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27&lt;region&gt;/tractor/&lt;AAA&gt;/tractor-&lt;brick&gt;.fits
28Goodness-of-Fits and Morphological type
29Galactic Extinction Coefficients
30Ellipticities
31
32
33
34&lt;region&gt;/tractor/&lt;AAA&gt;/tractor-&lt;brick&gt;.fits
35FITS binary ">
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230<article class="storypage" itemscope="itemscope" itemtype="http://schema.org/Article"><header><h1 class="p-name entry-title" itemprop="headline name">Tractor Catalog Format</h1>
231        
232
233    </header><div class="e-content entry-content" itemprop="articleBody text">
234    <nav class="contents pull-right well" id="contents" role="doc-toc"><p class="topic-title"><a class="reference internal" href="#top">Contents</a></p>
235<ul class="simple">
236<li><p><a class="reference internal" href="#region-tractor-aaa-tractor-brick-fits" id="toc-entry-1">&lt;region&gt;/tractor/&lt;AAA&gt;/tractor-&lt;brick&gt;.fits</a></p></li>
237<li><p><a class="reference internal" href="#goodness-of-fits-and-morphological-type" id="toc-entry-2">Goodness-of-Fits and Morphological <code class="docutils literal">type</code></a></p></li>
238<li><p><a class="reference internal" href="#galactic-extinction-coefficients" id="toc-entry-3">Galactic Extinction Coefficients</a></p></li>
239<li><p><a class="reference internal" href="#ellipticities" id="toc-entry-4">Ellipticities</a></p></li>
240</ul></nav><section id="region-tractor-aaa-tractor-brick-fits"><h2><a class="toc-backref" href="#toc-entry-1" role="doc-backlink">&lt;region&gt;/tractor/&lt;AAA&gt;/tractor-&lt;brick&gt;.fits</a></h2>
241<p>FITS binary table containing Tractor photometry. Before using these catalogs, note that there may be
242<a class="reference external" href="../issues">known issues</a> regarding their content and derivation. All flux-based quantities in the
243catalogs are on the AB system (we specify that WISE fluxes are AB in the table for clarity, as
244such quantities are often quoted on the Vega system). Note that <span class="math">\(i\)</span>-band quantities are only present for
245<code class="docutils literal"><span class="pre">&lt;region&gt;=south</span></code>.</p>
246<table class="table table-bordered table-condensed">
247<thead><tr>
248<th class="head"><p>Name</p></th>
249<th class="head"><p>Type</p></th>
250<th class="head"><p>Units</p></th>
251<th class="head"><p>Description</p></th>
252</tr></thead>
253<tbody>
254<tr>
255<td><p><code class="docutils literal">ls_id_dr11</code></p></td>
256<td><p>int64</p></td>
257<td></td>
258<td><p>Unique ID describing each Legacy Survey source</p></td>
259</tr>
260<tr>
261<td><p><code class="docutils literal">release</code></p></td>
262<td><p>int16</p></td>
263<td></td>
264<td><p>Integer denoting the camera and filter set used, which will be unique for a given processing run of the data (<a class="reference external" href="../../release">as documented here</a>)</p></td>
265</tr>
266<tr>
267<td><p><code class="docutils literal">brickid</code></p></td>
268<td><p>int32</p></td>
269<td></td>
270<td><p>Brick ID [1,662174]</p></td>
271</tr>
272<tr>
273<td><p><code class="docutils literal">brickname</code></p></td>
274<td><p>char[8]</p></td>
275<td></td>
276<td><p>Name of brick, encoding the brick sky position, eg "1126p222" near RA
276=112.6, Dec=+22.2</p></td>
277</tr>
278<tr>
279<td><p><code class="docutils literal">objid</code></p></td>
280<td><p>int32</p></td>
281<td></td>
282<td><p>Catalog object number within this brick; a unique identifier hash is <code class="docutils literal">release,brickid,objid</code>;  <code class="docutils literal">objid</code> spans [0,N-1] and is contiguously enumerated within each brick</p></td>
283</tr>
284<tr>
285<td><p><code class="docutils literal">brick_primary</code></p></td>
286<td><p>boolean</p></td>
287<td></td>
288<td><p><code class="docutils literal">True</code> if the object is within the brick boundary</p></td>
289</tr>
290<tr>
291<td><p><code class="docutils literal">maskbits</code></p></td>
292<td><p>int32</p></td>
293<td></td>
294<td><p>Bitwise mask indicating that an object touches a pixel in the <code class="docutils literal"><span class="pre">coadd/*/*/*maskbits*</span></code> maps, as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
295</tr>
296<tr>
297<td><p><code class="docutils literal">fitbits</code></p></td>
298<td><p>int16</p></td>
299<td></td>
300<td><p>Bitwise mask detailing pecularities of how an object was fit, as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
301</tr>
302<tr>
303<td><p><code class="docutils literal">type</code></p></td>
304<td><p>char[3]</p></td>
305<td></td>
306<td><p>Morphological model: "PSF"=stellar, "REX"="round exponential galaxy", "DEV"=deVauc, "EXP"=exponential, "SER"=Sersic, "DUP"=Gaia source fit by different model. See also <a class="reference external" href="../description/#morphological-classification">the larger description</a>.</p></td>
307</tr>
308<tr>
309<td><p><code class="docutils literal">ra</code></p></td>
310<td><p>float64</p></td>
311<td><p>deg</p></td>
312<td><p>Right ascension at equinox J2000</p></td>
313</tr>
314<tr>
315<td><p><code class="docutils literal">dec</code></p></td>
316<td><p>float64</p></td>
317<td><p>deg</p></td>
318<td><p>Declination at equinox J2000</p></td>
319</tr>
320<tr>
321<td><p><code class="docutils literal">ra_ivar</code></p></td>
322<td><p>float32</p></td>
323<td><p>1/deg²</p></td>
324<td><p>Inverse variance of RA (no cosine term!), excluding astrometric calibration errors</p></td>
325</tr>
326<tr>
327<td><p><code class="docutils literal">dec_ivar</code></p></td>
328<td><p>float32</p></td>
329<td><p>1/deg²</p></td>
330<td><p>Inverse variance of DEC, excluding astrometric calibration errors</p></td>
331</tr>
332<tr>
333<td><p><code class="docutils literal">bx</code></p></td>
334<td><p>float32</p></td>
335<td><p>pix</p></td>
336<td><p>X position (0-indexed) of coordinates in the brick image stack (<em>i.e.</em> in the <em>e.g.</em> <cite>legacysurvey-&lt;brick&gt;-image-g.fits.fz</cite> <a class="reference external" href="../files/#image-stacks-south-coadd">coadd file</a>)</p></td>
337</tr>
338<tr>
339<td><p><code class="docutils literal">by</code></p></td>
340<td><p>float32</p></td>
341<td><p>pix</p></td>
342<td><p>Y position (0-indexed) of coordinates in brick image stack</p></td>
343</tr>
344<tr>
345<td><p><code class="docutils literal">dchisq</code></p></td>
346<td><p>float32[5]</p></td>
347<td></td>
348<td><p>Difference in χ² between successively more-complex model fits: PSF, REX, DEV, EXP, SER.  The difference is versus no source.</p></td>
349</tr>
350<tr>
351<td><p><code class="docutils literal">ebv</code></p></td>
352<td><p>float32</p></td>
353<td><p>mag</p></td>
354<td><p>Galactic extinction E(B-V) reddening from <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/1998ApJ...500..525S/abstract">SFD98</a>, used to compute the <code class="docutils literal">mw_transmission_</code> columns</p></td>
355</tr>
356<tr>
357<td><p><code class="docutils literal">mjd_min</code></p></td>
358<td><p>float64</p></td>
359<td><p>days</p></td>
360<td><p>Minimum Modified Julian Date of observations used to construct the model of this object</p></td>
361</tr>
362<tr>
363<td><p><code class="docutils literal">mjd_max</code></p></td>
364<td><p>float64</p></td>
365<td><p>days</p></td>
366<td><p>Maximum Modified Julian Date of observations used to construct the model of this object</p></td>
367</tr>
368<tr>
369<td><p><code class="docutils literal">ref_cat</code></p></td>
370<td><p>char[2]</p></td>
371<td></td>
372<td><p>Reference catalog source for this star: "T2" for <a class="reference external" href="https://heasarc.gsfc.nasa.gov/W3Browse/all/tycho2.html">Tycho-2</a>, "G3" for <a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a>, "L4" for the <a class="reference external" href="https://sga.readthedocs.io/en/latest/">SGA</a>, "<a class="reference external" href="https://github.com/legacysurvey/legacypipe/issues/766">MC</a>" for an object in one of the Magellanic Clouds, empty otherwise</p></td>
373</tr>
374<tr>
375<td><p><code class="docutils literal">ref_id</code></p></td>
376<td><p>int64</p></td>
377<td></td>
378<td><p>Reference catalog identifier for this star; Tyc1*1,000,000+Tyc2*10+Tyc3 for Tycho2;
378 "sourceid" for <a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> and <a class="reference external" href="https://sga.readthedocs.io/en/latest/">SGA</a>; 1/2 for the LMC/SMC when <code class="docutils literal">ref_cat</code> is "<a class="reference external" href="https://github.com/legacysurvey/legacypipe/issues/766">MC</a>"</p></td>
379</tr>
380<tr>
381<td><p><code class="docutils literal">pmra</code></p></td>
382<td><p>float32</p></td>
