive use of photo flags to get a sample | |
| -- of galaxies within a size range as specified by their i-band Petrosian | |
| -- radius. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_357369514">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query but selects galaxies that | |
| -- are red (i-z color greater than a certain threshold). | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) | |
| </textarea><textarea style="display:none" id="q_2085753961">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests that selects Luminous | |
| -- Red Galaxies (LRGs). | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) ) | |
| </textarea><textarea style="display:none" id="q_1598688566">-- Spectra of Red Stars | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Galaxies with | |
| -- Emission Lines" sample query for an example of using galaxy spectra. | |
| -- | |
| -- Spectral lines for stars are calculated using the SEGUE Stellar Parameter | |
| -- Pipeline (SSPP; Lee et al. 2008) and are stored in the sppLines | |
| -- table. For more on how spectral lines of stars are found, see | |
| -- the SSPP page of the sdss3.org website. | |
| -- This query selects red stars (spectral type K), with large | |
| -- CaII triplet eq widths, with low errors on the CaII triplet | |
| -- equivalent widths. | |
| SELECT | |
| sl.plate,sl.mjd,sl.fiber, | |
| sl.caIIKside,sl.caIIKerr,sl.caIIKmask, | |
| sp.fehadop,sp.fehadopunc,sp.fehadopn, | |
| sp.loggadopn,sp.loggadopunc | |
| FROM sppLines AS sl | |
| JOIN sppParams AS sp ON sl.specobjid = sp.specobjid | |
| WHERE | |
| fehadop < -3.5 | |
| AND fehadopunc between 0.01 | |
| and 0.5 and fehadopn > 3 | |
| </textarea><textarea style="display:none" id="q_1031426103">-- Galaxy counts on HTM grid. | |
| -- | |
| -- Create a count of galaxies for each of the Hierarchical Triangular Mesh (HTM) triangles. | |
| -- Galaxies should satisfy a certain color cut like 0.7u-0.5g-0.2i<1.25 && r<21.75, output | |
| -- it in a form adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE | |
| -- RA/dec cut added to make query run in Quick mode | |
| (ra between 180 and 181 and dec between -1 and 1) and | |
| (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_907308906">-- Binary Stars Colors. | |
| -- | |
| -- Find binary stars with specific colors. | |
| -- At least one of them should have the colors (meets Paul Szkody's color cut) of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1 -- S1 is the white dwarf | |
| JOIN Neighbors N ON S1.objID = N. objID -- N is the precomputed neighbors link | |
| JOIN Star S2 ON S2.objID = N.NeighborObjID -- S2 is the second star | |
| WHERE | |
| N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets the color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_1246974053">-- Galaxies unsaturated near (given) coordinates. | |
| -- | |
| -- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'ORDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy AS G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) AS GN -- this function outputs a table, so we have to do a join | |
| ON G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE | |
| (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_1446002135">-- Search near BCG galaxies. | |
| -- | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- This query has a very complex WHERE clause. | |
| SELECT TOP 1000 G.objID, COUNT(N.NeighborObjID) AS pop | |
| FROM Galaxy AS G -- first gravitational lens candidate | |
| JOIN Neighbors AS N ON G.objID = N.objID -- precomputed list of neighbors | |
| JOIN Galaxy AS U ON U.objID = N.neighborObjID -- a neighbor galaxy of G | |
| JOIN photoZ AS Gpz ON G.objID = Gpz.objID -- photoZ of G. | |
| JOIN photoZ AS Npz ON U.objID = Npz.objID -- neighbor photoZ | |
| WHERE | |
| G.ra BETWEEN 160 AND 170 | |
| AND G.dec BETWEEN -5 AND 5 | |
| AND N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| AND ABS(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| AND (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| AND (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| AND (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| AND G.petroMag_i > 17.5 | |
| AND (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| AND (G.petroMag_r < 30 AND G.g < 30 AND G.r < 30 AND G.i < 30) | |
| AND (G.r < 19.2 | |
| AND ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| AND (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 AND 0.2 ) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| AND (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| AND ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| GROUP BY G.objID | |
| </textarea><textarea style="display:none" id="q_45055564">-- The detectionIndex table contains all detections of a given physical object, | |
| -- which is uniquely identified by the "thingid". In order to extract photometry, | |
| -- you need a join with the PhotoObjAll table, using the objid. | |
| -- There is also a flag field called isPrimary, which is 1 for the object that | |
| -- is found on a primary polygon/field, all the other detections have 0 in this field. | |
| -- Here is a compound query to find all time series around a certain object with a thingid= 97423000 | |
| SELECT | |
| LTRIM(STR(mjd_r,20,2)) AS MJD, | |
| dbo.fSDSS(p.objId) AS ID, | |
| modelMag_g, modelMagErr_g, | |
| modelMag_r, modelMagErr_r, | |
| modelMag_i, modelMagErr_i, p.ra, p.dec | |
| INTO #list | |
| FROM detectionindex d | |
| JOIN PhotoObjAll p ON d.objid=p.objid | |
| JOIN Field f ON p.fieldid=f.fieldid | |
| WHERE d.thingid=97423000 | |
| ORDER BY 1 | |
| GO | |
| -- | |
| -- Now find objects near each of the detections | |
| -- | |
| SELECT a.*, b.* | |
| FROM #list a | |
| CROSS APPLY dbo.fGetNearbyObjEq(a.ra, a.dec, 0.1) b | |
| </textarea><textarea style="display:none" id="q_1674347198">-- The APOGEE survey is conducted along a number of different lines of sight, | |
| -- each referred to as as a "field" or "location" (interchangeably). Each | |
| -- field has a name and an id number (LOCATION_ID). The stars in each field | |
| -- are observed multiple times on multiple visits, on different MJDs. These | |
| -- may involve one or more physical plug plates. | |
| -- To find all the plate visits, one can search as follows (for LOCATION_ID | |
| -- 4105): | |
| SELECT plate, mjd FROM apogeePlate WHERE location_id=4105 | |
| -- The same field can be searched by its name (in this case 'M13'): | |
| SELECT plate, mjd FROM apogeePlate WHERE name = 'M13' | |
| </textarea><textarea style="display:none" id="q_29000041">-- Get ASPCAP parameters and errors for all stars that were targeted as part | |
| -- of the main APOGEE survey: | |
| -- The stellar parameters are available for all stars that had ASPCAP run | |
| -- on them. However, this includes some spectra known to be bad as well as | |
| -- stars targeted as part of ancillary programs of various | |
| -- sorts. Restricting to the good, main survey targets requires checking on | |
| -- target and catalog flags, as in the examples below: | |
| SELECT TOP 100 | |
| s.apogee_id,s.ra, s.dec, s.glon, s.glat, | |
| s.vhelio_avg,s.vscatter, | |
| a.teff, a.teff_err, a.logg, a.logg_err, a.metals, a.metals_err, | |
| a.alphafe, a.alphafe_err, | |
| dbo.fApogeeAspcapFlagN(a.aspcapflag), | |
| dbo.fApogeeStarFlagN(s.starflag) | |
| FROM apogeeStar s | |
| JOIN aspcapStar a on a.apstar_id = s.apstar_id | |
| WHERE (a.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and | |
| s.commiss = 0 and | |
| (s.apogee_target1 & | |
| (dbo.fApogeeTarget1('APOGEE_SHORT')+ | |
| dbo.fApogeeTarget1('APOGEE_INTERMEDIATE')+ | |
| dbo.fApogeeTarget1('APOGEE_LONG'))) != 0 | |
| </textarea><textarea style="display:none" id="q_1193882752">-- Get parameters for all stars with [Fe/H] < -2 with no BAD FLAGS set: | |
| -- You can also select a subset of the stars based on their | |
| -- properties. This example finds a set of metal-poor stars, without any | |
| -- flags set indicating that the observations or analysis is bad. | |
| SELECT TOP 100 | |
| s.apogee_id,s.ra, s.dec, s.glon, s.glat, | |
| s.vhelio_avg,s.vscatter, | |
| a.teff,a.logg, a.metals, a.alphafe, | |
| dbo.fApogeeAspcapFlagN(a.aspcapflag), | |
| dbo.fApogeeStarFlagN(s.starflag) | |
| FROM apogeeStar s | |
| JOIN aspcapStar a on a.apstar_id = s.apstar_id | |
| WHERE (a.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 | |
| and a.teff > 0 and a.metals < -2 | |
| </textarea><textarea style="display:none" id="q_1745805745">-- Get ASPCAP parameters for stars flagged as known cluster members: | |
| -- In addition to selecting main survey targets, you can | |
| -- select other objects according how they were selected. This is | |
| -- an example of selecting objects chosen to be calibrator stars in | |
| -- clusters with known metallicities (APOGEE_CALIB_CLUSTER). | |
| SELECT TOP 100 | |
| s.apogee_id,s.ra, s.dec, s.glon, s.glat, | |
| s.vhelio_avg,s.vscatter, | |
| a.teff, a.teff_err, a.logg, a.logg_err, a.metals, a.metals_err, | |
| a.alphafe, a.alphafe_err, | |
| dbo.fApogeeAspcapFlagN(a.aspcapflag), | |
| dbo.fApogeeStarFlagN(s.starflag) | |
| FROM apogeeStar s | |
| JOIN aspcapStar a on a.apstar_id = s.apstar_id | |
| WHERE (a.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and | |
| s.commiss = 0 and | |
| (s.apogee_target2 & (dbo.fApogeeTarget2('APOGEE_CALIB_CLUSTER')) != 0) | |
| </textarea><textarea style="display:none" id="q_111582421">-- Get proper motions, JHK mag and errors, K-band extinction and radial | |
| -- velocities, for stars with RVs > 300 km/s (with no BAD flags for RVs): | |
| -- There is photometric data associated with each target, including proper | |
| -- motions and other information. This example looks for such information | |
| -- for larger (heliocentric) radial velocity stars. It restricts to objects | |
| -- with good measured ASPCAP parameters. This requires joining the apogeeStar and | |
| -- aspcapStar tables with the apogeeObject table, which has the target information. | |
| SELECT TOP 100 | |
| star.apogee_id, star.ra, star.dec, star.glon, star.glat, | |
| star.vhelio_avg, star.vscatter, | |
| obj.j, obj.h, obj.k, obj.ak_targ, obj.ak_targ_method, obj.ak_wise, | |
| aspcap.teff, aspcap.logg, aspcap.metals | |
| FROM apogeeStar star | |
| JOIN aspcapStar aspcap on aspcap.apstar_id = star.apstar_id | |
| JOIN apogeeObject obj on aspcap.target_id = obj.target_id | |
| WHERE (aspcap.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and aspcap.teff > 0 | |
| and (star.vhelio_avg > 300) and (star.starflag & | |
| dbo.fApogeeStarFlag('SUSPECT_RV_COMBINATION')) = 0 | |
| and star.nvisits > 2 order by aspcap.apogee_id | |
| </textarea><textarea style="display:none" id="q_1441850959">-- Get ASPCAP parameters and targeting flags for all stars with 1 degree of a cluster center: | |
| -- CASJobs allows search for objects near any particular RA and Dec. The | |
| -- following example searches for ASPCAP parameters and targeting flags for | |
| -- the stars observed near M13. | |
| SELECT star.apstar_id, | |
| star.apogee_id, star.ra, star.dec, star.glon, star.glat, | |
| star.apogee_target1, star.apogee_target2, | |
| aspcap.teff,aspcap.logg,aspcap.metals | |
| FROM apogeeStar star | |
| JOIN dbo.fGetNearbyApogeeStarEq(250.423458,36.461306,60) near on | |
| star.apstar_id=near.apstar_id | |
| JOIN aspcapStar aspcap on aspcap.apstar_id = star.apstar_id | |
| </textarea><textarea style="display:none" id="q_988146083"> | |
| -- Get individual RVs from individual visits, the ASPCAP parameters for the combined | |
| -- spectra for stars which have more than 6 visits: | |
| -- Each star is visited several times, and in some case many times, in | |
| -- order to build up signal-to-noise and to detect radial velocity | |
| -- variations. The information about each visit to each star is in the | |
| -- apogeeVisit table. One could join this table with apogeeStar on | |
| -- apogee_id in order to literally find all visits to each star. However, | |
| -- in this example we are interested in just finding those visits that | |
| -- actually contributed to each combined spectrum. In this case, bad visits | |
| -- are excluded and commissioning data and survey data are kept separate | |
| -- (not combined). To find these stars, one may use the apogeeStarVisit | |
| -- table in CAS, or the array visit_pk which exists for each star in the | |
| -- allStar file. Alternatively, if you wanted to find all visits to a | |
| -- particular star, one could replace in the code below apogeeStarVisit | |
| -- with apogeeStarAllVisit and visit_pk with all_visit_pk. | |
| SELECT top 100 | |
| visit.*, aspcap.teff, aspcap.logg, aspcap.metals | |
| FROM apogeeVisit visit | |
| JOIN apogeeStarVisit starvisit on visit.visit_id = starvisit.visit_id | |
| JOIN aspcapStar aspcap on aspcap.apstar_id = starvisit.apstar_id | |
| JOIN apogeeStar star on star.apstar_id = starvisit.apstar_id | |
| WHERE (aspcap.aspcapflag & dbo.fApogeeAspcapFlag('STAR_BAD')) = 0 and aspcap.teff > 0 | |
| and (star.apogee_target1 & dbo.fApogeeTarget1('APOGEE_LONG')) > 0 | |
| and star.nvisits > 6 | |
| ORDER BY visit.apogee_id | |
