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II/326 Revised SWIRE photometric redshifts (Rowan-Robinson+, 2013)
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zcatrev.dat
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Beginning of ReadMe :II/326 Revised SWIRE photometric redshifts (Rowan-Robinson+, 2013)
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Revised SWIRE photometric redshifts.
Rowan-Robinson M., Gonzalez-Solares E., Vaccari M., Marchetti L.
<Mon. Not. R. Astron. Soc., 428, 1958-1967 (2013)>
=2013MNRAS.428.1958R
=2013yCat.2336....0R
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ADC_Keywords: Surveys ; Galaxies, IR ; Galaxies, photometry ; Redshifts
Keywords: galaxies: evolution - galaxies: starburst - galaxies: star formation -
cosmology: observations - infrared: galaxies
Abstract:
We have revised the Spitzer Wide-Area Infrared Extragalactic survey
(SWIRE) Photometric Redshift Catalogue to take account of new optical
photometry in several of the SWIRE areas, and incorporating Two Micron
All Sky Survey (2MASS) and UKIRT Infrared Deep Sky Survey (UKIDSS)
near-infrared data. Aperture matching is an important issue for
combining near-infrared and optical data, and we have explored a
number of methods of doing this. The increased number of photometric
bands available for the redshift solution results in improvements both
in the rms error and, especially, in the outlier rate.
We have also found that incorporating the dust torus emission into the
quasi-stellar object (QSO) templates improves the performance for QSO
redshift estimation. Our revised redshift catalogue contains over 1
million extragalactic objects, of which 26 288 are QSOs.
Description:
The revised SWIRE photometric redshift catalogues for the Lockman,
EN1, EN2 and XMM-LSS areas (plus original catalogues for ES1, CDFS,
VVDS and SXDS areas). (version zcatrev12ff4.dat.gz, 2016)
There are 1160613 lines of data (EN1: 209696, EN2: 117845,
Lock: 220472, XMM-LSS (including VVDS and SXDS): 317136,
ES1: 145698, CDFS: 149766).
The methodology is based on Rowan-Robinson et al.
(2008MNRAS.386..697R).
Since publication of Rowan-Robinson et al (2008MNRAS.386..697R) I have
reprocessed the XMM-LSS and and ES1 areas using new photometric data
collected in the Mattia et al. fusion catalogues
(http://www.mattiavaccari.net/df/ ).
XMM benefited from the CFHTLS-T0007 data release and ES1 from the
substantially expanded ESIS BVR Final Data Release.
The number of SWIRE photometric redshifts has increased by 15%. The
quality of the XMM redshifts is significantly improved. The absence of
u-band photometry in ES1 and CDFS means these redshifts are of lower
reliability.
The main change here is the incorporation of SDSS and UKIDSS data into
the solution.
The details of how this was done will be reported in Rowan-Robinson et
al. (2013MNRAS.428.1958R) but the main features are:
(1) WFC data treated as in RR08 (Cat. II/290), but revised WFS data
of Gonzalez-Solares et al. (2011MNRAS.416..927G) used for
EN1, EN2, Lockman. New Megacam data used for XMM-LSS.
(2) SDSS model magnitudes used, aperture corrected by forcing r-band
magnitude to be same as r-WFC.
(3) 2MASS point-source magnitudes used if available, aperture
corrected by using a multiple (0.8) of the WFC r-band
aperture correction. If not, UKIDSS point-source magnitudes
used, aperture corrected by using a multiple (1.1) of the
WFC r-band aperture correction.
(4) IRAC fluxes are aperture corrected as in Rowan-Robinson et al.
(2008MNRAS.386..697R).
(5) Lockman data are from 2008 reduction, with requirement that
S(3.6)>7.5muJy.
(6) SXDS sources with new Megacam data are reanalyzed using
Subaru+Megacam data (40553 sources).
The remainder (13655 sources) are from the 2008 reduction.
New spectroscopic redshifts from Chris Simpson (2012 in prep)
are incorporated.
(7) For quasars we have added AGN dust torus templates to our 3 QSO
templates, with amplitudes corresponding to
L_tor_/L_opt_ = 0, 0.2, 0.4, 0.6, 0.8, 1.0, and used 1.25-8.0mum
data in the redshift solution. This improves the outlier rejection
(see the paper for details).
(8) Although the redshifts have not changed greatly from the 2008
catalogue, it was necessary to rerun the infrared template
fitting in order to register the correct infrared luminosity,
ir sed type and derived quantities like star formation rate,
dust mass and stellar mass. It is planned to refine the template
fitting to take into account the lessons of the IRS line
diagnostics (Rowan-Robinson and Efstathiou, 2009MNRAS.399..615R).