383<td><p>mas/yr</p></td>
384<td><p>Reference catalog proper motion in RA direction (<span class="math">\(\mu_\alpha^*\equiv\mu_\alpha\cos\delta\)</span>) in the ICRS at <code class="docutils literal">ref_epoch</code></p></td>
385</tr>
386<tr>
387<td><p><code class="docutils literal">pmdec</code></p></td>
388<td><p>float32</p></td>
389<td><p>mas/yr</p></td>
390<td><p>Reference catalog proper motion in Dec direction (<span class="math">\(\mu_\delta\)</span>) in the ICRS at <code class="docutils literal">ref_epoch</code></p></td>
391</tr>
392<tr>
393<td><p><code class="docutils literal">parallax</code></p></td>
394<td><p>float32</p></td>
395<td><p>mas</p></td>
396<td><p>Reference catalog parallax</p></td>
397</tr>
398<tr>
399<td><p><code class="docutils literal">pmra_ivar</code></p></td>
400<td><p>float32</p></td>
401<td><p>1/(mas/yr)²</p></td>
402<td><p>Reference catalog inverse-variance on <code class="docutils literal">pmra</code></p></td>
403</tr>
404<tr>
405<td><p><code class="docutils literal">pmdec_ivar</code></p></td>
406<td><p>float32</p></td>
407<td><p>1/(mas/yr)²</p></td>
408<td><p>Reference catalog inverse-variance on <code class="docutils literal">pmdec</code></p></td>
409</tr>
410<tr>
411<td><p><code class="docutils literal">parallax_ivar</code></p></td>
412<td><p>float32</p></td>
413<td><p>1/mas²</p></td>
414<td><p>Reference catalog inverse-variance on <code class="docutils literal">parallax</code></p></td>
415</tr>
416<tr>
417<td><p><code class="docutils literal">ref_epoch</code></p></td>
418<td><p>float32</p></td>
419<td><p>yr</p></td>
420<td><p>Reference catalog reference epoch (eg, 2015.5 for <a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a>)</p></td>
421</tr>
422<tr>
423<td><p><code class="docutils literal">gaia_phot_g_mean_mag</code></p></td>
424<td><p>float32</p></td>
425<td><p>mag</p></td>
426<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> G band mag</p></td>
427</tr>
428<tr>
429<td><p><code class="docutils literal">gaia_phot_g_mean_flux_over_error</code></p></td>
430<td><p>float32</p></td>
431<td></td>
432<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> G band signal-to-noise</p></td>
433</tr>
434<tr>
435<td><p><code class="docutils literal">gaia_phot_g_n_obs</code></p></td>
436<td><p>int32</p></td>
437<td></td>
438<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> G band number of observations</p></td>
439</tr>
440<tr>
441<td><p><code class="docutils literal">gaia_phot_bp_mean_mag</code></p></td>
442<td><p>float32</p></td>
443<td><p>mag</p></td>
444<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> BP mag</p></td>
445</tr>
446<tr>
447<td><p><code class="docutils literal">gaia_phot_bp_mean_flux_over_error</code></p></td>
448<td><p>float32</p></td>
449<td></td>
450<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> BP signal-to-noise</p></td>
451</tr>
452<tr>
453<td><p><code class="docutils literal">gaia_phot_bp_n_obs</code></p></td>
454<td><p>int32</p></td>
455<td></td>
456<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> BP number of observations</p></td>
457</tr>
458<tr>
459<td><p><code class="docutils literal">gaia_phot_rp_mean_mag</code></p></td>
460<td><p>float32</p></td>
461<td><p>mag</p></td>
462<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> RP mag</p></td>
463</tr>
464<tr>
465<td><p><code class="docutils literal">gaia_phot_rp_mean_flux_over_error</code></p></td>
466<td><p>float32</p></td>
467<td></td>
468<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> RP signal-to-noise</p></td>
469</tr>
470<tr>
471<td><p><code class="docutils literal">gaia_phot_rp_n_obs</code></p></td>
472<td><p>int32</p></td>
473<td></td>
474<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> RP number of observations</p></td>
475</tr>
476<tr>
477<td><p><code class="docutils literal">gaia_phot_variable_flag</code></p></td>
478<td><p>bool</p></td>
479<td></td>
480<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> photometric variable flag</p></td>
481</tr>
482<tr>
483<td><p><code class="docutils literal">gaia_astrometric_excess_noise</code></p></td>
484<td><p>float32</p></td>
485<td></td>
486<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> astrometric excess noise</p></td>
487</tr>
488<tr>
489<td><p><code class="docutils literal">gaia_astrometric_excess_noise_sig</code></p></td>
490<td><p>float32</p></td>
491<td></td>
492<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> astrometric excess noise uncertainty</p></td>
493</tr>
494<tr>
495<td><p><code class="docutils literal">gaia_astrometric_n_obs_al</code></p></td>
496<td><p>int16</p></td>
497<td></td>
498<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> number of astrometric observations along scan direction</p></td>
499</tr>
500<tr>
501<td><p><code class="docutils literal">gaia_astrometric_n_good_obs_al</code></p></td>
502<td><p>int16</p></td>
503<td></td>
504<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> number of good astrometric observations along scan direction</p></td>
505</tr>
506<tr>
507<td><p><code class="docutils literal">gaia_astrometric_weight_al</code></p></td>
508<td><p>float32</p></td>
509<td></td>
510<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> astrometric weight along scan direction</p></td>
511</tr>
512<tr>
513<td><p><code class="docutils literal">gaia_duplicated_source</code></p></td>
514<td><p>bool</p></td>
515<td></td>
516<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> duplicated source flag</p></td>
517</tr>
518<tr>
519<td><p><code class="docutils literal">gaia_a_g_val</code></p></td>
520<td><p>float32</p></td>
521<td><p>magnitudes</p></td>
522<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> line-of-sight extinction in the G band</p></td>
523</tr>
524<tr>
525<td><p><code class="docutils literal">gaia_e_bp_min_rp_val</code></p></td>
526<td><p>float32</p></td>
527<td><p>magnitudes</p></td>
528<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> line-of-sight reddening E(BP-RP)</p></td>
529</tr>
530<tr>
531<td><p><code class="docutils literal">gaia_phot_bp_rp_excess_factor</code></p></td>
532<td><p>float32</p></td>
533<td></td>
534<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> BP/RP excess factor</p></td>
535</tr>
536<tr>
537<td><p><code class="docutils literal">gaia_astrometric_sigma5d_max</code></p></td>
538<td><p>float32</p></td>
539<td><p>mas</p></td>
540<td><p><a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> longest semi-major axis of the 5-d error ellipsoid</p></td>
541</tr>
542<tr>
543<td><p><code class="docutils literal">gaia_astrometric_params_solved</code></p></td>
544<td><p>uint8</p></td>
545<td></td>
546<td><p>Which astrometric parameters were estimated for a <a class="reference external" href="https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_main_source_catalogue/ssec_dm_gaia_source.html">Gaia DR3</a> source</p></td>
547</tr>
548<tr>
549<td><p><code class="docutils literal">flux_g</code></p></td>
550<td><p>float32</p></td>
551<td><p>nanomaggy</p></td>
552<td><p>model flux in <span class="math">\(g\)</span></p></td>
553</tr>
554<tr>
555<td><p><code class="docutils literal">flux_r</code></p></td>
556<td><p>float32</p></td>
557<td><p>nanomaggy</p></td>
558<td><p>model flux in <span class="math">\(r\)</span></p></td>
559</tr>
560<tr>
561<td><p><code class="docutils literal">flux_i</code></p></td>
562<td><p>float32</p></td>
563<td><p>nanomaggy</p></td>
564<td><p>model flux in <span class="math">\(i\)</span></p></td>
565</tr>
566<tr>
567<td><p><code class="docutils literal">flux_z</code></p></td>
568<td><p>float32</p></td>
569<td><p>nanomaggy</p></td>
570<td><p>model flux in <span class="math">\(z\)</span></p></td>
571</tr>
572<tr>
573<td><p><code class="docutils literal">flux_w1</code></p></td>
574<td><p>float32</p></td>
575<td><p>nanomaggy</p></td>
576<td><p>WISE model flux in <span class="math">\(W1\)</span> (AB system)</p></td>
577</tr>
578<tr>
579<td><p><code class="docutils literal">flux_w2</code></p></td>
580<td><p>float32</p></td>
581<td><p>nanomaggy</p></td>
582<td><p>WISE model flux in <span class="math">\(W2\)</span> (AB)</p></td>
583</tr>
584<tr>
585<td><p><code class="docutils literal">flux_w3</code></p></td>
586<td><p>float32</p></td>
587<td><p>nanomaggy</p></td>
588<td><p>WISE model flux in <span class="math">\(W3\)</span> (AB)</p></td>
589</tr>
590<tr>
591<td><p><code class="docutils literal">flux_w4</code></p></td>
592<td><p>float32</p></td>
593<td><p>nanomaggy</p></td>
594<td><p>WISE model flux in <span class="math">\(W4\)</span> (AB)</p></td>
595</tr>
596<tr>
597<td><p><code class="docutils literal">flux_ivar_g</code></p></td>
598<td><p>float32</p></td>
599<td><p>1/nanomaggy²</p></td>
600<td><p>Inverse variance of <code class="docutils literal">flux_g</code></p></td>