| </textarea><textarea style="display:none" id="q_197092168">-- Get APOGEE_IDs and SDSS/BOSS plate, mjd, fiberid for all stars that have both APOGEE and SEGUE spectra: | |
| -- A small number of objects have been observed both in the optical with | |
| -- the SDSS and/or BOSS spectrographs and in the infrared with the APOGEE | |
| -- spectrograph. The examples below finds all matches between primary | |
| -- SDSS/BOSS spectra and APOGEE stars with a 3 arcsec tolerance for such | |
| -- cases (note that there are some cases where an entry in one catalog | |
| -- matches multiple entries in the other). | |
| SELECT TOP 50 | |
| specobj.plate as specobj_plate, specobj.mjd as specobj_mjd, | |
| specobj.fiberid as specobj_fiberid, | |
| specobj.ra as specobj_ra, specobj.dec as specobj_dec, | |
| star.apstar_id, star.ra as star_ra, star.dec as star_dec | |
| FROM apogeeStar AS star | |
| CROSS APPLY dbo.fGetNearestSpecObjEq( star.ra, star.dec, 0.05) AS near | |
| JOIN specobj ON near.specobjid=specobj.specobjid | |
| </textarea><textarea style="display:none" id="q_871745526">-- Get SDSS ugriz photometry, errors and flags, ASPCAP parameters for the APOGEE stars with b > 60: | |
| -- In addition to matching to the SDSS spectroscopy, you can also match to | |
| -- the SDSS photometric imaging data. In this case, we only give an example | |
| -- within CAS. To do this purely with flat files requires either | |
| -- downloading the full photometric catalog (about 3 Tbytes) or the | |
| -- "datasweep" files (about 300 Gbytes), both described in the imaging data | |
| -- access documentation, and constructing an efficient flat-file method to | |
| -- do the matching. For most purposes, CAS will be the right way to do this. | |
| SELECT TOP 50 | |
| photoobj.run, photoobj.camcol, photoobj.field, photoobj.obj, | |
| photoobj.psfmag_u, photoobj.psfmag_g, photoobj.psfmag_r, | |
| photoobj.psfmag_i, photoobj.psfmag_z, | |
| photoobj.ra as photoobj_ra, photoobj.dec as photoobj_dec, | |
| star.apstar_id, star.ra as star_ra, star.dec as star_dec, | |
| aspcap.teff, aspcap.metals, aspcap.logg | |
| FROM apogeeStar AS star | |
| CROSS APPLY dbo.fGetNearestObjEq( star.ra, star.dec, 0.05) AS near | |
| JOIN photoobj ON near.objid=photoobj.objid | |
| JOIN aspcapStar as aspcap ON star.apstar_id = aspcap.apstar_id | |
| WHERE star.glat > 60. and aspcap.teff > 0 | |
| </textarea> | |
| <textarea style="display:none" id="q_658663612">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_2046242728">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_100466571">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_473336052">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_1038272356">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1673976505">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_1262886835">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_1206688596">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_1341462147">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1497461636">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_166620452">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_605771979">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_384152764">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_239583990">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_513883755">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_123633451">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_964285562">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1428429823">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1014719417">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_955083894">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_2067166502">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1081925782">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1379940380">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_5571651">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_284612279">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_1514959216">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1269992360">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_1619536327">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_234499396">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_386537157">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_506396296">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_1230693149">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_2026053022">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_643163052">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1483607040">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_1458312124">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_998698239">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_324753475">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_638887334">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_1942123503">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_1122950537">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_203970260">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_155362706">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_2008048623">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_468185944">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1741581729">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_293030657">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_50066576">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1227312257">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1009123441">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_97947386">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_1715812784">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1301593803">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1729284068">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1709778956">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_1346173317">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_874416063">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1426553339">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_2092933015">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_2046005064">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_1937139908">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_1071911477">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1639576493">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_2052665602">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_1227456513">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_1795100394">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_1993463533">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_477859480">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_1558845305">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_30651545">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_598412421">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_834106047">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_190266330">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_399748022">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_168487273">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_1315505534">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_1675888762">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1650901083">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_763893289">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_1725633998">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_1178472613">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_828709702">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_1055252390">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_791936939">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_224126374">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_388139904">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_915208631">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_98652983">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_2027172584">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_730255691">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1691326363">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_1324808024">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_51406064">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1713458572">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_70783942">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_1804705991">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_167002323">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_834596942">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1424444742">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_175511087">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_1053909050">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_622853371">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_510380354">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_963813061">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_23925016">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_1398357282">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1944663326">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_166816670">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_314022943">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_2121237275">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_706908036">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_1510674311">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_342684245">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1821885322">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_654356252">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_420853709">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_631175478">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1165868693">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_1514903499">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_214576614">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_619033119">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1653404421">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_1527039772">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_1055015502">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1131150381">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_859289958">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1033172010">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_976449187">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_1404790795">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1368831015">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_642208693">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_674238270">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_1020817074">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_1695980969">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1794028875">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_875447540">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_408046859">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_2023911456">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_1739829469">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_1716646730">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_856840643">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_211714083">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_137356135">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_1480779043">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_1195248688">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_1747257364">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_1374627809">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_1381525768">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_909071920">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1357802971">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_1954141537">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_545014296">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_547865327">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_716142064">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_272200048">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_753648351">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1150951472">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_106085622">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_1713017857">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_270075329">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1540370546">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_365239915">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_179278427">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_2005973150">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_1400899770">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1330058026">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1048676048">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_53648337">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_1793902941">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_1876907516">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1499026876">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_253037019">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_627065552">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_873473743">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_1226072052">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_1201934799">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_1778610482">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_2026496616">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_813213932">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_1470069848">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_1442356757">-- Basic_SELECT_FROM_WHERE | |
| -- Find objects in a particular field. | |
| SELECT objID, | |
| field, ra, dec -- Get the unique object ID, field number, and coords | |
| FROM PhotoObj -- From the photometric data | |
| WHERE fieldID = 587722951961673728 -- that is in a specific field | |
| </textarea><textarea style="display:none" id="q_25768111">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 17, where the local | |
| -- extinction is > 0.275. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| -- | |
| -- Finds 6604 galaxies in under 10 mins on DR2, but beware that increasing | |
| -- the limiting r magnitude will significantly add to the execution time. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE | |
| r < 17 -- r IS NOT deredenned | |
| and extinction_r > 0.275 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_836207046">-- Find all objects with unclassified spectra. | |
| -- A simple SELECT-FROM-WHERE query, using a function | |
| -- | |
| -- On DR2, returns 3109 rows in 20 sec. | |
| SELECT specObjID | |
| FROM SpecObj | |
| WHERE SpecClass = dbo.fSpecClass('UNKNOWN')</textarea><textarea style="display:none" id="q_1444654077">-- Galaxies meeting multiple simple criteria. | |
| -- Find all galaxies with blue surface brightness between 23 and 25 | |
| -- mag per square arcseconds, and -10 < supergalactic latitude (sgb) < 10, and | |
| -- declination less than zero. Currently, we have to live with ra/dec until we | |
| -- get galactic coordinates. To calculate surface brightness per sq. arcsec, | |
| -- we use (g + rho), where g is the blue magnitude, and rho= 5*log(r). This | |
| -- query now has three requirements, one involving simple math. | |
| -- | |
| -- On DR2, returns 61090 rows in 330 sec. | |
| SELECT objID | |
| FROM Galaxy | |
| WHERE ra between 178 and 180 | |
| and dec < 0 | |
| -- and (g+rho) between 23 and 25 | |
| and g between (23-rho) and (25-rho) | |
| -- g is the blue magnitude, and rho= 5*log(Petro radius)</textarea><textarea style="display:none" id="q_824393739">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- Finds 100 galaxies in 230 sec on DR2, but this is a very slow way to do | |
| -- coordinate cuts. Using RA/dec is *much* faster due to indexing. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_1467158080">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| -- | |
| -- Finishes in 72 sec on DR2. | |
| SELECT TOP 10000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_922576218">-- Getting a subsample of the data. | |
| -- Uses the integer short object id (obj) and the '%' syntax (like awk) | |
| -- to get every 1000th object. THIS IS NOT A TRULY RANDOM SUBSET! | |
| -- | |
| -- Returns 11367 objects in DR2 (in about 10-15mins). | |
| SELECT u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_256345731">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_1261782764">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 1000 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1772065995">-- Using the BETWEEN syntax. | |
| -- Find galaxies with an isophotal surface brightness (SB) larger | |
| -- than 24 in the red band, and with an ellipticity > 0.5, and with the major | |
| -- axis of the ellipse having a declination between 30" and 60" arc seconds. | |
| -- This is also a simple query that uses a WHERE clause with three conditions | |
| -- that must be met. We introduce the syntax 'BETWEEN' to do a range search. | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy | |
| WHERE r < 24 - rho | |
| -- surface brightness brighter than 24 mag. per sq. arcsec in the red | |
| -- Note that isolating r (indexed) on one side helps this run faster | |
| and isoA_r between 30 and 60 | |
| -- major axis between 30" and 60" | |
| and (power(q_r,2) + power(u_r,2)) > 0.25 | |
| -- square of ellipticity is > 0.5 squared. The SQL term 'power' is used for exponentiation.</textarea><textarea style="display:none" id="q_731851157">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| --This Sample Query will not work for SDSS3 contexts | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_197942948">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 1000 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_307791979">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_663453829">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you ,ust specify which table each quantity in the SELECT | |
| -- clause comes from. Finally, the last line in the query is the join between | |
| -- the two tables, which is achieved by requiring that a quantity present in | |
| -- both tables be equal. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z --get the ObjID and final mags | |
| FROM Galaxy G, Star S -- use two Views, Galaxy and Star, as a convenient mechanism to compare objects | |
| WHERE G.parentID > 0 -- galaxy has a "parent", which tells us this object was deblended | |
| and G.parentID = S.parentID -- and the star has the same parent | |
| </textarea><textarea style="display:none" id="q_1970118298">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s, Field f | |
| WHERE s.fieldID = f.fieldID | |
| and s.psfMag_g < 20 | |
| and f.pspStatus = 2</textarea><textarea style="display:none" id="q_1322104004">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| -- NOTE: This query times out (takes too long) without the "TOP 1000". | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r | |
| FROM | |
| photoObj p, field f | |
| WHERE | |
| f.fieldid = p.fieldid | |
| and f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_488717385">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. | |
| SELECT TOP 10 P.ObjID -- distinct cases | |
| FROM PhotoPrimary P, -- P is the primary object | |
| Neighbors N, -- N is the neighbor link | |
| PhotoPrimary L -- L is the lens candidate of P | |
| WHERE P.ObjID = N.ObjID -- N is a neighbor record | |
| and L.ObjID = N.NeighborObjID -- L is a neighbor of P | |
| and P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra. | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_666094160">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1391190496">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or their sum is zero. | |
| -- (From Gordon Richards) | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr)</textarea><textarea style="display:none" id="q_12263065">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. NOTE THAT THE | |
| -- NAMES and VALUES OF THE LIKELIHOODS HAVE CHANGED SINCE THE EDR; they are | |
| -- now log likelihoods, and named accordingly (lDev is now lnlDev, etc.) to | |
| -- indicate these are log likelihoods. This query has many conditions, and | |
| -- also has the use of bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_1540682795">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1674685583">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| SELECT TOP 1000 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_335683413">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query. | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) -- i and z in primary tables DO NOT include extinction</textarea><textarea style="display:none" id="q_1986785076">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) )</textarea><textarea style="display:none" id="q_279312168">-- Find galaxies with specific spectra. | |
| -- Namely, they have an equivalent width in | |
| -- H_alpha > 40 Angstroms. We want object ID's from the photometry (Galaxy) | |
| -- but constraints from spectroscopy. The line widths and IDs are stored in | |
| -- SpecLine. --This is a simple query, but now we are using three tables. The | |
| -- spectroscopy tables of measured lines are arranged non-intuitively, and we | |
| -- urge users to read about them on the DAS help pages. --IMPORTANT NOTE: | |
| -- Each spectroscopic object now has a match to at least two photometric | |
| -- objects, one in Target and one in Best. Therefore, when performing a join | |
| -- between spectroscopic photometric objects, you must specify either | |
| -- PhotoObj.ObjID=SpecObj.bestObjID or PhotoObj.ObjID = SpecObj.targetObjID. | |
| -- Normally, the default photometric database is BEST, so you will want to use | |
| -- SpecObj.bestObjID | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- we want the photometric ObjID | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L, -- L is a line of S | |
| SpecLineNames as LN -- the names of the lines | |
| WHERE G.ObjID = S.bestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- and the spectral line L is detected in the spectrum | |
| and L.LineId = LN.value -- L is the H alpha line | |
| and LN.name = 'Ha_6565' | |
| and L.ew > 40 -- and H alpha is at least 40 angstroms wide. | |
| </textarea><textarea style="display:none" id="q_168810913">-- Find galaxies with more specific spectra. | |
| -- Same as prior query, but also require weak Hbeta line (Halpha/Hbeta > 20.) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT G.ObjID -- return qualifying galaxies | |
| FROM Galaxy as G, -- G is the galaxy | |
| SpecObj as S, -- S is the spectra of galaxy G | |
| SpecLine as L1, -- L1 is a line of S | |
| SpecLine as L2, -- L2 is a second line of S | |
| specLineNames as LN1, -- the names of the lines (Halpha) | |
| specLineNames as LN2 -- the names of the lines (Hbeta) | |
| WHERE G.ObjID = S.BestObjID -- connect the galaxy to the spectrum | |
| and S.SpecObjID = L1.SpecObjID -- L1 is a line of S. | |
| and S.SpecObjID = L2.SpecObjID -- L2 is a line of S. | |
| and L1.LineId = LN1. value | |
| and LN1.name = 'Ha_6565' -- L1 is the H alpha line | |
| and L2.LineId = LN2.value -- L2 is the H alpha line | |
| and LN2.name = 'Hb_4863' -- | |
| and L1.ew > 200 -- BIG Halpha | |
| and L2.ew > 10 -- significant Hbeta emission line | |
| and L2.ew * 20 < L1.ew -- Hbeta is comparatively small | |
| </textarea><textarea style="display:none" id="q_1868611009">-- Find binary stars with specific colors. | |
| -- At least one of them should have the colors of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1, -- S1 is the white dwarf | |
| Neighbors N, -- N is the precomputed neighbors links | |
| Star S2 -- S2 is the second star | |
| WHERE S1.objID = N. objID -- S1 and S2 are neighbors-within 30 arc sec | |
| and S2.objID = N.NeighborObjID | |
| and N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets Paul Szkodys color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_686166294">-- Find quasars with a broad absorption line and a nearby galaxy. | |
| -- within 10 arcseconds. | |
| -- Return both the quasars and the galaxies. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT Q.BestObjID as Quasar_candidate_ID , G.ObjID as Galaxy_ID, N.distance | |
| FROM SpecObj as Q, -- Q is the specObj of the quasar candidate | |
| Neighbors as N, -- N is the Neighbors list of Q | |
| Galaxy as G, -- G is the nearby galaxy | |
| SpecClass as SC, -- Spec Class | |
| SpecLine as L, -- L is the broad line we are looking for | |
| SpecLineNames as LN -- Line Name | |
| WHERE Q.SpecClass =SC.value -- Q is a QSO | |
| and SC.name in ('QSO', 'HIZ_QSO') -- Spectrum says "QSO" | |
| and Q.SpecObjID = L.SpecObjID -- L is a spectral line of Q. | |
| and L.LineID = LN.value -- line found and | |
| and LN.Name != 'UNKNOWN' -- not not identified | |
| and L.ew < -10 -- but its a prominent absorption line | |
| and Q.BestObjID = N.ObjID -- N is a neighbor record | |
| and G.ObjID = N.NeighborObjID -- G is a neighbor of Q | |
| and N.distance < 10.0/60 -- and it is within 10 arcseconds of the Q. | |
| </textarea><textarea style="display:none" id="q_2089021461">-- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'orDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy as G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) as GN -- this function outputs a table, so we have to do a join | |
| on G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_535089494">-- Ellipticals with odd lines. | |
| -- Find all elliptical galaxies with spectra that have an anomalous | |
| -- emission line. This query introduces the SQL syntax DISTINCT, which will | |
| -- return only one instance of the requested parameter (ObjID, in this case), | |
| -- because our query may return the same object more than once. This is also | |