601</tr>
602<tr>
603<td><p><code class="docutils literal">flux_ivar_r</code></p></td>
604<td><p>float32</p></td>
605<td><p>1/nanomaggy²</p></td>
606<td><p>Inverse variance of <code class="docutils literal">flux_r</code></p></td>
607</tr>
608<tr>
609<td><p><code class="docutils literal">flux_ivar_i</code></p></td>
610<td><p>float32</p></td>
611<td><p>1/nanomaggy²</p></td>
612<td><p>Inverse variance of <code class="docutils literal">flux_i</code></p></td>
613</tr>
614<tr>
615<td><p><code class="docutils literal">flux_ivar_z</code></p></td>
616<td><p>float32</p></td>
617<td><p>1/nanomaggy²</p></td>
618<td><p>Inverse variance of <code class="docutils literal">flux_z</code></p></td>
619</tr>
620<tr>
621<td><p><code class="docutils literal">flux_ivar_w1</code></p></td>
622<td><p>float32</p></td>
623<td><p>1/nanomaggy²</p></td>
624<td><p>Inverse variance of <code class="docutils literal">flux_w1</code> (AB system)</p></td>
625</tr>
626<tr>
627<td><p><code class="docutils literal">flux_ivar_w2</code></p></td>
628<td><p>float32</p></td>
629<td><p>1/nanomaggy²</p></td>
630<td><p>Inverse variance of <code class="docutils literal">flux_w2</code> (AB)</p></td>
631</tr>
632<tr>
633<td><p><code class="docutils literal">flux_ivar_w3</code></p></td>
634<td><p>float32</p></td>
635<td><p>1/nanomaggy²</p></td>
636<td><p>Inverse variance of <code class="docutils literal">flux_w3</code> (AB)</p></td>
637</tr>
638<tr>
639<td><p><code class="docutils literal">flux_ivar_w4</code></p></td>
640<td><p>float32</p></td>
641<td><p>1/nanomaggy²</p></td>
642<td><p>Inverse variance of <code class="docutils literal">flux_w4</code> (AB)</p></td>
643</tr>
644<tr>
645<td><p><code class="docutils literal">fiberflux_g</code></p></td>
646<td><p>float32</p></td>
647<td><p>nanomaggy</p></td>
648<td><p>Predicted <span class="math">\(g\)</span>-band flux within a fiber of diameter 1.5 arcsec from this object in 1 arcsec Gaussian seeing</p></td>
649</tr>
650<tr>
651<td><p><code class="docutils literal">fiberflux_r</code></p></td>
652<td><p>float32</p></td>
653<td><p>nanomaggy</p></td>
654<td><p>Predicted <span class="math">\(r\)</span>-band flux within a fiber of diameter 1.5 arcsec from this object in 1 arcsec Gaussian seeing</p></td>
655</tr>
656<tr>
657<td><p><code class="docutils literal">fiberflux_i</code></p></td>
658<td><p>float32</p></td>
659<td><p>nanomaggy</p></td>
660<td><p>Predicted <span class="math">\(i\)</span>-band flux within a fiber of diameter 1.5 arcsec from this object in 1 arcsec Gaussian seeing</p></td>
661</tr>
662<tr>
663<td><p><code class="docutils literal">fiberflux_z</code></p></td>
664<td><p>float32</p></td>
665<td><p>nanomaggy</p></td>
666<td><p>Predicted <span class="math">\(z\)</span>-band flux within a fiber of diameter 1.5 arcsec from this object in 1 arcsec Gaussian seeing</p></td>
667</tr>
668<tr>
669<td><p><code class="docutils literal">fibertotflux_g</code></p></td>
670<td><p>float32</p></td>
671<td><p>nanomaggy</p></td>
672<td><p>Predicted <span class="math">\(g\)</span>-band flux within a fiber of diameter 1.5 arcsec from all sources at this location in 1 arcsec Gaussian seeing</p></td>
673</tr>
674<tr>
675<td><p><code class="docutils literal">fibertotflux_r</code></p></td>
676<td><p>float32</p></td>
677<td><p>nanomaggy</p></td>
678<td><p>Predicted <span class="math">\(r\)</span>-band flux within a fiber of diameter 1.5 arcsec from all sources at this location in 1 arcsec Gaussian seeing</p></td>
679</tr>
680<tr>
681<td><p><code class="docutils literal">fibertotflux_i</code></p></td>
682<td><p>float32</p></td>
683<td><p>nanomaggy</p></td>
684<td><p>Predicted <span class="math">\(i\)</span>-band flux within a fiber of diameter 1.5 arcsec from all sources at this location in 1 arcsec Gaussian seeing</p></td>
685</tr>
686<tr>
687<td><p><code class="docutils literal">fibertotflux_z</code></p></td>
688<td><p>float32</p></td>
689<td><p>nanomaggy</p></td>
690<td><p>Predicted <span class="math">\(z\)</span>-band flux within a fiber of diameter 1.5 arcsec from all sources at this location in 1 arcsec Gaussian seeing</p></td>
691</tr>
692<tr>
693<td><p><code class="docutils literal">apflux_g</code></p></td>
694<td><p>float32[8]</p></td>
695<td><p>nanomaggy</p></td>
696<td><p>Aperture fluxes on the co-added images in apertures of radius [0.5, 0.75, 1.0, 1.5, 2.0, 3.5, 5.0, 7.0] arcsec in <span class="math">\(g\)</span>, masked by <span class="math">\(invvar=0\)</span> (inverse variance of zero <a class="brackets" href="#footnote-1" id="footnote-reference-1" role="doc-noteref"><span class="fn-bracket">[</span>1<span class="fn-bracket">]</span></a>)</p></td>
697</tr>
698<tr>
699<td><p><code class="docutils literal">apflux_r</code></p></td>
700<td><p>float32[8]</p></td>
701<td><p>nanomaggy</p></td>
702<td><p>Aperture fluxes on the co-added images in apertures of radius [0.5, 0.75, 1.0, 1.5, 2.0, 3.5, 5.0, 7.0] arcsec in <span class="math">\(r\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
703</tr>
704<tr>
705<td><p><code class="docutils literal">apflux_i</code></p></td>
706<td><p>float32[8]</p></td>
707<td><p>nanomaggy</p></td>
708<td><p>Aperture fluxes on the co-adde
708d images in apertures of radius [0.5, 0.75, 1.0, 1.5, 2.0, 3.5, 5.0, 7.0] arcsec in <span class="math">\(i\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
709</tr>
710<tr>
711<td><p><code class="docutils literal">apflux_z</code></p></td>
712<td><p>float32[8]</p></td>
713<td><p>nanomaggy</p></td>
714<td><p>Aperture fluxes on the co-added images in apertures of radius [0.5, 0.75, 1.0, 1.5, 2.0, 3.5, 5.0, 7.0] arcsec in <span class="math">\(z\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
715</tr>
716<tr>
717<td><p><code class="docutils literal">apflux_resid_g</code></p></td>
718<td><p>float32[8]</p></td>
719<td><p>nanomaggy</p></td>
720<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(g\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
721</tr>
722<tr>
723<td><p><code class="docutils literal">apflux_resid_r</code></p></td>
724<td><p>float32[8]</p></td>
725<td><p>nanomaggy</p></td>
726<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(r\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
727</tr>
728<tr>
729<td><p><code class="docutils literal">apflux_resid_i</code></p></td>
730<td><p>float32[8]</p></td>
731<td><p>nanomaggy</p></td>
732<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(i\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
733</tr>
734<tr>
735<td><p><code class="docutils literal">apflux_resid_z</code></p></td>
736<td><p>float32[8]</p></td>
737<td><p>nanomaggy</p></td>
738<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(z\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
739</tr>
740<tr>
741<td><p><code class="docutils literal">apflux_blobresid_g</code></p></td>
742<td><p>float32[8]</p></td>
743<td><p>nanomaggy</p></td>
744<td><p>Aperture fluxes on <span class="math">\(image-blobmodel\)</span> residual maps in <span class="math">\(g\)</span> <a class="brackets" href="#footnote-2" id="footnote-reference-2" role="doc-noteref"><span class="fn-bracket">[</span>2<span class="fn-bracket">]</span></a>, masked by <span class="math">\(invvar=0\)</span></p></td>
745</tr>
746<tr>
747<td><p><code class="docutils literal">apflux_blobresid_r</code></p></td>
748<td><p>float32[8]</p></td>
749<td><p>nanomaggy</p></td>
750<td><p>Aperture fluxes on <span class="math">\(image-blobmodel\)</span> residual maps in <span class="math">\(r\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
751</tr>
752<tr>
753<td><p><code class="docutils literal">apflux_blobresid_i</code></p></td>
754<td><p>float32[8]</p></td>
755<td><p>nanomaggy</p></td>
756<td><p>Aperture fluxes on <span class="math">\(image-blobmodel\)</span> residual maps in <span class="math">\(i\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
757</tr>
758<tr>
759<td><p><code class="docutils literal">apflux_blobresid_z</code></p></td>
760<td><p>float32[8]</p></td>
761<td><p>nanomaggy</p></td>
762<td><p>Aperture fluxes on <span class="math">\(image-blobmodel\)</span> residual maps in <span class="math">\(z\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
763</tr>
764<tr>
765<td><p><code class="docutils literal">apflux_ivar_g</code></p></td>
766<td><p>float32[8]</p></td>
767<td><p>1/nanomaggy²</p></td>
768<td><p>Inverse variance of <code class="docutils literal">apflux_resid_g</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
769</tr>
770<tr>
771<td><p><code class="docutils literal">apflux_ivar_r</code></p></td>
772<td><p>float32[8]</p></td>
773<td><p>1/nanomaggy²</p></td>
774<td><p>Inverse variance of <code class="docutils literal">apflux_resid_r</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
775</tr>
776<tr>
777<td><p><code class="docutils literal">apflux_ivar_i</code></p></td>
778<td><p>float32[8]</p></td>
779<td><p>1/nanomaggy²</p></td>
780<td><p>Inverse variance of <code class="docutils literal">apflux_resid_i</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
781</tr>
782<tr>
783<td><p><code class="docutils literal">apflux_ivar_z</code></p></td>
784<td><p>float32[8]</p></td>
785<td><p>1/nanomaggy²</p></td>
786<td><p>Inverse variance of <code class="docutils literal">apflux_resid_z</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
787</tr>
788<tr>
789<td><p><code class="docutils literal">apflux_masked_g</code></p></td>
790<td><p>float32[8]</p></td>
791<td></td>
792<td><p>Fraction of pixels masked in <span class="math">\(g\)</span>-band aperture flux measurements; 1 means fully masked (ie, fully ignored; contributing zero to the measurement)</p></td>
793</tr>
794<tr>
795<td><p><code class="docutils literal">apflux_masked_r</code></p></td>
796<td><p>float32[8]</p></td>
797<td></td>
798<td><p>Fraction of pixels masked in <span class="math">\(r\)</span>-band aperture flux measurements; 1 means fully masked (ie, fully ignored; contributing zero to the measurement)</p></td>
799</tr>
800<tr>
801<td><p><code class="docutils literal">apflux_masked_i</code></p></td>
802<td><p>float32[8]</p></td>
803<td></td>
804<td><p>Fraction of pixels masked in <span class="math">\(i\)</span>-band aperture flux measurements; 1 means fully masked (ie, fully ignored; contributing zero to the measurement)</p></td>
805</tr>
806<tr>
807<td><p><code class="docutils literal">apflux_masked_z</code></p></td>
808<td><p>float32[8]</p></td>
809<td></td>
810<td><p>Fraction of pixels masked in <span class="math">\(z\)</span>-band aperture flux measurements; 1 means fully masked (ie, fully ignored; contributing zero to the measurement)</p></td>
811</tr>
812<tr>
813<td><p><code class="docutils literal">apflux_w1</code></p></td>
814<td><p>float32[5]</p></td>
815<td><p>nanomaggy</p></td>
816<td><p>Aperture fluxes on the co-added images in apertures of radius [3, 5, 7, 9, 11] <a class="brackets" href="#footnote-3" id="footnote-reference-3" role="doc-noteref"><span class="fn-bracket">[</span>3<span class="fn-bracket">]</span></a> arcsec in <span class="math">\(W1\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
817</tr>
818<tr>
819<td><p><code class="docutils literal">apflux_w2</code></p></td>
820<td><p>float32[5]</p></td>
821<td><p>nanomaggy</p></td>
822<td><p>Aperture fluxes on the co-added images in apertures of radius [3, 5, 7, 9, 11] arcsec in <span class="math">\(W2\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
823</tr>
824<tr>
825<td><p><code class="docutils literal">apflux_w3</code></p></td>
826<td><p>float32[5]</p></td>
827<td><p>nanomaggy</p></td>
828<td><p>Aperture fluxes on the co-added images in apertures of radius [3, 5, 7, 9, 11] arcsec in <span class="math">\(W3\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
829</tr>
830<tr>
831<td><p><code class="docutils literal">apflux_w4</code></p></td>
832<td><p>float32[5]</p></td>
833<td><p>nanomaggy</p></td>
834<td><p>Aperture fluxes on the co-added images in apertures of radius [3, 5, 7, 9, 11] arcsec in <span class="math">\(W4\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
835</tr>
836<tr>
837<td><p><code class="docutils literal">apflux_resid_w1</code></p></td>
838<td><p>float32[5]</p></td>
839<td><p>nanomaggy</p></td>
840<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(W1\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
841</tr>
842<tr>
843<td><p><code class="docutils literal">apflux_resid_w2</code></p></td>
844<td><p>float32[5]</p></td>
845<td><p>nanomaggy</p></td>
846<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(W2\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
847</tr>
848<tr>
849<td><p><code class="docutils literal">apflux_resid_w3</code></p></td>
850<td><p>float32[5]</p></td>
851<td><p>nanomaggy</p></td>
852<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(W3\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
853</tr>
854<tr>
855<td><p><code class="docutils literal">apflux_resid_w4</code></p></td>
856<td><p>float32[5]</p></td>
857<td><p>nanomaggy</p></td>
858<td><p>Aperture fluxes on the co-added residual images in <span class="math">\(W4\)</span>, masked by <span class="math">\(invvar=0\)</span></p></td>
859</tr>
860<tr>
861<td><p><code class="docutils literal">apflux_ivar_w1</code></p></td>
862<td><p>float32[5]</p></td>
863<td><p>1/nanomaggy²</p></td>
864<td><p>Inverse variance of <code class="docutils literal">apflux_resid_w1</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
865</tr>
866<tr>
867<td><p><code class="docutils literal">apflux_ivar_w2</code></p></td>
868<td><p>float32[5]</p></td>
869<td><p>1/nanomaggy²</p></td>
870<td><p>Inverse variance of <code class="docutils literal">apflux_resid_w2</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
871</tr>
872<tr>
873<td><p><code class="docutils literal">apflux_ivar_w3</code></p></td>
874<td><p>float32[5]</p></td>
875<td><p>1/nanomaggy²</p></td>
876<td><p>Inverse variance of <code class="docutils literal">apflux_resid_w3</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
877</tr>
878<tr>
879<td><p><code class="docutils literal">apflux_ivar_w4</code></p></td>
880<td><p>float32[5]</p></td>
881<td><p>1/nanomaggy²</p></td>
882<td><p>Inverse variance of <code class="docutils literal">apflux_resid_w4</code>, masked by <span class="math">\(invvar=0\)</span></p></td>
883</tr>
884<tr>
885<td><p><code class="docutils literal">mw_transmission_g</code></p></td>
886<td><p>float32</p></td>
887<td></td>
888<td><p>Galactic transmission in <span class="math">\(g\)</span> filter in linear units [0, 1]</p></td>
889</tr>
890<tr>
891<td><p><code class="docutils literal">mw_transmission_r</code></p></td>
892<td><p>float32</p></td>
893<td></td>
894<td><p>Galactic transmission in <span class="math">\(r\)</span> filter in linear units [0, 1]</p></td>
895</tr>
896<tr>
897<td><p><code class="docutils literal">mw_transmission_i</code></p></td>
898<td><p>float32</p></td>
899<td></td>
900<td><p>Galactic transmission in <span class="math">\(i\)</span> filter in linear units [0, 1]</p></td>
901</tr>
902<tr>
903<td><p><code class="docutils literal">mw_transmission_z</code></p></td>
904<td><p>float32</p></td>
905<td></td>
906<td><p>Galactic transmission in <span class="math">\(z\)</span> filter in linear units [0, 1]</p></td>
907</tr>
908<tr>
909<td><p><code class="docutils literal">mw_transmission_w1</code></p></td>
910<td><p>float32</p></td>
911<td></td>
912<td><p>Galactic transmission in <span class="math">\(W1\)</span> filter in linear units [0, 1]</p></td>
913</tr>
914<tr>
915<td><p><code class="docutils literal">mw_transmission_w2</code></p></td>
916<td><p>float32</p></td>
917<td></td>
918<td><p>Galactic transmission in <span class="math">\(W2\)</span> filter in linear units [0, 1]</p></td>
919</tr>
920<tr>
921<td><p><code class="docutils literal">mw_transmission_w3</code></p></td>
922<td><p>float32</p></td>
923<td></td>
924<td><p>Galactic transmission in <span class="math">\(W3\)</span> filter in linear units [0, 1]</p></td>
925</tr>
926<tr>
927<td><p><code class="docutils literal">mw_transmission_w4</code></p></td>
928<td><p>float32</p></td>
929<td></td>
930<td><p>Galactic transmission in <span class="math">\(W4\)</span> filter in linear units [0, 1]</p></td>
931</tr>
932<tr>
933<td><p><code class="docutils literal">nobs_g</code></p></td>
934<td><p>int16</p></td>
935<td></td>
936<td><p>Number of images that contribute to the central pixel in <span class="math">\(g\)</span> filter for this object (not profile-weighted)</p></td>
937</tr>
938<tr>
939<td><p><code class="docutils literal">nobs_r</code></p></td>
940<td><p>int16</p></td>
941<td></td>
942<td><p>Number of images that contribute to the central pixel in <span class="math">\(r\)</span> filter for this object (not profile-weighted)</p></td>
943</tr>
944<tr>
945<td><p><code class="docutils literal">nobs_i</code></p></td>
946<td><p>int16</p></td>
947<td></td>
948<td><p>Number of images that contribute to the central pixel in <span class="math">\(i\)</span> filter for this object (not profile-weighted)</p></td>
949</tr>
950<tr>
951<td><p><code class="docutils literal">nobs_z</code></p></td>
952<td><p>int16</p></td>
953<td></td>
954<td><p>Number of images that contribute to the central pixel in <span class="math">\(z\)</span> filter for this object (not profile-weighted)</p></td>
955</tr>
956<tr>
957<td><p><code class="docutils literal">nobs_w1</code></p></td>
958<td><p>int16</p></td>
959<td></td>
960<td><p>Number of images that contribute to the central pixel in <span class="math">\(W1\)</span> filter for this object (not profile-weighted)</p></td>
961</tr>