| -- the first nested query, where we use one SELECT (the inner one) to get a | |
| -- group of objects we are not interested in. The outer SELECT includes the | |
| -- new syntax 'not in', which is used to perform the exclusion. | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT DISTINCT G.ObjID -- return qualifying galaxies | |
| FROM | |
| Galaxy as G, -- G is the galaxy | |
| SpecObjAll as S, -- S is the spectra of galaxy G | |
| SpecLineAll as L, -- L is a line of S | |
| -- we must use SpecLineAll because SpecLine only has ID's lines | |
| XCRedshift as XC -- the template cross-correlation redshift | |
| WHERE G.ObjID = S.bestObjID -- connect galaxy to the spectrum | |
| and S.SpecObjID = L.SpecObjID -- The line L must be in the spectrum S | |
| and S.SpecObjID = XC.SpecObjID -- and there is a crosscorrelation redshift | |
| and XC.tempNo = 8 -- Template('Elliptical') -- best Cross correlation template used is "elliptical" | |
| and L.LineID = 0 | |
| and L.ew > 10 -- and the line is prominent by some definition, in this case, the equivalent width is over 10 Angstroms | |
| and S.SpecObjID not in ( | |
| -- insist that there are no other lines | |
| SELECT S.SpecObjID -- This is the chosen line. | |
| FROM SpecLine as L1 -- L1 is another line... | |
| -- by using SpecLine, we are automatically requiring that the line | |
| -- be identified | |
| WHERE S.SpecObjID = L1.SpecObjID -- ...for this object... | |
| and abs(L.wave - L1.wave) <.01 | |
| -- ...at nearly the same wavelength... | |
| ) | |
| </textarea><textarea style="display:none" id="q_1581828007">-- Search near BCG galaxies. | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- An extremely complex WHERE clause. | |
| SELECT G.objID, count(N.NeighborObjID) as pop | |
| FROM Galaxy as G, -- first gravitational lens candidate | |
| Neighbors as N, -- precomputed list of neighbors | |
| Galaxy as U, -- a neighbor galaxy of G | |
| photoZ as Gpz, -- photoZ of G. | |
| photoZ as Npz -- Neighbor photoZ | |
| WHERE G.ra between 160 and 170 | |
| and G.dec between -5 and 5 | |
| and G.objID = N.objID -- connect G and U via the neighbors table | |
| and U.objID = N.neighborObjID -- so that we know G and U are within | |
| and N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| and G.objID = Gpz.objID | |
| and U.objID = Npz.objID | |
| and abs(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| and G.petroMag_i > 17.5 | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r < 30 and G.g < 30 and G.r < 30 and G.i < 30) | |
| and (G.r < 19.2 | |
| and ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| and (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 and 0.2 ) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| and (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| and ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| and ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| group by G.objID | |
| </textarea><textarea style="display:none" id="q_1954768468">-- Broadest line of each spectrum with its ID. | |
| -- (or more generally, all the columns for | |
| -- the spectral line with the highest/lowest something)? The line width is | |
| -- stored in the column sigma, the identification is in the column restwave. | |
| -- (Sebastian Jester ) | |
| -- | |
| --This Sample Query will not work for SDSS3 DR8 contexts | |
| SELECT | |
| L.specObjId, | |
| L.specLineID, | |
| sMax.Maxwidth -- get the spectroscopic object ID, the line ID, and the width | |
| FROM specLine L, | |
| (SELECT specObjID, | |
| Max(waveMax-waveMin) as MaxWidth | |
| -- Define MaxWidth as the largest difference in the min and max wavelength of | |
| -- an identified line, using the built-in Max function of SQL | |
| FROM SpecLine | |
| GROUP BY specObjID) as sMax | |
| -- sMax contains a single specObjID and MaxWidth. Remember that for each line | |
| -- identified in a given object's spectrum, there is an entry in | |
| -- SpecLine. This means that each specObjID appears many times in SpecLine, | |
| -- once for each line found, and they must be aggregated before performing any | |
| -- operation such as Max. The GROUP BY is thus NECESSARY. | |
| -- The upper FROM clause is telling us we will use the table SpecLine and this | |
| -- new output called sMax, which contains one entry with the SpecObjID and | |
| -- MaxWidth. If we used some other function instead of 'Max', such as 'top | |
| -- 10', sMax would have more than row. | |
| WHERE | |
| L.specObjID = sMax.specObjID | |
| and (L.waveMax-L.waveMin) = sMax.MaxWidth | |
| -- Just as with the specObjID, each specLineID appears many times in specLine. | |
| -- This final WHERE clause makes sure we get the one specLineID from SpecObj | |
| -- which matches the unique combination of specObjID and MaxWidth in sMax. | |
| </textarea><textarea style="display:none" id="q_1311402765">-- Gridded galaxy counts and masks. Actually consists of TWO queries: | |
| -- 1) Create a gridded count of galaxies with u-g > 1 and r < 21.5 over -1 < dec < 1, | |
| -- and 179 < R.A. < 181, on a grid, and create a map of masks over the same grid. | |
| -- Scan the table for galaxies and group them in cells 2 arc-minuteson a side. Provide | |
| -- predicates for the color restrictions on u-g and r and to limit the search to the | |
| -- portion of the sky defined by the right ascension and declination conditions. Return | |
| -- the count of qualifying galaxies in each cell. | |
| -- 2) Run another query with the same grouping, but with a predicate to include only | |
| -- objects such as satellites, planets, and airplanes that obscure the cell. The second | |
| -- query returns a list of cell coordinates that serve as a mask for the first query. | |
| --- First find the gridded galaxy count (with the color cut) | |
| --- In local tangent plane, ra/cos(dec) is a linear degree. | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM Galaxy as G | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON G.htmID BETWEEN T.HTMIDstart AND T. HTMIDend | |
| WHERE ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and u-g > 1 | |
| and r < 21.5 | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 | |
| -- now build mask grid. | |
| -- This is a separate query if no temp tables can be made | |
| SELECT cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0 as raCosDec, | |
| cast(dec*30 as int)/30.0 as dec, | |
| count(*) as pop | |
| FROM PhotoObj as PO | |
| JOIN dbo.fHTMCoverRegion('CHULL J2000 179 -1 179 1 181 1 181 -1') AS T | |
| ON PO.htmID BETWEEN T.HTMIDstart AND T.HTMIDend | |
| JOIN PhotoType as PT ON PO.type = PT.value | |
| WHERE | |
| ra between 179 and 181 | |
| and dec between -1 and 1 | |
| and PT.name in ('COSMIC_RAY', 'DEFECT', 'GHOST', 'TRAIL', 'UNKNOWN') | |
| GROUP BY cast((ra/cos(cast(dec*30 as int)/30.0))*30 as int)/30.0, | |
| cast(dec*30 as int)/30.0 </textarea><textarea style="display:none" id="q_1594656083">-- Create a count of galaxies for each of the HTM triangles. | |
| -- Galaxies should satisfy a certain color cut, | |
| -- like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form | |
| -- adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1399733903">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_532479277">-- This query uses the new SQL Server 2005 CROSS APPLY and OUTER APPLY | |
| -- constructs to apply a table-valued function to the results of a query. | |
| -- In this example, we use the fFootPrintEq function which returns a list | |
| -- of SDSS regions that intersect the area specified by the RA, dec and | |
| -- radius, or NULL if the area is outside the SDSS footprint. | |
| -- For each point in the input list, in this case the result of a query | |
| -- on PhotoObj, return "yes" or "no" depending on whether the point is in | |
| -- the SDSS footprint or not, and any other needed columns. | |
| SELECT top 100 objID, ra, dec, | |
| (case when p.type is null then 'NO' else 'YES' end) as found | |
| FROM PhotoObj AS p | |
| OUTER APPLY dbo.fFootprintEq(ra,dec,0.1) | |
| WHERE (ra between 179.5 and 182.3) and (dec between -1.0 and 1.8) | |
| </textarea> | |
| <textarea style="display:none" id="q_1774811490">-- Find unique objects in an RA/Dec box. | |
| -- PhotoPrimary is a view which selects only unique objects. | |
| -- The full list of good detections including duplicates is in PhotoObj | |
| -- A basic SELECT-FROM-WHERE query. | |
| SELECT TOP 100 objID, -- Get the unique object ID, | |
| field, ra, dec -- the field number, and coordinates | |
| FROM PhotoPrimary -- From the photometric data | |
| WHERE | |
| ra > 185. and ra < 185.1 and dec > 15. and dec < 15.1 </textarea><textarea style="display:none" id="q_1950906038">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 22, where the local | |
| -- extinction is > 0.175. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| SELECT TOP 10 objID | |
| FROM Galaxy | |
| WHERE | |
| r < 22 -- r IS NOT deredenned | |
| and extinction_r > 0.175 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_118442681">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_1087655456">-- Using the BETWEEN syntax. | |
| -- Find all galaxies in a certain area of the sky that also meet other | |
| -- criteria in their measured parameters. This query intriduces the | |
| -- BETWEEN construct to specify a range of values. | |
| SELECT TOP 100 objID, ra, dec, cModelMag_g | |
| FROM Galaxy | |
| WHERE ra BETWEEN 178 AND 180 | |
| AND dec < 0 | |
| AND cModelMag_g BETWEEN 18 AND 19 | |
| </textarea><textarea style="display:none" id="q_1315557362">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- NOTE: This query must be run in batch mode, i.e. using the Submit button | |
| -- because it takes too long to execute in Quick mode. | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_671661625">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_474354453">-- Getting a subsample of the data. | |
| -- | |
| -- Uses the integer short object id (obj) - which is the least significant bits | |
| -- of the long objID - and the '%' operator (remainder) to get every 1000th | |
| -- object. | |
| -- NOTE: THIS IS NOT A TRULY RANDOM SAMPLE! | |
| SELECT TOP 100 u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_765492618">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_453245167">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 10 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1745962591">-- Finding galaxies by their emission lines: | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Spectra of Red | |
| -- Stars" sample query for an example of using stellar spectra. | |
| -- | |
| -- Spectral lines for galaxies are calculated using the MPA-JHU | |
| -- spectroscopic reanalysis (Tremonti et al. 2004; Brinchmann et al. 2004) | |
| -- and are stored in the galSpecLine table. For more on how spectral lines | |
| -- of galaxies are found, see the Galspec page of the sdss3.org website. | |
| -- | |
| -- This query selects galaxy spectra with high internal reddening, | |
| -- as measured by the standard Balmer decrement technique. It | |
| -- makes use of the galSpec tables for the measurements of | |
| -- galaxy lines. In this case we use galSpecLine, which has | |
| -- emission line measurements. | |
| SELECT | |
| s.plate, s.fiberid, s.mjd, s.z, s.zwarning, | |
| g.h_beta_flux, g.h_beta_flux_err, | |
| g.h_alpha_flux, g.h_alpha_flux_err | |
| FROM GalSpecLine AS g | |
| JOIN dbo.SpecObj AS s ON s.specobjid = g.specobjid | |
| WHERE | |
| h_alpha_flux > h_alpha_flux_err*5 | |
| AND h_beta_flux > h_beta_flux_err*5 | |
| AND h_beta_flux_err > 0 | |
| AND h_alpha_flux > 10.*h_beta_flux | |
| AND s.class = 'GALAXY' | |
| AND s.zwarning = 0 | |
| </textarea><textarea style="display:none" id="q_23566870">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| -- NOTE: Since asteroids are rare objects in the SDSS data, this query will | |
| -- take a long time to run without the "TOP 10" and should be executed | |
| -- in batch mode (with the Submit button). | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_225105383">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_834528110">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| -- An area restriction is added so the query will run in the Quick queue. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE | |
| (ra between 180 and 190) and (dec between -5 and 5) | |
| and (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_245836436">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you must specify which table each quantity in the SELECT | |
| -- clause comes from. The query illustrates the JOIN syntax between | |
| -- the two tables, which requires that a common quantity that is present in | |
| -- both tables be equal, in this case their common parent object. | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z | |
| FROM Galaxy G -- compare Galaxy and Star | |
| JOIN Star S ON G.parentID = S.parentID -- using the same parent | |
| WHERE | |
| G.parentID > 0 -- if the galaxy has a "parent", this object was deblended | |
| </textarea><textarea style="display:none" id="q_1952789469">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s | |