962<tr>
963<td><p><code class="docutils literal">nobs_w2</code></p></td>
964<td><p>int16</p></td>
965<td></td>
966<td><p>Number of images that contribute to the central pixel in <span class="math">\(W2\)</span> filter for this object (not profile-weighted)</p></td>
967</tr>
968<tr>
969<td><p><code class="docutils literal">nobs_w3</code></p></td>
970<td><p>int16</p></td>
971<td></td>
972<td><p>Number of images that contribute to the central pixel in <span class="math">\(W3\)</span> filter for this object (not profile-weighted)</p></td>
973</tr>
974<tr>
975<td><p><code class="docutils literal">nobs_w4</code></p></td>
976<td><p>int16</p></td>
977<td></td>
978<td><p>Number of images that contribute to the central pixel in <span class="math">\(W4\)</span> filter for this object (not profile-weighted)</p></td>
979</tr>
980<tr>
981<td><p><code class="docutils literal">rchisq_g</code></p></td>
982<td><p>float32</p></td>
983<td></td>
984<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(g\)</span></p></td>
985</tr>
986<tr>
987<td><p><code class="docutils literal">rchisq_r</code></p></td>
988<td><p>float32</p></td>
989<td></td>
990<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(r\)</span></p></td>
991</tr>
992<tr>
993<td><p><code class="docutils literal">rchisq_i</code></p></td>
994<td><p>float32</p></td>
995<td></td>
996<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(i\)</span></p></td>
997</tr>
998<tr>
999<td><p><code class="docutils literal">rchisq_z</code></p></td>
1000<td><p>float32</p></td>
1001<td></td>
1002<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(z\)</span></p></td>
1003</tr>
1004<tr>
1005<td><p><code class="docutils literal">rchisq_w1</code></p></td>
1006<td><p>float32</p></td>
1007<td></td>
1008<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(W1\)</span></p></td>
1009</tr>
1010<tr>
1011<td><p><code class="docutils literal">rchisq_w2</code></p></td>
1012<td><p>float32</p></td>
1013<td></td>
1014<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(W2\)</span></p></td>
1015</tr>
1016<tr>
1017<td><p><code class="docutils literal">rchisq_w3</code></p></td>
1018<td><p>float32</p></td>
1019<td></td>
1020<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(W3\)</span></p></td>
1021</tr>
1022<tr>
1023<td><p><code class="docutils literal">rchisq_w4</code></p></td>
1024<td><p>float32</p></td>
1025<td></td>
1026<td><p>Profile-weighted χ² of model fit normalized by the number of pixels in <span class="math">\(W4\)</span></p></td>
1027</tr>
1028<tr>
1029<td><p><code class="docutils literal">fracflux_g</code></p></td>
1030<td><p>float32</p></td>
1031<td></td>
1032<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(g\)</span> (typically [0,1])</p></td>
1033</tr>
1034<tr>
1035<td><p><code class="docutils literal">fracflux_r</code></p></td>
1036<td><p>float32</p></td>
1037<td></td>
1038<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(r\)</span> (typically [0,1])</p></td>
1039</tr>
1040<tr>
1041<td><p><code class="docutils literal">fracflux_i</code></p></td>
1042<td><p>float32</p></td>
1043<td></td>
1044<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(i\)</span> (typically [0,1])</p></td>
1045</tr>
1046<tr>
1047<td><p><code class="docutils literal">fracflux_z</code></p></td>
1048<td><p>float32</p></td>
1049<td></td>
1050<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(z\)</span> (typically [0,1])</p></td>
1051</tr>
1052<tr>
1053<td><p><code class="docutils literal">fracflux_w1</code></p></td>
1054<td><p>float32</p></td>
1055<td></td>
1056<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(W1\)</span> (typically [0,1])</p></td>
1057</tr>
1058<tr>
1059<td><p><code class="docutils literal">fracflux_w2</code></p></td>
1060<td><p>float32</p></td>
1061<td></td>
1062<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(W2\)</span> (typically [0,1])</p></td>
1063</tr>
1064<tr>
1065<td><p><code class="docutils literal">fracflux_w3</code></p></td>
1066<td><p>float32</p
1066></td>
1067<td></td>
1068<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(W3\)</span> (typically [0,1])</p></td>
1069</tr>
1070<tr>
1071<td><p><code class="docutils literal">fracflux_w4</code></p></td>
1072<td><p>float32</p></td>
1073<td></td>
1074<td><p>Profile-weighted fraction of the flux from other sources divided by the total flux in <span class="math">\(W4\)</span> (typically [0,1])</p></td>
1075</tr>
1076<tr>
1077<td><p><code class="docutils literal">fracmasked_g</code></p></td>
1078<td><p>float32</p></td>
1079<td></td>
1080<td><p>Profile-weighted fraction of pixels masked from all observations of this object in <span class="math">\(g\)</span>, strictly between [0,1]</p></td>
1081</tr>
1082<tr>
1083<td><p><code class="docutils literal">fracmasked_r</code></p></td>
1084<td><p>float32</p></td>
1085<td></td>
1086<td><p>Profile-weighted fraction of pixels masked from all observations of this object in <span class="math">\(r\)</span>, strictly between [0,1]</p></td>
1087</tr>
1088<tr>
1089<td><p><code class="docutils literal">fracmasked_i</code></p></td>
1090<td><p>float32</p></td>
1091<td></td>
1092<td><p>Profile-weighted fraction of pixels masked from all observations of this object in <span class="math">\(i\)</span>, strictly between [0,1]</p></td>
1093</tr>
1094<tr>
1095<td><p><code class="docutils literal">fracmasked_z</code></p></td>
1096<td><p>float32</p></td>
1097<td></td>
1098<td><p>Profile-weighted fraction of pixels masked from all observations of this object in <span class="math">\(z\)</span>, strictly between [0,1]</p></td>
1099</tr>
1100<tr>
1101<td><p><code class="docutils literal">fracin_g</code></p></td>
1102<td><p>float32</p></td>
1103<td></td>
1104<td><p>Fraction of a source's flux within the blob in <span class="math">\(g\)</span>, near unity for real sources</p></td>
1105</tr>
1106<tr>
1107<td><p><code class="docutils literal">fracin_r</code></p></td>
1108<td><p>float32</p></td>
1109<td></td>
1110<td><p>Fraction of a source's flux within the blob in <span class="math">\(r\)</span>, near unity for real sources</p></td>
1111</tr>
1112<tr>
1113<td><p><code class="docutils literal">fracin_i</code></p></td>
1114<td><p>float32</p></td>
1115<td></td>
1116<td><p>Fraction of a source's flux within the blob in <span class="math">\(i\)</span>, near unity for real sources</p></td>
1117</tr>
1118<tr>
1119<td><p><code class="docutils literal">fracin_z</code></p></td>
1120<td><p>float32</p></td>
1121<td></td>
1122<td><p>Fraction of a source's flux within the blob in <span class="math">\(z\)</span>, near unity for real sources</p></td>
1123</tr>
1124<tr>
1125<td><p><code class="docutils literal">ngood_g</code></p></td>
1126<td><p>int16</p></td>
1127<td></td>
1128<td><p>Number of <cite>good</cite> (unmasked) images that contribute in <span class="math">\(g\)</span> (this quantity is consistent with the <cite>nexp</cite> maps in the <a class="reference external" href="../files/#image-stacks-region-coadd">image stacks</a>)</p></td>
1129</tr>
1130<tr>
1131<td><p><code class="docutils literal">ngood_r</code></p></td>
1132<td><p>int16</p></td>
1133<td></td>
1134<td><p>Number of <cite>good</cite> (unmasked) images that contribute in <span class="math">\(r\)</span> (this quantity is consistent with the <cite>nexp</cite> maps in the <a class="reference external" href="../files/#image-stacks-region-coadd">image stacks</a>)</p></td>
1135</tr>
1136<tr>
1137<td><p><code class="docutils literal">ngood_i</code></p></td>
1138<td><p>int16</p></td>
1139<td></td>
1140<td><p>Number of <cite>good</cite> (unmasked) images that contribute in <span class="math">\(i\)</span> (this quantity is consistent with the <cite>nexp</cite> maps in the <a class="reference external" href="../files/#image-stacks-region-coadd">image stacks</a>)</p></td>
1141</tr>
1142<tr>
1143<td><p><code class="docutils literal">ngood_z</code></p></td>
1144<td><p>int16</p></td>
1145<td></td>
1146<td><p>Number of <cite>good</cite> (unmasked) images that contribute in <span class="math">\(z\)</span> (this quantity is consistent with the <cite>nexp</cite> maps in the <a class="reference external" href="../files/#image-stacks-region-coadd">image stacks</a>)</p></td>
1147</tr>
1148<tr>
1149<td><p><code class="docutils literal">anymask_g</code></p></td>
1150<td><p>int16</p></td>
1151<td></td>
1152<td><p>Bitwise mask set if the central pixel from any image satisfies each condition in <span class="math">\(g\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1153</tr>
1154<tr>
1155<td><p><code class="docutils literal">anymask_r</code></p></td>
1156<td><p>int16</p></td>
1157<td></td>
1158<td><p>Bitwise mask set if the central pixel from any image satisfies each condition in <span class="math">\(r\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1159</tr>
1160<tr>
1161<td><p><code class="docutils literal">anymask_i</code></p></td>
1162<td><p>int16</p></td>
1163<td></td>
1164<td><p>Bitwise mask set if the central pixel from any image satisfies each condition in <span class="math">\(i\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1165</tr>
1166<tr>
1167<td><p><code class="docutils literal">anymask_z</code></p></td>
1168<td><p>int16</p></td>
1169<td></td>
1170<td><p>Bitwise mask set if the central pixel from any image satisfies each condition in <span class="math">\(z\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1171</tr>
1172<tr>
1173<td><p><code class="docutils literal">allmask_g</code></p></td>
1174<td><p>int16</p></td>
1175<td></td>
1176<td><p>Bitwise mask set if the central pixel from all images satisfy each condition in <span class="math">\(g\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1177</tr>
1178<tr>
1179<td><p><code class="docutils literal">allmask_r</code></p></td>
1180<td><p>int16</p></td>
1181<td></td>
1182<td><p>Bitwise mask set if the central pixel from all images satisfy each condition in <span class="math">\(r\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1183</tr>
1184<tr>
1185<td><p><code class="docutils literal">allmask_i</code></p></td>
1186<td><p>int16</p></td>
1187<td></td>
1188<td><p>Bitwise mask set if the central pixel from all images satisfy each condition in <span class="math">\(i\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1189</tr>
1190<tr>
1191<td><p><code class="docutils literal">allmask_z</code></p></td>
1192<td><p>int16</p></td>
1193<td></td>
1194<td><p>Bitwise mask set if the central pixel from all images satisfy each condition in <span class="math">\(z\)</span> as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1195</tr>
1196<tr>
1197<td><p><code class="docutils literal">wisemask_w1</code></p></td>
1198<td><p>uint8</p></td>
1199<td></td>
1200<td><p>W1 bitmask as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1201</tr>
1202<tr>
1203<td><p><code class="docutils literal">wisemask_w2</code></p></td>
1204<td><p>uint8</p></td>
1205<td></td>
1206<td><p>W2 bitmask as cataloged on the <a class="reference external" href="../bitmasks">DR11 bitmasks page</a></p></td>
1207</tr>
1208<tr>
1209<td><p><code class="docutils literal">psfsize_g</code></p></td>
1210<td><p>float32</p></td>
1211<td><p>arcsec</p></td>
1212<td><p>Weighted average PSF FWHM in the <span class="math">\(g\)</span> band</p></td>
1213</tr>
1214<tr>
1215<td><p><code class="docutils literal">psfsize_r</code></p></td>
1216<td><p>float32</p></td>
1217<td><p>arcsec</p></td>
1218<td><p>Weighted average PSF FWHM in the <span class="math">\(r\)</span> band</p></td>
1219</tr>
1220<tr>
1221<td><p><code class="docutils literal">psfsize_i</code></p></td>
1222<td><p>float32</p></td>
1223<td><p>arcsec</p></td>
1224<td><p>Weighted average PSF FWHM in the <span class="math">\(i\)</span> band</p></td>
1225</tr>
1226<tr>
1227<td><p><code class="docutils literal">psfsize_z</code></p></td>
1228<td><p>float32</p></td>
1229<td><p>arcsec</p></td>
1230<td><p>Weighted average PSF FWHM in the <span class="math">\(z\)</span> band</p></td>
1231</tr>
1232<tr>
1233<td><p><code class="docutils literal">psfdepth_g</code></p></td>
1234<td><p>float32</p></td>
1235<td><p>1/nanomaggy²</p></td>
1236<td><p>For a <span class="math">\(5\sigma\)</span> point source detection limit in <span class="math">\(g\)</span>, <span class="math">\(5/\sqrt(\mathrm{psfdepth\_g})\)</span> gives flux in nanomaggies and <span class="math">\(-2.5[\log_{10}(5 / \sqrt(\mathrm{psfdepth\_g})) - 9]\)</span> gives corresponding AB magnitude</p></td>
1237</tr>
1238<tr>
1239<td><p><code class="docutils literal">psfdepth_r</code></p></td>
1240<td><p>float32</p></td>
1241<td><p>1/nanomaggy²</p></td>
1242<td><p>For a <span class="math">\(5\sigma\)</span> point source detection limit in <span class="math">\(r\)</span>, <span class="math">\(5/\sqrt(\mathrm{psfdepth\_r})\)</span> gives flux in nanomaggies and <span class="math">\(-2.5[\log_{10}(5 / \sqrt(\mathrm{psfdepth\_r})) - 9]\)</span> gives corresponding AB magnitude</p></td>
1243</tr>
1244<tr>
1245<td><p><code class="docutils literal">psfdepth_i</code></p></td>
1246<td><p>float32</p></td>
1247<td><p>1/nanomaggy²</p></td>
1248<td><p>For a <span class="math">\(5\sigma\)</span> point source detection limit in <span class="math">\(i\)</span>, <span class="math">\(5/\sqrt(\mathrm{psfdepth\_i})\)</span> gives flux in nanomaggies and <span class="math">\(-2.5[\log_{10}(5 / \sqrt(\mathrm{psfdepth\_i})) - 9]\)</span> gives corresponding AB magnitude</p></td>
1249</tr>
1250<tr>
1251<td><p><code class="docutils literal">psfdepth_z</code></p></td>
1252<td><p>float32</p></td>
1253<td><p>1/nanomaggy²</p></td>
1254<td><p>For a <span class="math">\(5\sigma\)</span> point source detection limit in <span class="math">\(z\)</span>, <span class="math">\(5/\sqrt(\mathrm{psfdepth\_z})\)</span> gives flux in nanomaggies and <span class="math">\(-2.5[\log_{10}(5 / \sqrt(\mathrm{psfdepth\_z})) - 9]\)</span> gives corresponding AB magnitude</p></td>
1255</tr>
1256<tr>
1257<td><p><code class="docutils literal">galdepth_g</code></p></td>
1258<td><p>float32</p></td>
1259<td><p>1/nanomaggy²</p></td>
1260<td><p>As for <code class="docutils literal">psfdepth_g</code> but for a galaxy (0.45" exp, round) detection sensitivity</p></td>
1261</tr>
1262<tr>
1263<td><p><code class="docutils literal">galdepth_r</code></p></td>
1264<td><p>float32</p></td>
1265<td><p>1/nanomaggy²</p></td>
1266<td><p>As for <code class="docutils literal">psfdepth_r</code> but for a galaxy (0.45" exp, round) detection sensitivity</p></td>
1267</tr>
1268<tr>
1269<td><p><code class="docutils literal">galdepth_i</code></p></td>
1270<td><p>float32</p></td>
1271<td><p>1/nanomaggy²</p></td>
1272<td><p>As for <code class="docutils literal">psfdepth_i</code> but for a galaxy (0.45" exp, round) detection sensitivity</p></td>
1273</tr>
1274<tr>
1275<td><p><code class="docutils literal">galdepth_z</code></p></td>
1276<td><p>float32</p></td>
1277<td><p>1/nanomaggy²</p></td>
1278<td><p>As for <code class="docutils literal">psfdepth_z</code> but for a galaxy (0.45" exp, round) detection sensitivity</p></td>
1279</tr>
1280<tr>
1281<td><p><code class="docutils literal">nea_g</code></p></td>
1282<td><p>float32</p></td>
1283<td><p>arcsec²</p></td>
1284<td><p><a class="reference external" href="../../dr9/nea">Noise equivalent area</a> in <span class="math">\(g\)</span>.</p></td>
1285</tr>
1286<tr>
1287<td><p><code class="docutils literal">nea_r</code></p></td>
1288<td><p>float32</p></td>
1289<td><p>arcsec²</p></td>
1290<td><p><a class="reference external" href="../../dr9/nea">Noise equivalent area</a> in <span class="math">\(r\)</span>.</p></td>
1291</tr>
1292<tr>
1293<td><p><code class="docutils literal">nea_i</code></p></td>
1294<td><p>float32</p></td>
1295<td><p>arcsec²</p></td>
1296<td><p><a class="reference external" href="../../dr9/nea">Noise equivalent area</a> in <span class="math">\(i\)</span>.</p></td>
1297</tr>
1298<tr>
1299<td><p><code class="docutils literal">nea_z</code></p></td>
1300<td><p>float32</p></td>
1301<td><p>arcsec²</p></td>
1302<td><p><a class="reference external" href="../../dr9/nea">Noise equivalent area</a> in <span class="math">\(z\)</span>.</p></td>
1303</tr>
1304<tr>
1305<td><p><code class="docutils literal">blob_nea_g</code></p></td>
1306<td><p>float32</p></td>
1307<td><p>arcsec²</p></td>
1308<td><p><a class="reference external" href="../../dr9/nea">Blob-masked noise equivalent area</a> in <span class="math">\(g\)</span>.</p></td>
1309</tr>
1310<tr>
1311<td><p><code class="docutils literal">blob_nea_r</code></p></td>
1312<td><p>float32</p></td>
1313<td><p>arcsec²</p></td>
1314<td><p><a class="reference external" href="../../dr9/nea">Blob-masked noise equivalent area</a> in <span class="math">\(r\)</span>.</p></td>
1315</tr>
1316<tr>
1317<td><p><code class="docutils literal">blob_nea_i</code></p></td>
1318<td><p>float32</p></td>
1319<td><p>arcsec²</p></td>
1320<td><p><a class="reference external" href="../../dr9/nea">Blob-masked noise equivalent area</a> in <span class="math">\(i\)</span>.</p></td>
1321</tr>
1322<tr>
1323<td><p><code class="docutils literal">blob_nea_z</code></p></td>
1324<td><p>float32</p></td>
1325<td><p>arcsec²</p></td>
1326<td><p><a class="reference external" href="../../dr9/nea">Blob-masked noise equivalent area</a> in <span class="math">\(z\)</span>.</p></td>
1327</tr>
1328<tr>
1329<td><p><code class="docutils literal">psfdepth_w1</code></p></td>
1330<td><p>float32</p></td>
1331<td><p>1/nanomaggy²</p></td>
1332<td><p>As for <code class="docutils literal">psfdepth_g</code> (and also on the AB system) but for WISE W1</p></td>
1333</tr>
1334<tr>