| JOIN Field f ON s.fieldID = f.fieldID | |
| WHERE | |
| s.psfMag_g < 20 | |
| and f.pspStatus = 2 | |
| </textarea><textarea style="display:none" id="q_1577813389">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r, | |
| r.stripe, | |
| r.strip | |
| FROM | |
| photoObj p | |
| JOIN field f ON f.fieldid = p.fieldid | |
| JOIN run r ON r.run=f.run | |
| WHERE | |
| f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1362554404">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. This query introduces the | |
| -- Neighbors table, which is a pre-computed list of the nearest | |
| -- neighbors of each object within 30 arcseconds. | |
| SELECT TOP 10 P.ObjID as objid1, L.ObjID as objid2, N.distance | |
| FROM PhotoPrimary P -- P is the primary object | |
| JOIN Neighbors N ON P.ObjID = N.ObjID -- N is the neighbor link | |
| JOIN PhotoPrimary L ON L.ObjID = N.NeighborObjID -- L is the lens candidate of P | |
| WHERE | |
| P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1335992021">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_999622185">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or that their sum is zero. | |
| -- (From Gordon Richards) | |
| -- | |
| -- NOTE: A caveat about using functons (like fPhotoFlags) is that if your | |
| -- query is selecting a very large number of rows (e.g. hundreds of | |
| -- thousands or millions) then it's that many function calls, and | |
| -- this will slow down the query execution significantly. In that | |
| -- case, you should replace the function call with its equivalent | |
| -- binary bitmask, e.g. if you run the query (with Quick button) | |
| -- SELECT (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT')) | |
| -- you will get the value 36507222016, which you can substitute in | |
| -- first line of the WHERE clause below as: | |
| -- (flags & 36507222016) > 0 | |
| -- to avoid zillions of function calls. | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr) | |
| </textarea><textarea style="display:none" id="q_416441924">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. | |
| -- This query has many conditions, and also shows more of the | |
| -- bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_2043177420">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_538360056">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| -- Another query that makes extensive use of photo flags to get a sample | |
| -- of galaxies within a size range as specified by their i-band Petrosian | |
| -- radius. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1596667058">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query but selects galaxies that | |
| -- are red (i-z color greater than a certain threshold). | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) | |
| </textarea><textarea style="display:none" id="q_1317231909">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests that selects Luminous | |
| -- Red Galaxies (LRGs). | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) ) | |
| </textarea><textarea style="display:none" id="q_1838668250">-- Spectra of Red Stars | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Galaxies with | |
| -- Emission Lines" sample query for an example of using galaxy spectra. | |
| -- | |
| -- Spectral lines for stars are calculated using the SEGUE Stellar Parameter | |
| -- Pipeline (SSPP; Lee et al. 2008) and are stored in the sppLines | |
| -- table. For more on how spectral lines of stars are found, see | |
| -- the SSPP page of the sdss3.org website. | |
| -- This query selects red stars (spectral type K), with large | |
| -- CaII triplet eq widths, with low errors on the CaII triplet | |
| -- equivalent widths. | |
| SELECT | |
| sl.plate,sl.mjd,sl.fiber, | |
| sl.caIIKside,sl.caIIKerr,sl.caIIKmask, | |
| sp.fehadop,sp.fehadopunc,sp.fehadopn, | |
| sp.loggadopn,sp.loggadopunc | |
| FROM sppLines AS sl | |
| JOIN sppParams AS sp ON sl.specobjid = sp.specobjid | |
| WHERE | |
| fehadop < -3.5 | |
| AND fehadopunc between 0.01 | |
| and 0.5 and fehadopn > 3 | |
| </textarea><textarea style="display:none" id="q_2014769771">-- Galaxy counts on HTM grid. | |
| -- | |
| -- Create a count of galaxies for each of the Hierarchical Triangular Mesh (HTM) triangles. | |
| -- Galaxies should satisfy a certain color cut like 0.7u-0.5g-0.2i<1.25 && r<21.75, output | |
| -- it in a form adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE | |
| -- RA/dec cut added to make query run in Quick mode | |
| (ra between 180 and 181 and dec between -1 and 1) and | |
| (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1687012106">-- Binary Stars Colors. | |
| -- | |
| -- Find binary stars with specific colors. | |
| -- At least one of them should have the colors (meets Paul Szkody's color cut) of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1 -- S1 is the white dwarf | |
| JOIN Neighbors N ON S1.objID = N. objID -- N is the precomputed neighbors link | |
| JOIN Star S2 ON S2.objID = N.NeighborObjID -- S2 is the second star | |
| WHERE | |
| N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets the color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_1632881509">-- Galaxies unsaturated near (given) coordinates. | |
| -- | |
| -- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'ORDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy AS G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) AS GN -- this function outputs a table, so we have to do a join | |
| ON G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE | |
| (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_103654135">-- Search near BCG galaxies. | |
| -- | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- This query has a very complex WHERE clause. | |
| SELECT TOP 1000 G.objID, COUNT(N.NeighborObjID) AS pop | |
| FROM Galaxy AS G -- first gravitational lens candidate | |
| JOIN Neighbors AS N ON G.objID = N.objID -- precomputed list of neighbors | |
| JOIN Galaxy AS U ON U.objID = N.neighborObjID -- a neighbor galaxy of G | |
| JOIN photoZ AS Gpz ON G.objID = Gpz.objID -- photoZ of G. | |
| JOIN photoZ AS Npz ON U.objID = Npz.objID -- neighbor photoZ | |
| WHERE | |
| G.ra BETWEEN 160 AND 170 | |
| AND G.dec BETWEEN -5 AND 5 | |
| AND N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| AND ABS(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| AND (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| AND (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| AND (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| AND G.petroMag_i > 17.5 | |
| AND (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| AND (G.petroMag_r < 30 AND G.g < 30 AND G.r < 30 AND G.i < 30) | |
| AND (G.r < 19.2 | |
| AND ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| AND (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 AND 0.2 ) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| AND (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| AND ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| GROUP BY G.objID | |
| </textarea><textarea style="display:none" id="q_675428088">-- The detectionIndex table contains all detections of a given physical object, | |
| -- which is uniquely identified by the "thingid". In order to extract photometry, | |
| -- you need a join with the PhotoObjAll table, using the objid. | |
| -- There is also a flag field called isPrimary, which is 1 for the object that | |
| -- is found on a primary polygon/field, all the other detections have 0 in this field. | |
| -- Here is a compound query to find all time series around a certain object with a thingid= 97423000 | |
| SELECT | |
| LTRIM(STR(mjd_r,20,2)) AS MJD, | |
| dbo.fSDSS(p.objId) AS ID, | |
| modelMag_g, modelMagErr_g, | |
| modelMag_r, modelMagErr_r, | |
| modelMag_i, modelMagErr_i, p.ra, p.dec | |
| INTO #list | |
| FROM detectionindex d | |
| JOIN PhotoObjAll p ON d.objid=p.objid | |
| JOIN Field f ON p.fieldid=f.fieldid | |
| WHERE d.thingid=97423000 | |
| ORDER BY 1 | |
| GO | |
| -- | |
| -- Now find objects near each of the detections | |
| -- | |
| SELECT a.*, b.* | |
| FROM #list a | |
| CROSS APPLY dbo.fGetNearbyObjEq(a.ra, a.dec, 0.1) b | |
| </textarea> | |
| <textarea style="display:none" id="q_1651054877">-- Find unique objects in an RA/Dec box. | |
| -- PhotoPrimary is a view which selects only unique objects. | |
| -- The full list of good detections including duplicates is in PhotoObj | |
| -- A basic SELECT-FROM-WHERE query. | |
| SELECT TOP 100 objID, -- Get the unique object ID, | |
| field, ra, dec -- the field number, and coordinates | |
| FROM PhotoPrimary -- From the photometric data | |
| WHERE | |
| ra > 185. and ra < 185.1 and dec > 15. and dec < 15.1 </textarea><textarea style="display:none" id="q_229416785">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 22, where the local | |
| -- extinction is > 0.175. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| SELECT TOP 10 objID | |
| FROM Galaxy | |
| WHERE | |
| r < 22 -- r IS NOT deredenned | |
| and extinction_r > 0.175 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_639018260">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_906922939">-- Using the BETWEEN syntax. | |
| -- Find all galaxies in a certain area of the sky that also meet other | |
| -- criteria in their measured parameters. This query intriduces the | |
| -- BETWEEN construct to specify a range of values. | |
| SELECT TOP 100 objID, ra, dec, cModelMag_g | |
| FROM Galaxy | |
| WHERE ra BETWEEN 178 AND 180 | |
| AND dec < 0 | |
| AND cModelMag_g BETWEEN 18 AND 19 | |
| </textarea><textarea style="display:none" id="q_1646205417">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- NOTE: This query must be run in batch mode, i.e. using the Submit button | |
| -- because it takes too long to execute in Quick mode. | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_150519266">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_943895088">-- Getting a subsample of the data. | |
| -- | |
| -- Uses the integer short object id (obj) - which is the least significant bits | |
| -- of the long objID - and the '%' operator (remainder) to get every 1000th | |
| -- object. | |
| -- NOTE: THIS IS NOT A TRULY RANDOM SAMPLE! | |
| SELECT TOP 100 u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_1380995089">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_2032074038">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 10 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_77418842">-- Finding galaxies by their emission lines: | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Spectra of Red | |
| -- Stars" sample query for an example of using stellar spectra. | |
| -- | |
| -- Spectral lines for galaxies are calculated using the MPA-JHU | |
| -- spectroscopic reanalysis (Tremonti et al. 2004; Brinchmann et al. 2004) | |
| -- and are stored in the galSpecLine table. For more on how spectral lines | |
| -- of galaxies are found, see the Galspec page of the sdss3.org website. | |
| -- | |
| -- This query selects galaxy spectra with high internal reddening, | |
| -- as measured by the standard Balmer decrement technique. It | |
| -- makes use of the galSpec tables for the measurements of | |
| -- galaxy lines. In this case we use galSpecLine, which has | |
| -- emission line measurements. | |
| SELECT | |
| s.plate, s.fiberid, s.mjd, s.z, s.zwarning, | |
| g.h_beta_flux, g.h_beta_flux_err, | |
| g.h_alpha_flux, g.h_alpha_flux_err | |
| FROM GalSpecLine AS g | |
| JOIN dbo.SpecObj AS s ON s.specobjid = g.specobjid | |
| WHERE | |
| h_alpha_flux > h_alpha_flux_err*5 | |
| AND h_beta_flux > h_beta_flux_err*5 | |
| AND h_beta_flux_err > 0 | |
| AND h_alpha_flux > 10.*h_beta_flux | |
| AND s.class = 'GALAXY' | |
| AND s.zwarning = 0 | |
| </textarea><textarea style="display:none" id="q_436084239">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| -- NOTE: Since asteroids are rare objects in the SDSS data, this query will | |
| -- take a long time to run without the "TOP 10" and should be executed | |
| -- in batch mode (with the Submit button). | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_352254942">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1677687603">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| -- An area restriction is added so the query will run in the Quick queue. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE | |
| (ra between 180 and 190) and (dec between -5 and 5) | |
| and (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1019428081">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you must specify which table each quantity in the SELECT | |
| -- clause comes from. The query illustrates the JOIN syntax between | |
| -- the two tables, which requires that a common quantity that is present in | |
| -- both tables be equal, in this case their common parent object. | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z | |
| FROM Galaxy G -- compare Galaxy and Star | |
| JOIN Star S ON G.parentID = S.parentID -- using the same parent | |
| WHERE | |
| G.parentID > 0 -- if the galaxy has a "parent", this object was deblended | |
| </textarea><textarea style="display:none" id="q_1340958328">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s | |