1335<td><p><code class="docutils literal">psfdepth_w2</code></p></td>
1336<td><p>float32</p></td>
1337<td><p>1/nanomaggy²</p></td>
1338<td><p>As for <code class="docutils literal">psfdepth_g</code> (and also on the AB system) but for WISE W2</p></td>
1339</tr>
1340<tr>
1341<td><p><code class="docutils literal">psfdepth_w3</code></p></td>
1342<td><p>float32</p></td>
1343<td><p>1/nanomaggy²</p></td>
1344<td><p>As for <code class="docutils literal">psfdepth_g</code> (and also on the AB system) but for WISE W3</p></td>
1345</tr>
1346<tr>
1347<td><p><code class="docutils literal">psfdepth_w4</code></p></td>
1348<td><p>float32</p></td>
1349<td><p>1/nanomaggy²</p></td>
1350<td><p>As for <code class="docutils literal">psfdepth_g</code> (and also on the AB system) but for WISE W4</p></td>
1351</tr>
1352<tr>
1353<td><p><code class="docutils literal">wise_coadd_id</code></p></td>
1354<td><p>char[8]</p></td>
1355<td></td>
1356<td><p>unWISE coadd brick name (corresponding to the, <em>e.g.</em>, <cite>legacysurvey-&lt;brick&gt;-image-W1.fits.fz</cite> <a class="reference external" href="../files/#image-stacks-south-coadd">
1356coadd file</a>) for the center of each object</p></td>
1357</tr>
1358<tr>
1359<td><p><code class="docutils literal">wise_x</code></p></td>
1360<td><p>float32</p></td>
1361<td><p>pix</p></td>
1362<td><p>X position of coordinates in the brick image stack that corresponds to <code class="docutils literal">wise_coadd_id</code> (see the <a class="reference external" href="../../dr9/updates/#data-model-changes">DR9 updates page</a> for transformations between <code class="docutils literal">wise_x</code> and <code class="docutils literal">bx</code>)</p></td>
1363</tr>
1364<tr>
1365<td><p><code class="docutils literal">wise_y</code></p></td>
1366<td><p>float32</p></td>
1367<td><p>pix</p></td>
1368<td><p>Y position of coordinates in the brick image stack that corresponds to <code class="docutils literal">wise_coadd_id</code> (see the <a class="reference external" href="../../dr9/updates/#data-model-changes">DR9 updates page</a> for transformations between <code class="docutils literal">wise_y</code> and <code class="docutils literal">by</code>)</p></td>
1369</tr>
1370<tr>
1371<td><p><code class="docutils literal">lc_flux_w1</code></p></td>
1372<td><p>float32[25]</p></td>
1373<td><p>nanomaggy</p></td>
1374<td><p><code class="docutils literal">flux_w1</code> in each of up to twenty five unWISE coadd epochs (AB system; defaults to zero for unused entries)</p></td>
1375</tr>
1376<tr>
1377<td><p><code class="docutils literal">lc_flux_w2</code></p></td>
1378<td><p>float32[25]</p></td>
1379<td><p>nanomaggy</p></td>
1380<td><p><code class="docutils literal">flux_w2</code> in each of up to twenty five unWISE coadd epochs (AB; defaults to zero for unused entries)</p></td>
1381</tr>
1382<tr>
1383<td><p><code class="docutils literal">lc_flux_ivar_w1</code></p></td>
1384<td><p>float32[25]</p></td>
1385<td><p>1/nanomaggy²</p></td>
1386<td><p>Inverse variance of <code class="docutils literal">lc_flux_w1</code> (AB system; defaults to zero for unused entries)</p></td>
1387</tr>
1388<tr>
1389<td><p><code class="docutils literal">lc_flux_ivar_w2</code></p></td>
1390<td><p>float32[25]</p></td>
1391<td><p>1/nanomaggy²</p></td>
1392<td><p>Inverse variance of <code class="docutils literal">lc_flux_w2</code> (AB; defaults to zero for unused entries)</p></td>
1393</tr>
1394<tr>
1395<td><p><code class="docutils literal">lc_nobs_w1</code></p></td>
1396<td><p>int16[25]</p></td>
1397<td></td>
1398<td><p><code class="docutils literal">nobs_w1</code> in each of up to twenty five unWISE coadd epochs</p></td>
1399</tr>
1400<tr>
1401<td><p><code class="docutils literal">lc_nobs_w2</code></p></td>
1402<td><p>int16[25]</p></td>
1403<td></td>
1404<td><p><code class="docutils literal">nobs_w2</code> in each of up to twenty five unWISE coadd epochs</p></td>
1405</tr>
1406<tr>
1407<td><p><code class="docutils literal">lc_fracflux_w1</code></p></td>
1408<td><p>float32[25]</p></td>
1409<td></td>
1410<td><p><code class="docutils literal">fracflux_w1</code> in each of up to twenty five unWISE coadd epochs (defaults to zero for unused entries)</p></td>
1411</tr>
1412<tr>
1413<td><p><code class="docutils literal">lc_fracflux_w2</code></p></td>
1414<td><p>float32[25]</p></td>
1415<td></td>
1416<td><p><code class="docutils literal">fracflux_w2</code> in each of up to twenty five unWISE coadd epochs (defaults to zero for unused entries)</p></td>
1417</tr>
1418<tr>
1419<td><p><code class="docutils literal">lc_rchisq_w1</code></p></td>
1420<td><p>float32[25]</p></td>
1421<td></td>
1422<td><p><code class="docutils literal">rchisq_w1</code> in each of up to twenty five unWISE coadd epochs (defaults to zero for unused entries)</p></td>
1423</tr>
1424<tr>
1425<td><p><code class="docutils literal">lc_rchisq_w2</code></p></td>
1426<td><p>float32[25]</p></td>
1427<td></td>
1428<td><p><code class="docutils literal">rchisq_w2</code> in each of up to twenty five unWISE coadd epochs (defaults to zero for unused entries)</p></td>
1429</tr>
1430<tr>
1431<td><p><code class="docutils literal">lc_mjd_w1</code></p></td>
1432<td><p>float64[25]</p></td>
1433<td></td>
1434<td><p><code class="docutils literal">mjd_w1</code> in each of up to twenty five unWISE coadd epochs (defaults to zero for unused entries)</p></td>
1435</tr>
1436<tr>
1437<td><p><code class="docutils literal">lc_mjd_w2</code></p></td>
1438<td><p>float64[25]</p></td>
1439<td></td>
1440<td><p><code class="docutils literal">mjd_w2</code> in each of up to twenty five unWISE coadd epochs (defaults to zero for unused entries)</p></td>
1441</tr>
1442<tr>
1443<td><p><code class="docutils literal">lc_epoch_index_w1</code></p></td>
1444<td><p>int16[25]</p></td>
1445<td></td>
1446<td><p>Index number of unWISE epoch for W1 (defaults to -1 for unused entries)</p></td>
1447</tr>
1448<tr>
1449<td><p><code class="docutils literal">lc_epoch_index_w2</code></p></td>
1450<td><p>int16[25]</p></td>
1451<td></td>
1452<td><p>Index number of unWISE epoch for W2 (defaults to -1 for unused entries)</p></td>
1453</tr>
1454<tr>
1455<td><p><code class="docutils literal">sersic</code></p></td>
1456<td><p>float32</p></td>
1457<td></td>
1458<td><p>Power-law index for the Sersic profile model (<code class="docutils literal"><span class="pre">type="SER"</span></code>)</p></td>
1459</tr>
1460<tr>
1461<td><p><code class="docutils literal">sersic_ivar</code></p></td>
1462<td><p>float32</p></td>
1463<td></td>
1464<td><p>Inverse variance of <code class="docutils literal">sersic</code></p></td>
1465</tr>
1466<tr>
1467<td><p><code class="docutils literal">shape_r</code></p></td>
1468<td><p>float32</p></td>
1469<td><p>arcsec</p></td>
1470<td><p>Half-light radius of galaxy model for galaxy type <code class="docutils literal">type</code> (&gt;0)</p></td>
1471</tr>
1472<tr>
1473<td><p><code class="docutils literal">shape_r_ivar</code></p></td>
1474<td><p>float32</p></td>
1475<td><p>1/arcsec²</p></td>
1476<td><p>Inverse variance of <code class="docutils literal">shape_r</code></p></td>
1477</tr>
1478<tr>
1479<td><p><code class="docutils literal">shape_e1</code></p></td>
1480<td><p>float32</p></td>
1481<td></td>
1482<td><p>Ellipticity component 1 of galaxy model for galaxy type <code class="docutils literal">type</code></p></td>
1483</tr>
1484<tr>
1485<td><p><code class="docutils literal">shape_e1_ivar</code></p></td>
1486<td><p>float32</p></td>
1487<td></td>
1488<td><p>Inverse variance of <code class="docutils literal">shape_e1</code></p></td>
1489</tr>
1490<tr>
1491<td><p><code class="docutils literal">shape_e2</code></p></td>
1492<td><p>float32</p></td>
1493<td></td>
1494<td><p>Ellipticity component 2 of galaxy model for galaxy type <code class="docutils literal">type</code></p></td>
1495</tr>
1496<tr>
1497<td><p><code class="docutils literal">shape_e2_ivar</code></p></td>
1498<td><p>float32</p></td>
1499<td></td>
1500<td><p>Inverse variance of <code class="docutils literal">shape_e2</code></p></td>
1501</tr>
1502</tbody>
1503</table></section><section id="goodness-of-fits-and-morphological-type"><h2><a class="toc-backref" href="#toc-entry-2" role="doc-backlink">Goodness-of-Fits and Morphological <code class="docutils literal">type</code></a></h2>
1504<p>The <code class="docutils literal">dchisq</code> values represent the χ² sum of all pixels in the source's blob
1505for various models.  This 5-element vector contains the χ² difference between
1506the best-fit point source (type="PSF"), round exponential galaxy model ("REX"),
1507de Vaucouleurs model ("DEV"), exponential model ("EXP"), and a Sersic model ("SER"), in that order. Note that the Sersic model replaces the composite ("COMP") model used in <a class="reference external" href="../../dr8/catalogs">DR8</a> (and before).