| JOIN Field f ON s.fieldID = f.fieldID | |
| WHERE | |
| s.psfMag_g < 20 | |
| and f.pspStatus = 2 | |
| </textarea><textarea style="display:none" id="q_1563485422">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r, | |
| r.stripe, | |
| r.strip | |
| FROM | |
| photoObj p | |
| JOIN field f ON f.fieldid = p.fieldid | |
| JOIN run r ON r.run=f.run | |
| WHERE | |
| f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_466532201">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. This query introduces the | |
| -- Neighbors table, which is a pre-computed list of the nearest | |
| -- neighbors of each object within 30 arcseconds. | |
| SELECT TOP 10 P.ObjID as objid1, L.ObjID as objid2, N.distance | |
| FROM PhotoPrimary P -- P is the primary object | |
| JOIN Neighbors N ON P.ObjID = N.ObjID -- N is the neighbor link | |
| JOIN PhotoPrimary L ON L.ObjID = N.NeighborObjID -- L is the lens candidate of P | |
| WHERE | |
| P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_1381126224">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_570846738">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or that their sum is zero. | |
| -- (From Gordon Richards) | |
| -- | |
| -- NOTE: A caveat about using functons (like fPhotoFlags) is that if your | |
| -- query is selecting a very large number of rows (e.g. hundreds of | |
| -- thousands or millions) then it's that many function calls, and | |
| -- this will slow down the query execution significantly. In that | |
| -- case, you should replace the function call with its equivalent | |
| -- binary bitmask, e.g. if you run the query (with Quick button) | |
| -- SELECT (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT')) | |
| -- you will get the value 36507222016, which you can substitute in | |
| -- first line of the WHERE clause below as: | |
| -- (flags & 36507222016) > 0 | |
| -- to avoid zillions of function calls. | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr) | |
| </textarea><textarea style="display:none" id="q_1884815287">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. | |
| -- This query has many conditions, and also shows more of the | |
| -- bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_689792689">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_193732499">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| -- Another query that makes extensive use of photo flags to get a sample | |
| -- of galaxies within a size range as specified by their i-band Petrosian | |
| -- radius. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_883674423">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query but selects galaxies that | |
| -- are red (i-z color greater than a certain threshold). | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) | |
| </textarea><textarea style="display:none" id="q_498791126">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests that selects Luminous | |
| -- Red Galaxies (LRGs). | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) ) | |
| </textarea><textarea style="display:none" id="q_620022539">-- Spectra of Red Stars | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Galaxies with | |
| -- Emission Lines" sample query for an example of using galaxy spectra. | |
| -- | |
| -- Spectral lines for stars are calculated using the SEGUE Stellar Parameter | |
| -- Pipeline (SSPP; Lee et al. 2008) and are stored in the sppLines | |
| -- table. For more on how spectral lines of stars are found, see | |
| -- the SSPP page of the sdss3.org website. | |
| -- This query selects red stars (spectral type K), with large | |
| -- CaII triplet eq widths, with low errors on the CaII triplet | |
| -- equivalent widths. | |
| SELECT | |
| sl.plate,sl.mjd,sl.fiber, | |
| sl.caIIKside,sl.caIIKerr,sl.caIIKmask, | |
| sp.fehadop,sp.fehadopunc,sp.fehadopn, | |
| sp.loggadopn,sp.loggadopunc | |
| FROM sppLines AS sl | |
| JOIN sppParams AS sp ON sl.specobjid = sp.specobjid | |
| WHERE | |
| fehadop < -3.5 | |
| AND fehadopunc between 0.01 | |
| and 0.5 and fehadopn > 3 | |
| </textarea><textarea style="display:none" id="q_1606095120">-- Galaxy counts on HTM grid. | |
| -- | |
| -- Create a count of galaxies for each of the Hierarchical Triangular Mesh (HTM) triangles. | |
| -- Galaxies should satisfy a certain color cut like 0.7u-0.5g-0.2i<1.25 && r<21.75, output | |
| -- it in a form adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE | |
| -- RA/dec cut added to make query run in Quick mode | |
| (ra between 180 and 181 and dec between -1 and 1) and | |
| (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_2056596239">-- Binary Stars Colors. | |
| -- | |
| -- Find binary stars with specific colors. | |
| -- At least one of them should have the colors (meets Paul Szkody's color cut) of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1 -- S1 is the white dwarf | |
| JOIN Neighbors N ON S1.objID = N. objID -- N is the precomputed neighbors link | |
| JOIN Star S2 ON S2.objID = N.NeighborObjID -- S2 is the second star | |
| WHERE | |
| N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets the color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_1200129878">-- Galaxies unsaturated near (given) coordinates. | |
| -- | |
| -- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'ORDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy AS G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) AS GN -- this function outputs a table, so we have to do a join | |
| ON G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE | |
| (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_1036893522">-- Search near BCG galaxies. | |
| -- | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- This query has a very complex WHERE clause. | |
| SELECT TOP 1000 G.objID, COUNT(N.NeighborObjID) AS pop | |
| FROM Galaxy AS G -- first gravitational lens candidate | |
| JOIN Neighbors AS N ON G.objID = N.objID -- precomputed list of neighbors | |
| JOIN Galaxy AS U ON U.objID = N.neighborObjID -- a neighbor galaxy of G | |
| JOIN photoZ AS Gpz ON G.objID = Gpz.objID -- photoZ of G. | |
| JOIN photoZ AS Npz ON U.objID = Npz.objID -- neighbor photoZ | |
| WHERE | |
| G.ra BETWEEN 160 AND 170 | |
| AND G.dec BETWEEN -5 AND 5 | |
| AND N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| AND ABS(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| AND (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| AND (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| AND (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| AND G.petroMag_i > 17.5 | |
| AND (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| AND (G.petroMag_r < 30 AND G.g < 30 AND G.r < 30 AND G.i < 30) | |
| AND (G.r < 19.2 | |
| AND ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| AND (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 AND 0.2 ) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| AND (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| AND ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| GROUP BY G.objID | |
| </textarea><textarea style="display:none" id="q_1368842829">-- The detectionIndex table contains all detections of a given physical object, | |
| -- which is uniquely identified by the "thingid". In order to extract photometry, | |
| -- you need a join with the PhotoObjAll table, using the objid. | |
| -- There is also a flag field called isPrimary, which is 1 for the object that | |
| -- is found on a primary polygon/field, all the other detections have 0 in this field. | |
| -- Here is a compound query to find all time series around a certain object with a thingid= 97423000 | |
| SELECT | |
| LTRIM(STR(mjd_r,20,2)) AS MJD, | |
| dbo.fSDSS(p.objId) AS ID, | |
| modelMag_g, modelMagErr_g, | |
| modelMag_r, modelMagErr_r, | |
| modelMag_i, modelMagErr_i, p.ra, p.dec | |
| INTO #list | |
| FROM detectionindex d | |
| JOIN PhotoObjAll p ON d.objid=p.objid | |
| JOIN Field f ON p.fieldid=f.fieldid | |
| WHERE d.thingid=97423000 | |
| ORDER BY 1 | |
| GO | |
| -- | |
| -- Now find objects near each of the detections | |
| -- | |
| SELECT a.*, b.* | |
| FROM #list a | |
| CROSS APPLY dbo.fGetNearbyObjEq(a.ra, a.dec, 0.1) b | |
| </textarea> | |
| <textarea style="display:none" id="q_442485668">-- Find unique objects in an RA/Dec box. | |
| -- PhotoPrimary is a view which selects only unique objects. | |
| -- The full list of good detections including duplicates is in PhotoObj | |
| -- A basic SELECT-FROM-WHERE query. | |
| SELECT TOP 100 objID, -- Get the unique object ID, | |
| field, ra, dec -- the field number, and coordinates | |
| FROM PhotoPrimary -- From the photometric data | |
| WHERE | |
| ra > 185. and ra < 185.1 and dec > 15. and dec < 15.1 </textarea><textarea style="display:none" id="q_2039614472">-- Galaxies meeting two simple criteria. | |
| -- Find all galaxies brighter than r magnitude 22, where the local | |
| -- extinction is > 0.175. This is a simple query that uses a WHERE clause, | |
| -- but now two conditions that must be met simultaneously. | |
| SELECT TOP 10 objID | |
| FROM Galaxy | |
| WHERE | |
| r < 22 -- r IS NOT deredenned | |
| and extinction_r > 0.175 -- extinction more than 0.175 | |
| </textarea><textarea style="display:none" id="q_1763264299">-- Find specific types of quasars using spectroscopy. | |
| -- The easiest way to find quasars is by finding objects whose spectra have | |
| -- been classified as quasars. This sample query searches the SpecObj | |
| -- table for the IDs and redshifts of objects with the class column equal to 'QSO' | |
| SELECT TOP 100 specObjID, z | |
| FROM SpecObj | |
| WHERE class = 'QSO' AND zWarning = 0 | |
| </textarea><textarea style="display:none" id="q_2013120862">-- Using the BETWEEN syntax. | |
| -- Find all galaxies in a certain area of the sky that also meet other | |
| -- criteria in their measured parameters. This query intriduces the | |
| -- BETWEEN construct to specify a range of values. | |
| SELECT TOP 100 objID, ra, dec, cModelMag_g | |
| FROM Galaxy | |
| WHERE ra BETWEEN 178 AND 180 | |
| AND dec < 0 | |
| AND cModelMag_g BETWEEN 18 AND 19 | |
| </textarea><textarea style="display:none" id="q_930225692">-- Using spatial unit vectors for coordinate cuts. | |
| -- Find galaxies in a given area of the sky, using a coordinate cut | |
| -- in the unit vector cx,cy,cz that corresponds to a specific RA range. | |
| -- Another simple query that uses math in the WHERE clause. | |
| -- | |
| -- NOTE: This query must be run in batch mode, i.e. using the Submit button | |
| -- because it takes too long to execute in Quick mode. | |
| SELECT TOP 100 colc_g, colc_r | |
| FROM Galaxy | |
| WHERE | |
| (-0.466 * cx + 0.689 * cy>=0) | |
| and (-0.385 * cx - 0.173 * cy <0) | |
| </textarea><textarea style="display:none" id="q_129227591">-- Find CVs using colors. | |
| -- Search for Cataclysmic Variables and pre-CVs with White Dwarfs and | |
| -- very late secondaries. Just uses some simple color cuts from Paula Szkody. | |
| -- Another simple query that uses math in the WHERE clause | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec -- Just get some basic quantities | |
| FROM PhotoPrimary -- From all primary detections, regardless of class | |
| WHERE u - g < 0.4 | |
| and g - r < 0.7 | |
| and r - i > 0.4 | |
| and i - z > 0.4 -- that meet the color criteria | |
| </textarea><textarea style="display:none" id="q_1795754421">-- Getting a subsample of the data. | |
| -- | |
| -- Uses the integer short object id (obj) - which is the least significant bits | |
| -- of the long objID - and the '%' operator (remainder) to get every 1000th | |
| -- object. | |
| -- NOTE: THIS IS NOT A TRULY RANDOM SAMPLE! | |
| SELECT TOP 100 u, g, r, i, z | |
| FROM Galaxy with (nolock) | |
| WHERE (objID%1000) = 1 | |
| AND (r between 18 and 21) | |
| </textarea><textarea style="display:none" id="q_787192452">-- Low-z QSO candidates using color cuts. | |
| -- from Gordon Richards. | |
| -- Also a simple query with a long WHERE clause. | |
| SELECT TOP 1000 g, run, rerun, camcol, field, objID | |
| FROM | |
| Galaxy | |
| WHERE ( | |
| (g <= 22) and | |
| (u-g >= -0.27) and (u-g < 0.71) and | |
| (g-r >= -0.24) and (g-r < 0.35) and | |
| (r-i >= -0.27) and (r-i < 0.57) and | |
| (i-z >= -0.35) and (i-z < 0.70) | |
| )</textarea><textarea style="display:none" id="q_268548153">-- Get object velocities and errors. | |
| -- This is also a simple query that uses a WHERE clause. | |
| -- However, now we perform a more complex mathematical operation. | |
| SELECT TOP 10 | |
| run, -- get a bunch of quantities | |
| camCol, | |
| field, | |
| objID, | |
| rowC, colC, rowV, colV, rowVErr, colVErr, | |
| flags, | |
| psfMag_u, psfMag_g, psfMag_r, psfMag_i, psfMag_z, | |
| psfMagErr_u, psfMagErr_g, psfMagErr_r, psfMagErr_i, psfMagErr_z | |
| FROM PhotoPrimary | |
| WHERE ((rowv * rowv) / (rowvErr * rowvErr) + | |
| (colv * colv) / (colvErr * colvErr) > 4) | |
| -- where the velocities are reliable | |
| </textarea><textarea style="display:none" id="q_1047280483">-- Finding galaxies by their emission lines: | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Spectra of Red | |
| -- Stars" sample query for an example of using stellar spectra. | |
| -- | |
| -- Spectral lines for galaxies are calculated using the MPA-JHU | |
| -- spectroscopic reanalysis (Tremonti et al. 2004; Brinchmann et al. 2004) | |
| -- and are stored in the galSpecLine table. For more on how spectral lines | |
| -- of galaxies are found, see the Galspec page of the sdss3.org website. | |
| -- | |
| -- This query selects galaxy spectra with high internal reddening, | |
| -- as measured by the standard Balmer decrement technique. It | |
| -- makes use of the galSpec tables for the measurements of | |
| -- galaxy lines. In this case we use galSpecLine, which has | |
| -- emission line measurements. | |
| SELECT | |
| s.plate, s.fiberid, s.mjd, s.z, s.zwarning, | |
| g.h_beta_flux, g.h_beta_flux_err, | |
| g.h_alpha_flux, g.h_alpha_flux_err | |
| FROM GalSpecLine AS g | |
| JOIN dbo.SpecObj AS s ON s.specobjid = g.specobjid | |
| WHERE | |
| h_alpha_flux > h_alpha_flux_err*5 | |
| AND h_beta_flux > h_beta_flux_err*5 | |
| AND h_beta_flux_err > 0 | |
| AND h_alpha_flux > 10.*h_beta_flux | |
| AND s.class = 'GALAXY' | |
| AND s.zwarning = 0 | |
| </textarea><textarea style="display:none" id="q_191604836">-- Moving objects consistent with an asteroid. | |
| -- Also a simple query, but we introduce the 'as' syntax, which allows us to | |
| -- name derived quantities in the result file. | |
| -- | |
| -- NOTE: Since asteroids are rare objects in the SDSS data, this query will | |
| -- take a long time to run without the "TOP 10" and should be executed | |
| -- in batch mode (with the Submit button). | |
| SELECT TOP 10 | |
| objID, | |
| sqrt( power(rowv,2) + power(colv, 2) ) as velocity | |
| FROM PhotoObj | |
| WHERE | |
| (power(rowv,2) + power(colv, 2)) between 50 and 1000 | |
| </textarea><textarea style="display:none" id="q_1893814627">-- Find quasars in imaging data. | |
| -- as specified by Xiaohui Fan et.al. | |
| -- A rather straightforward query, just with many conditions. | |
| SELECT TOP 100 run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| u, g, r, i, z, | |
| ra, dec | |
| FROM Star -- or Galaxy | |
| WHERE ( u - g > 2.0 or u > 22.3 ) | |
| and ( i < 19 ) | |
| and ( i > 0 ) | |
| and ( g - r > 1.0 ) | |
| and ( r - i < | |
| (0.08 + 0.42 * (g - r - 0.96) ) | |
| or g - r > 2.26 ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1199374736">-- Using object counting and logic in a query. | |
| -- Find all objects similar to the colors of a quasar at 5.5<redshift<6.5. | |
| -- An area restriction is added so the query will run in the Quick queue. | |
| SELECT count(*) as 'total', | |
| sum( case when (Type=3) then 1 else 0 end) as 'Galaxies', | |
| sum( case when (Type=6) then 1 else 0 end) as 'Stars', | |
| sum( case when (Type not in (3,6)) then 1 else 0 end) as 'Other' | |
| FROM PhotoPrimary -- for each object | |
| WHERE | |
| (ra between 180 and 190) and (dec between -5 and 5) | |
| and (( u - g > 2.0) or (u > 22.3) ) -- apply the quasar color cut. | |
| and ( i between 0 and 19 ) | |
| and ( g - r > 1.0 ) | |
| and ( (r - i < 0.08 + 0.42 * (g - r - 0.96)) or (g - r > 2.26 ) ) | |
| and ( i - z < 0.25 ) | |
| </textarea><textarea style="display:none" id="q_1733737046">-- Find galaxies that are blended with a star. | |
| -- Output the deblended galaxy magnitudes. | |
| -- This query introduces the use of multiple tables or views. You can assign | |
| -- nicknames to tables as in the FROM clause below. Since you are using | |
| -- multiple tables, you must specify which table each quantity in the SELECT | |
| -- clause comes from. The query illustrates the JOIN syntax between | |
| -- the two tables, which requires that a common quantity that is present in | |
| -- both tables be equal, in this case their common parent object. | |
| SELECT top 1000 G.ObjID, G.u, G.g, G.r, G.i, G.z | |
| FROM Galaxy G -- compare Galaxy and Star | |
| JOIN Star S ON G.parentID = S.parentID -- using the same parent | |
| WHERE | |
| G.parentID > 0 -- if the galaxy has a "parent", this object was deblended | |
| </textarea><textarea style="display:none" id="q_317286293">-- Stars selected using Field criteria. | |
| -- Give me the PSF colors of all stars brighter than g=20 that have PSP_STATUS = 2. | |
| -- Another simple multi-table query. | |
| SELECT TOP 1000 | |
| s.psfMag_g, -- or whatever you want from each object | |
| s.run, | |
| s.camCol, | |
| s.rerun, | |
| s.field | |
| FROM Star s | |
| JOIN Field f ON s.fieldID = f.fieldID | |
| WHERE | |
| s.psfMag_g < 20 | |
| and f.pspStatus = 2 | |
| </textarea><textarea style="display:none" id="q_1874540969">-- Objects selected by cuts on three tables. | |
| -- Find the parameters for all objects in a selected field with | |
| -- desired PSF width and range of columns. | |
| -- Now we are using three tables, but it is still a simple query. | |
| SELECT TOP 1000 | |
| f.run, | |
| f.rerun, | |
| f.camCol, | |
| f.field, | |
| p.objID, | |
| p.ra, | |
| p.dec, | |
| p.Rowc, | |
| p.Colc, | |
| p.u, | |
| p.modelMagErr_u , | |
| p.g, | |
| p.modelMagErr_g, | |
| p.r, | |
| p.modelMagErr_r, | |
| p.petroMag_r - p.extinction_r, | |
| p.petroMagErr_r, | |
| p.i, | |
| p.modelMagErr_i, | |
| p.z, | |
| f.psfWidth_r, | |
| r.stripe, | |
| r.strip | |
| FROM | |
| photoObj p | |
| JOIN field f ON f.fieldid = p.fieldid | |
| JOIN run r ON r.run=f.run | |
| WHERE | |
| f.psfWidth_r > 1.2 | |
| and p.colc > 400.0 | |
| </textarea><textarea style="display:none" id="q_1435232814">-- Find all objects within 30 arcseconds of one another | |
| -- that have very similar colors: that is where the color ratios | |
| -- u-g, g-r, r-I are less than 0.05m. This query introduces the | |
| -- Neighbors table, which is a pre-computed list of the nearest | |
| -- neighbors of each object within 30 arcseconds. | |
| SELECT TOP 10 P.ObjID as objid1, L.ObjID as objid2, N.distance | |
| FROM PhotoPrimary P -- P is the primary object | |
| JOIN Neighbors N ON P.ObjID = N.ObjID -- N is the neighbor link | |
| JOIN PhotoPrimary L ON L.ObjID = N.NeighborObjID -- L is the lens candidate of P | |
| WHERE | |
| P.ObjID < L. ObjID -- avoid duplicates | |
| and abs((P.u-P.g)-(L.u-L.g))<0.05 -- L and P have similar spectra | |
| and abs((P.g-P.r)-(L.g-L.r))<0.05 | |
| and abs((P.r-P.i)-(L.r-L.i))<0.05 | |
| and abs((P.i-P.z)-(L.i-L.z))<0.05 | |
| </textarea><textarea style="display:none" id="q_2060639971">-- Find stars with multiple measurements with magnitude variations >0.1. | |
| -- Note that this runs very slowly unless explicit workarounds are included | |
| -- for some SQLServer Optimizer bugs, which are NOT included here | |
| SELECT TOP 100 | |
| S1.objID as objID1, S2.objID as ObjID2 -- select object IDs of star and its pair | |
| FROM Star as S1, -- the primary star | |
| photoObj as S2, -- the second observation of the star | |
| neighbors as N -- the neighbor record | |
| WHERE S1.objID = N.objID -- insist the stars are neighbors | |
| and S2.objID = N.neighborObjID -- using precomputed neighbors table | |
| and distance < 0.5/60 -- distance is 0.5 arc second or less | |
| and S1.run != S2.run -- observations are two different runs | |
| and S2.type = dbo.fPhotoType('Star') -- S2 is indeed a star | |
| and S1.u between 1 and 27 -- S1 magnitudes are reasonable | |
| and S1.g between 1 and 27 | |
| and S1.r between 1 and 27 | |
| and S1.i between 1 and 27 | |
| and S1.z between 1 and 27 | |
| and S2.u between 1 and 27 -- S2 magnitudes are reasonable. | |
| and S2.g between 1 and 27 | |
| and S2.r between 1 and 27 | |
| and S2.i between 1 and 27 | |
| and S2.z between 1 and 27 | |
| and ( -- and one of the colors is different. | |
| abs(S1.u-S2.u) > .1 + (abs(S1.Err_u) + abs(S2.Err_u)) | |
| or abs(S1.g-S2.g) > .1 + (abs(S1.Err_g) + abs(S2.Err_g)) | |
| or abs(S1.r-S2.r) > .1 + (abs(S1.Err_r) + abs(S2.Err_r)) | |
| or abs(S1.i-S2.i) > .1 + (abs(S1.Err_i) + abs(S2.Err_i)) | |
| or abs(S1.z-S2.z) > .1 + (abs(S1.Err_z) + abs(S2.Err_z)) | |
| ) | |
| </textarea><textarea style="display:none" id="q_1200416665">-- Checking for errors using flags. | |
| -- Another useful query is to see if the errors on moving (or | |
| -- apparently moving) objects are correct. For example, it used to be that | |
| -- some known QSOs were being flagged as moving objects. One way to look for | |
| -- such objects is to compare the velocity to the error in velocity and see if | |
| -- the "OBJECT1_MOVED" or "OBJECT2_BAD_MOVING_FIT" is set. | |
| -- This query introduces bitwise logic for flags, and uses the 'as' syntax to | |
| -- make the query more readable. Note that if a flag is not set, the value | |
| -- will be zero. If you want to ensure multiple flags are not set, you can | |
| -- either check that each individually is zero, or that their sum is zero. | |
| -- (From Gordon Richards) | |
| -- | |
| -- NOTE: A caveat about using functons (like fPhotoFlags) is that if your | |
| -- query is selecting a very large number of rows (e.g. hundreds of | |
| -- thousands or millions) then it's that many function calls, and | |
| -- this will slow down the query execution significantly. In that | |
| -- case, you should replace the function call with its equivalent | |
| -- binary bitmask, e.g. if you run the query (with Quick button) | |
| -- SELECT (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT')) | |
| -- you will get the value 36507222016, which you can substitute in | |
| -- first line of the WHERE clause below as: | |
| -- (flags & 36507222016) > 0 | |
| -- to avoid zillions of function calls. | |
| SELECT TOP 1000 | |
| run, | |
| rerun, | |
| camcol, | |
| field, | |
| objID, | |
| ra, dec, | |
| rowv, colv, | |
| rowvErr, colvErr, | |
| i, | |
| (flags & dbo.fPhotoFlags('MOVED')) as MOVED, | |
| (flags & dbo.fPhotoFlags('BAD_MOVING_FIT')) as BAD_MOVING_FIT | |
| FROM Galaxy | |
| WHERE | |
| (flags & (dbo.fPhotoFlags('MOVED') + dbo.fPhotoFlags('BAD_MOVING_FIT'))) > 0 | |
| and (rowv * rowv + colv * colv) >= | |
| (rowvErr * rowvErr + colvErr * colvErr) | |
| </textarea><textarea style="display:none" id="q_1563979474">-- Elliptical galaxies based on model fits. | |
| -- Find all galaxies with a deVaucouleours profile and the | |
| -- photometric colors consistent with an elliptical galaxy. | |
| -- This query has many conditions, and also shows more of the | |
| -- bitwise logic necessary for dealing with flags. | |
| SELECT TOP 100 ObjID | |
| FROM Galaxy as G | |
| WHERE | |
| G.lnlDev_r > G.lnlExp_r + 0.1 | |
| -- the likelihood of the deVaucouleours profile fit is 10% greater than the likelihood of the exponential fit | |
| and G.lnlExp_r > -999 | |
| -- and the likelihoods are actually meaningful | |
| and (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images ??? | |
| and (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| and (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| and G.petroMag_i > 17.5 | |
| -- and it is fainter than 17.5 in i-band | |
| and (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| and (G.petroMag_r > 0 and G.g > 0 and G.r > 0 and G.i > 0) | |
| and ( (G.petroMag_r - G.extinction_r) < 19.2 | |
| and (G.petroMag_r - G.extinction_r < | |
| (13.1 + (7/3)*(G.g - G.r) + 4 *(G.r - G.i) - 4 * 0.18 ) ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) < 0.2 ) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > -0.2 ) ) | |
| or ( (G.petroMag_r - G.extinction_r < 19.5) | |
| and ( (G.r - G.i - (G.g - G.r)/4 - 0.18) > | |
| (0.45 - 4*(G.g - G.r) ) ) | |
| and ( (G.g - G.r) > (1.35 + 0.25 *(G.r - G.i) ) ) ) | |
| -- and many constraints on colors and mags are met to make it have | |
| -- elliptical-type colors. | |
| </textarea><textarea style="display:none" id="q_673740146">-- Galaxies with bluer centers. | |
| -- by Michael Strauss. For all galaxies | |
| -- with r_Petro < 18, not saturated, not bright, and not edge, give me those | |
| -- with centers appreciably bluer than their outer parts, i.e., define the | |
| -- center color as: u_psf - g_psf and define the outer color as: u_model - | |
| -- g_model; give me all objs which have (u_model - g_model) - (u_psf - g_psf) | |
| -- < -0.4 | |
| -- Another flags-based query. | |
| SELECT TOP 1000 | |
| colc_u, colc_g, objID | |
| FROM Galaxy | |
| WHERE | |
| ( Flags & (dbo.fPhotoFlags('SATURATED') + | |
| dbo.fPhotoFlags('BRIGHT') + | |
| dbo.fPhotoFlags('EDGE')) ) = 0 | |
| and petrorad_r < 18 | |
| and ((colc_u - colc_g) - (psfMag_u - psfMag_g)) < -0.4</textarea><textarea style="display:none" id="q_1080565066">-- Diameter-limited sample of galaxies | |
| -- from James Annis. | |
| -- Another query that makes extensive use of photo flags to get a sample | |
| -- of galaxies within a size range as specified by their i-band Petrosian | |
| -- radius. | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( ( (flags & dbo.fPhotoFlags('NOPETRO') = 0) | |
| and petrorad_i > 15) | |
| or ( (flags & dbo.fPhotoFlags('NOPETRO') > 0) | |
| and petrorad_i > 7.5) | |
| or ( (flags & dbo.fPhotoFlags('TOO_LARGE') > 0) | |
| and petrorad_i > 2.5) | |
| or | |
| ( (flags & dbo.fPhotoFlags('SATURATED') = 0) | |
| and petrorad_i > 17.5) ) | |
| </textarea><textarea style="display:none" id="q_1549277712">-- Extremely red galaxies. | |