1508The "REX" model is a round exponential galaxy profile with a variable radius
1509and is meant to capture slightly-extended but low signal-to-noise objects.
1510The <code class="docutils literal">dchisq</code> values are the χ² difference versus no source in this location---that is, it is the improvement from adding the given source to our model of the sky.  The first element (for PSF) corresponds to a traditional notion of detection significance.
1511Note that the <code class="docutils literal">dchisq</code> values are negated so that positive values indicate better fits.
1512We penalize models with negative flux in a band by subtracting rather than adding its χ² improvement in that band.</p>
1513<p>The <code class="docutils literal">rchisq</code> values are interpreted as the reduced χ² pixel-weighted by the model fit,
1514computed as the following sum over pixels in the blob for each object:</p>
1515<div class="math">
1516\begin{equation*}
1517\chi^2 = \frac{\sum \left[ \left(\mathrm{image} - \mathrm{model}\right)^2 \times \mathrm{model} \times \mathrm{inverse\, variance}\right]}{\sum \left[ \mathrm{model} \right]}
1518\end{equation*}
1519</div>
1520<p>The above sum is over all images contributing to a particular filter, and can be negative-valued for sources
1521that have a flux measured as negative in some bands where they are not detected.</p>
1522<p>The final, additional moropholigical type is "DUP." This type is set for Gaia sources that are coincident with, and so have been fit by, an extended source.
1523No optical flux is assigned to <code class="docutils literal">DUP</code> sources, but they are retained to ensure that all Gaia sources appear in the catalogs even if Tractor prefers an alternate fit.</p>
1524</section><section id="galactic-extinction-coefficients"><h2><a class="toc-backref" href="#toc-entry-3" role="doc-backlink">Galactic Extinction Coefficients</a></h2>
1525<p>The Galactic extinction values are derived from the <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/1998ApJ...500..525S/abstract">SFD98</a> maps, but with updated coefficients to
1526convert E(B-V) to the extinction in each filter.  These are reported in linear units of transmission,
1527with 1 representing a fully transparent region of the Milky Way and 0 representing a fully opaque region.
1528The value can slightly exceed unity owing to noise in the <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/1998ApJ...500..525S/abstract">SFD98</a> maps, although it is never below 0.</p>
1529<p>Eddie Schlafly has computed the extinction coefficients for the DECam filters through airmass=1.3, computed for a 7000K source spectrum as was
1530done in the Appendix of <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/2011ApJ...737..103S/abstract">Schlafly &amp; Finkbeiner (2011)</a>.
1531These coefficients are <span class="math">\(A / E(B-V)\)</span> = 3.995, 3.214, 2.165, 1.592, 1.211, 1.064
1532for the DECam <span class="math">\(u\)</span>, <span class="math">\(g\)</span>, <span class="math">\(r\)</span>, <span class="math">\(i\)</span>, <span class="math">\(z\)</span>, <span class="math">\(Y\)</span> filters,
1533respectively. Note that these are <em>slightly</em> different from the coefficients in <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/2011ApJ...737..103S/abstract">Schlafly &amp; Finkbeiner (2011)</a>.
1534The coefficients are multiplied by the <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/1998ApJ...500..525S/abstract">SFD98</a> E(B-V) values at the coordinates
1535of each object to derive the <span class="math">\(g\)</span>, <span class="math">\(r\)</span> and <span class="math">\(z\)</span> <code class="docutils literal">mw_transmission</code> values in the Legacy Surveys catalogs. The coefficients at different airmasses
1536only change by a small amount, with the largest effect in <span class="math">\(g\)</span>-band where the coefficient would be 3.219 at airmass=1 and 3.202 at airmass=2.</p>
1537<p>We calculate Galactic extinction for <a class="reference external" href="../../bass">BASS</a> and <a class="reference external" href="../../mzls">MzLS</a> as if they are on the DECam filter system.</p>
1538<p>The coefficients for the four WISE filters are derived from <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/1999PASP..111...63F/abstract">Fitzpatrick (1999)</a>, as recommended by <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/2011ApJ...737..103S/abstract">Schlafly &amp; Finkbeiner (2011)</a>,
1539considered better than either the <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/1989ApJ...345..245C/abstract">Cardelli et al. (1989)</a> curves or the newer <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/2009ApJ...699.1209F/abstract">Fitzpatrick &amp; Massa (2009)</a> NIR curve (which is not vetted beyond 2 microns).
1540These coefficients are A / E(B-V) = 0.184,  0.113, 0.0241, 0.00910.</p>
1541</section><section id="ellipticities"><h2><a class="toc-backref" href="#toc-entry-4" role="doc-backlink">Ellipticities</a></h2>
1542<p>The ellipticities for each galaxy <code class="docutils literal">type</code> (i.e. <code class="docutils literal">shape_e1</code>, <code class="docutils literal">shape_e2</code>) are different from the usual
1543eccentricity, <span class="math">\(e \equiv \sqrt{1 - (b/a)^2}\)</span>.  In gravitational lensing
1544studies, the ellipticity is taken to be a complex number:</p>
1545<div class="math">
1546\begin{equation*}
1547\epsilon = \frac{a-b}{a+b} \exp( 2i\phi ) = \epsilon_1 + i \epsilon_2
1548\end{equation*}
1549</div>
1550<p>Where ϕ is the position angle with a range of 180°, due to the
1551ellipse's symmetry. Going between <span class="math">\(r, \epsilon_1, \epsilon_2\)</span>
1552and <span class="math">\(r, b/a, \phi\)</span>:</p>
1553<div class="math">
1554\begin{align*}
1555r           &amp; = &amp; r \\
1556|\epsilon|  &amp; = &amp; \sqrt{\epsilon_1^2 + \epsilon_2^2} \\
1557\frac{b}{a} &amp; = &amp; \frac{1 - |\epsilon|}{1 + |\epsilon|} \\
1558\phi        &amp; = &amp; \frac{1}{2} \arctan \frac{\epsilon_2}{\epsilon_1} \\
1559|\epsilon|  &amp; = &amp; \frac{1 - b/a}{1 + b/a} \\
1560\epsilon_1  &amp; = &amp; |\epsilon| \cos(2 \phi) \\
1561\epsilon_2  &amp; = &amp; |\epsilon| \sin(2 \phi) \\
1562\end{align*}
1563</div>
1564<p>The angle ϕ is related to the more typical astronomical position
1565angle (<span class="math">\(PA\)</span>), measured counterclockwise from the North axis, via:</p>
1566<div class="math">
1567\begin{align*}
1568PA &amp; = &amp; (180-\phi) % \phi \\
1569\end{align*}
1570</div>
1571<div class="line-block">
1572<div class="line"><br></div>
1573</div>
1574<p><strong>Footnotes</strong></p>
1575<aside class="footnote-list brackets"><aside class="footnote brackets" id="footnote-1" role="doc-footnote"><span class="label"><span class="fn-bracket">[</span><a role="doc-backlink" href="#footnote-reference-1">1</a><span class="fn-bracket">]</span></span>
1576<p>We define a mask for the aperture fluxes using an inverse variance of zero. So, pixels with undefined ("infinite") measurement errors are not used when calculating aperture fluxes in the Tractor catalogs. As the aperture fluxes are calculated from the coadd images described on the <a class="reference external" href="../files/#image-stacks-south-coadd">files page</a>, pixels end up being ignored if they are masked in <cite>every</cite> overlapping exposure in a given band. Thus, for example, the saturated cores and bleed trails of bright stars will be masked. Further, in the case that a coadd is only built from a single image, cosmic rays and other mask bits will cause poorly measured and saturated pixels to be ignored for aperture flux measurements.</p>
1577</aside><aside class="footnote brackets" id="footnote-2" role="doc-footnote"><span class="label"><span class="fn-bracket">[</span><a role="doc-backlink" href="#footnote-reference-2">2</a><span class="fn-bracket">]</span></span>
1578<p><cite>blobmodel</cite> refers to the "blob-model" maps (i.e. the <code class="docutils literal"><span class="pre">&lt;AAA&gt;/&lt;brick&gt;/legacysurvey-&lt;brick&gt;-blobmodel-&lt;filter&gt;.fits.fz</span></code> maps described on the <a class="reference external" href="../files/#image-stacks-south-coadd">files page</a>).</p>
1579</aside><aside class="footnote brackets" id="footnote-3" role="doc-footnote"><span class="label"><span class="fn-bracket">[</span><a role="doc-backlink" href="#footnote-reference-3">3</a><span class="fn-bracket">]</span></span>
1580<p>The aperture sizes for WISE, and the rationale for including them, are detailed in <a class="reference external" href="https://github.com/legacysurvey/legacypipe/issues/447">issue #447</a>.</p>
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