| -- from James Annis. | |
| -- Similar to the diameter limited sample query but selects galaxies that | |
| -- are red (i-z color greater than a certain threshold). | |
| SELECT TOP 1000 | |
| g.run, | |
| g.camCol, | |
| g.rerun, | |
| g.field, | |
| g.objID, | |
| g.ra, g.dec | |
| FROM Field f, Galaxy g | |
| WHERE | |
| g.fieldID = f.fieldID | |
| and ( g.flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( g.flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( g.flags & (dbo.fPhotoFlags('COSMIC_RAY') | |
| + dbo.fPhotoFlags('INTERP')) ) = 0 | |
| and f.psfWidth_r < 1.5 | |
| and (g.i - g.z > 1.0 ) | |
| </textarea><textarea style="display:none" id="q_1688445031">-- A version of the LRG sample. | |
| -- by James Annis. | |
| -- Another query with many conditions and flag tests that selects Luminous | |
| -- Red Galaxies (LRGs). | |
| SELECT TOP 100 | |
| run, | |
| camCol, | |
| rerun, | |
| field, | |
| objID, | |
| ra, | |
| dec | |
| FROM Galaxy | |
| WHERE ( ( flags & (dbo.fPhotoFlags('BINNED1') | |
| + dbo.fPhotoFlags('BINNED2') | |
| + dbo.fPhotoFlags('BINNED4')) ) > 0 | |
| and ( flags & (dbo.fPhotoFlags('BLENDED') | |
| + dbo.fPhotoFlags('NODEBLEND') | |
| + dbo.fPhotoFlags('CHILD')) ) != dbo.fPhotoFlags('BLENDED') | |
| and ( flags & (dbo.fPhotoFlags('EDGE') | |
| + dbo.fPhotoFlags('SATURATED')) ) = 0 | |
| and petroMag_i > 17.5 | |
| and (petroMag_r > 15.5 or petror50_r > 2) | |
| and (petroMag_r > 0 and g > 0 and r > 0 and i > 0) | |
| and ( (petroMag_r-extinction_r) < 19.2 | |
| and (petroMag_r - extinction_r < | |
| (13.1 + (7/3) * (dered_g - dered_r) + 4 * (dered_r - dered_i) - 4 * 0.18) ) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) < 0.2) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > -0.2) | |
| --dered_ quantities already include extinction | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r)) < 24.2) ) | |
| or ( (petroMag_r - extinction_r < 19.5) | |
| and ( (dered_r - dered_i - (dered_g - dered_r)/4 - 0.18) > (0.45 - 4 * (dered_g - dered_r)) ) | |
| and ( (dered_g - dered_r) > (1.35 + 0.25 * (dered_r - dered_i)) ) ) | |
| and ( (petroMag_r - extinction_r + | |
| 2.5 * LOG10(2 * 3.1415 * petror50_r * petror50_r) ) < 23.3 ) ) | |
| </textarea><textarea style="display:none" id="q_1276987864">-- Spectra of Red Stars | |
| -- | |
| -- SDSS-III handles searches by spectral lines differently than previous | |
| -- releases. In addition, spectral lines for galaxies and stars are | |
| -- identified through different processes. See the "Galaxies with | |
| -- Emission Lines" sample query for an example of using galaxy spectra. | |
| -- | |
| -- Spectral lines for stars are calculated using the SEGUE Stellar Parameter | |
| -- Pipeline (SSPP; Lee et al. 2008) and are stored in the sppLines | |
| -- table. For more on how spectral lines of stars are found, see | |
| -- the SSPP page of the sdss3.org website. | |
| -- This query selects red stars (spectral type K), with large | |
| -- CaII triplet eq widths, with low errors on the CaII triplet | |
| -- equivalent widths. | |
| SELECT | |
| sl.plate,sl.mjd,sl.fiber, | |
| sl.caIIKside,sl.caIIKerr,sl.caIIKmask, | |
| sp.fehadop,sp.fehadopunc,sp.fehadopn, | |
| sp.loggadopn,sp.loggadopunc | |
| FROM sppLines AS sl | |
| JOIN sppParams AS sp ON sl.specobjid = sp.specobjid | |
| WHERE | |
| fehadop < -3.5 | |
| AND fehadopunc between 0.01 | |
| and 0.5 and fehadopn > 3 | |
| </textarea><textarea style="display:none" id="q_1804992033">-- Galaxy counts on HTM grid. | |
| -- | |
| -- Create a count of galaxies for each of the Hierarchical Triangular Mesh (HTM) triangles. | |
| -- Galaxies should satisfy a certain color cut like 0.7u-0.5g-0.2i<1.25 && r<21.75, output | |
| -- it in a form adequate for visualization. | |
| SELECT (htmID / power(2,24)) as htm_8 , | |
| -- group by 8-deep HTMID (rshift HTM by 12) | |
| avg(ra) as ra, | |
| avg(dec) as [dec], | |
| count(*) as pop -- return center point and count for display | |
| FROM Galaxy -- only look at galaxies | |
| WHERE | |
| -- RA/dec cut added to make query run in Quick mode | |
| (ra between 180 and 181 and dec between -1 and 1) and | |
| (0.7*u - 0.5*g - 0.2*i) < 1.25 -- meeting this color cut | |
| and r < 21.75 -- brighter than 21.75 magnitude in red band. | |
| group by (htmID /power(2,24)) -- group into 8-deep HTM buckets. | |
| </textarea><textarea style="display:none" id="q_1055302504">-- Binary Stars Colors. | |
| -- | |
| -- Find binary stars with specific colors. | |
| -- At least one of them should have the colors (meets Paul Szkody's color cut) of a white dwarf. | |
| SELECT TOP 100 s1.objID as s1, s2.objID as s2 | |
| FROM Star S1 -- S1 is the white dwarf | |
| JOIN Neighbors N ON S1.objID = N. objID -- N is the precomputed neighbors link | |
| JOIN Star S2 ON S2.objID = N.NeighborObjID -- S2 is the second star | |
| WHERE | |
| N.neighborType = dbo.fPhotoType('Star') -- and S2 is a star | |
| and N.distance < .05 -- the 3 arcsecond test | |
| and ((S1.u - S1.g) < 0.4 ) -- and S1 meets the color cut for | |
| and (S1.g - S1.r) < 0.7 -- white dwarfs. | |
| and (S1.r - S1.i) > 0.4 | |
| and (S1.i - S1.z) > 0.4 | |
| </textarea><textarea style="display:none" id="q_183659941">-- Galaxies unsaturated near (given) coordinates. | |
| -- | |
| -- Find galaxies without saturated pixels within 1' of a given point. | |
| -- ra=185.0, dec=-0.5. This query uses a function fGetNearbyObjEq, | |
| -- which takes 3 arguments (ra,dec, distance in arcmin); this function uses | |
| -- the Neighbors table. The Neighbors table and the Galaxy table have in | |
| -- common the objID, so we have to select objects from both where the objIDs | |
| -- are the same. The output of the function is a table with the Galaxy Object | |
| -- ID and distance in arcmin from the input. This query introduces the use of | |
| -- a JOIN to combine table contents. Also, we use the 'ORDER BY' syntax, | |
| -- which will sort the output. | |
| SELECT TOP 100 G.objID, GN.distance | |
| FROM Galaxy AS G | |
| JOIN dbo.fGetNearbyObjEq(185.,-0.5, 1) AS GN -- this function outputs a table, so we have to do a join | |
| ON G.objID = GN.objID -- get objects from temporary neighbors table GN with desired ObjID | |
| WHERE | |
| (G.flags & dbo.fPhotoFlags('saturated')) = 0 -- and the object is not saturated. f.PhotoFlags is a function that interprets the flag bits. | |
| ORDER BY distance -- sort these by distance | |
| </textarea><textarea style="display:none" id="q_2000917639">-- Search near BCG galaxies. | |
| -- | |
| -- For each galaxy in the BCG data set (brightest cluster galaxy), | |
| -- in 160<right ascension<170, -25<declination<35 count the number of | |
| -- galaxies within 30" of it that have a photoz within 0.05 | |
| -- of that galaxy. | |
| -- This query has a very complex WHERE clause. | |
| SELECT TOP 1000 G.objID, COUNT(N.NeighborObjID) AS pop | |
| FROM Galaxy AS G -- first gravitational lens candidate | |
| JOIN Neighbors AS N ON G.objID = N.objID -- precomputed list of neighbors | |
| JOIN Galaxy AS U ON U.objID = N.neighborObjID -- a neighbor galaxy of G | |
| JOIN photoZ AS Gpz ON G.objID = Gpz.objID -- photoZ of G. | |
| JOIN photoZ AS Npz ON U.objID = Npz.objID -- neighbor photoZ | |
| WHERE | |
| G.ra BETWEEN 160 AND 170 | |
| AND G.dec BETWEEN -5 AND 5 | |
| AND N.objID < N.neighborObjID -- 30 arcseconds of one another. | |
| AND ABS(Gpz.Z - Npz.Z) < 0.05 -- restrict the photoZ differences | |
| AND (G.flags & (dbo.fPhotoFlags('BINNED1') + dbo.fPhotoFlags('BINNED2') + dbo.fPhotoFlags('BINNED4'))) > 0 | |
| --and it is detected from at least one of the binned images | |
| AND (G.flags & ( dbo.fPhotoFlags('BLENDED') + dbo.fPhotoFlags('NODEBLEND') + dbo.fPhotoFlags('CHILD'))) != dbo.fPhotoFlags('BLENDED') | |
| --and, if it is blended, it is either a child or not deblended further ?? | |
| AND (G.flags & (dbo.fPhotoFlags('EDGE') + dbo.fPhotoFlags('SATURATED'))) = 0 | |
| -- and it is not near a ccd edge or saturated, where measurements may be bad | |
| -- and apply color cut for a BCG courtesy of James Annis of Fermilab | |
| AND G.petroMag_i > 17.5 | |
| AND (G.petroMag_r > 15.5 or G.petror50_r > 2) | |
| AND (G.petroMag_r < 30 AND G.g < 30 AND G.r < 30 AND G.i < 30) | |
| AND (G.r < 19.2 | |
| AND ( 1=1 or -- huh? | |
| (G.r < (13.1 + (7/3)*(G.g - G.r) + | |
| -- deRed_r < 13.1 + 0.7 / 0.3 * deRed_gr | |
| 4 *(G.r - G.i - 0.18 )) | |
| -- 1.2 / 0.3 * deRed_ri | |
| AND (( G.r - G.i - (G.g - G.r)/4 - 0.18) BETWEEN -0.2 AND 0.2 ) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 24.2 ) | |
| ) | |
| or | |
| ( (G.r < 19.5 ) | |
| AND (( G.r - G.i -(G.g - G.r)/4 -.18) > | |
| -- - deRed_gr/4 - 0.18 | |
| -- cperp = deRed_ri | |
| (0.45 - 4*( G.g - G.r))) | |
| -- 0.45 - deRed_gr/0.25 | |
| AND ((G.g - G.r) > ( 1.35 + 0.25 *(G.r - G.i))) | |
| AND ((G.r + | |
| -- petSB - deRed_r + 2.5 log10(2Pi*petror50^2) | |
| 2.5 * LOG( 2 * 3.1415 * G.petror50_r * G.petror50_r )) < 23.3 ) | |
| )) ) | |
| GROUP BY G.objID | |
| </textarea><textarea style="display:none" id="q_359595534">-- The detectionIndex table contains all detections of a given physical object, | |
| -- which is uniquely identified by the "thingid". In order to extract photometry, | |
| -- you need a join with the PhotoObjAll table, using the objid. | |
| -- There is also a flag field called isPrimary, which is 1 for the object that | |
| -- is found on a primary polygon/field, all the other detections have 0 in this field. | |
| -- Here is a compound query to find all time series around a certain object with a thingid= 97423000 | |
| SELECT | |
| LTRIM(STR(mjd_r,20,2)) AS MJD, | |
| dbo.fSDSS(p.objId) AS ID, | |
| modelMag_g, modelMagErr_g, | |
| modelMag_r, modelMagErr_r, | |
| modelMag_i, modelMagErr_i, p.ra, p.dec | |
| INTO #list | |
| FROM detectionindex d | |
| JOIN PhotoObjAll p ON d.objid=p.objid | |
| JOIN Field f ON p.fieldid=f.fieldid | |
| WHERE d.thingid=97423000 | |
| ORDER BY 1 | |
| GO | |
| -- | |
| -- Now find objects near each of the detections | |
| -- | |
| SELECT a.*, b.* | |
| FROM #list a | |
| CROSS APPLY dbo.fGetNearbyObjEq(a.ra, a.dec, 0.1) b | |
| </textarea> | |
| <textarea style="display:none" id="q_752833322">-- This query gets the SQL queries per month for a given database name (pattern). | |
| select yy, mm as mth, count(*) | |
| into mydb.MonthyUsageDR8 | |
| from sqllogall | |
| where dbname like '%dr8' | |
| group by yy, mm | |
| order by yy, mm</textarea><textarea style="display:none" id="q_652519058">-- This query gets the rough GB served per month from SQL queries on a given database name (pattern). | |
| -- The query assumes a fiducial average row size of 100 bytes and hence divides the total number of | |
| -- rows per month by 10^7 (i.e. 10^9/100) to get the approximate # of GBs returned to the user. | |
| select yy, mm as mth, cast(sum(rows) as float)/10000000 as GB | |
| into mydb.MonthyGBforDR8 | |
| from sqllogall | |
| where yy >=2011 and dbname like '%dr8' | |
| group by yy, mm | |
| order by yy, mm | |
| </textarea><textarea style="display:none" id="q_518325890">-- This query gets the SQL queries per quarter for a given year (2012) for a given SQL product (DR8) in the LogSource table. | |
| select datepart(qq,s.thetime) as Qtr, count(*) as Queries | |
| into mydb.QtrlyUsageDR8 | |
| from sqllogall s join logsource l on s.logid=l.logid | |
| where s.yy = 2012 and l.product='DR8' | |
| group by datepart(qq,s.thetime) | |
| order by Qtr | |
| -- To get the same data for multiple years, you can do something like: | |
| select (cast(yy as varchar(4)) + '-Q' + cast(datepart(qq,s.thetime) as varchar(1))) as Qtr, | |
| count(*) as Queries | |
| into mydb.QtrlyUsageDR8 | |
| from sqllogall s join logsource l on s.logid=l.logid | |
| where s.yy > 2010 and l.product='DR8' | |
| group by yy, datepart(qq,s.thetime) | |
| order by Qtr | |
| </textarea><textarea style="display:none" id="q_1785185606">-- This query gets the Web hits for a given quarter (2012-Q1) for a given Web product (DR8) in the LogSource table. | |
| select count(*) as Hits | |
| into mydb.Q1HitsDR8 | |
| from Weblogall s join logsource l on s.logid=l.logid | |
| where s.yy = 2012 and (s.mm between 1 and 3) and l.product='DR8' | |
| </textarea> | |
| </div> | |
| <!--<div style="width:auto; border:none;" class="qpop" id="samplePreviewPane"></div>--> | |
| <div style="width: auto; padding: 0 0 0 0;" class="qpop" id="samplePreviewPane"> | |
| </div> | |
| <div id="tableHelpDiv" class="qpopH"> | |
| Submitted queries are required to direct their output into a table in MyDB. You | |
| can do this either by manually specifying 'select into' clause within your query, | |
| or by letting CasJobs automatically add the table in this field. Default table names | |
| in this field are usually unique.; | |
| </div> | |
| <div id="contextHelpDiv" class="qpopH"> | |
| A <i>context</i> is a unique catalog of data. Use this field to determine where your queries should run. | |
| </div> | |
| <div id="taskNameHelpDiv" class="qpopH"> | |
| You can search your job history by taskname, so using a unique value in this field | |
| can help when searching for a particular job. | |
| </div> | |
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