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) are available here in gzipped form as zcatrev12ff2.dat.gz. It has a header line and is Topcat-compatible. There are 1026933 lines of data (EN1: 209696, EN2: 117845, Lock: 220472, VVDS: 26906, SXDS: 54209, XMM-LSS(non VVDS,SXDS): 205342, CDFS: 149766, ES1: 41757) The methodology is based on Rowan-Robinson et al 2008 (MN 386, 697), and the full revision history of the original SWIRE photometric redshift catalogue can be read in the 'readme' file in this directory. 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 (2011), (draft available in this directory as MRRphotz4.pdf) but the main features are: (i) WFC data treated as in RR08, but revised WFS data of Gonzalez-Solares et al (2011) used for EN1, EN2, Lockman. New Megacam data used for XMM-LSS. (ii) SDSS model magnitudes used, aperture corrected by forcing r-band magnitude to be same as r-WFC. (iii) 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. (iv) IRAC fluxes are aperture corrected as in Rowan-Robinson et al (2008). (v) Lockman data are from 2008 reduction, with requirement that S(3.6) > 7.5 muJy. (vi) 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. (vii) 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 1.25-8.0 mu data in the redshift solution. This improves the outlier rejection (see MRRphotz4.pdf for details). (viii) Although the redshifts have not changed greatly from the 2008 catalogue, it was necessary to rerun the infared 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 (RR and Efstathiou 2009). Format for revised SWIRE Lockman photometric redshift catalogue: write(7,136)nidir,nidopt,ra,dec, 1 s36,s45,s58,s8,s24,s70,s160,err36,err45,err58,err8,err24, 2 err70,err160,am1,am2,am3,am4,am5,em1,em2,em3,em4,em5, 3 am21,am22,am23,am25,am26,em21,em22,em23,em25,em26, 4 am6,am7,am8,em6,em7,em8,mst, 3 delmag,delmag1, 1 j1,alz,err0,j2,alz2,av1,err1, 2 n91,nbopt,amb2,alb,spectz0,nzclass0,nzref0, 3 nir,alp1,alp2,alp3,alp4,errir3, 4 alcirr,alsb,alagn,ala220,alir,nirtem, 8 als70,als160,als350,als450,als850,als1250, 1 al36,alm,sfr,almd, 5 chi2 c 136 format(i8,1x,i8,1x,f11.6,1x,f11.6,1x,14(f10.2,1x),26(f8.2,1x), 1 i4,1x,f8.3,1x,f8.3,1x,i3,1x,f7.3,1x,f10.3,1x,i3,1x,f7.3,1x, 2 f6.2,1x,d10.3,1x,i3,1x,i3,1x,f8.2,1x,f8.2,1x,f10.5,1x,2(i4,1x), 3 i3,1x,f6.2,1x,f6.2,1x,f6.2,1x,f6.2,1x,f10.3,1x, 4 5(f8.2,1x),i3,6(f6.2,1x),4(f6.2,1x),1x,85(f8.2,1x)) Explanation of magnitude fields ______________________________ field am1-5 am21-26 am6-8 N1 rev. WFC SDSS 2MASS/UKIDSS N2 rev. WFC SDSS 2MASS Lock rev. SWIRE SDSS 2MASS/UKIDSS VVDS VVDS ugri UBVRI VVDS JK SXDS Subaru Megacam - XMM SWIRE Megacam UKIDSS CDFS SWIRE - - S1 SWIRE - - \section{Catalogue description} The columns listed are: \noindent nidir(i8), infrared identifier \noindent nidopt(i8), optical identifier \noindent ra(f11.6), RA in degrees \noindent dec(f11.6), dec in degrees \noindent s36(f10.2), S(3.6$\mu$m) in $\mu$Jy (and similarly for 4.5, 5.8, 8.0 mu) \noindent s24(f10.2), S(24$\mu$m) in $\mu$Jy \noindent s70(f10.2), S(70$\mu$m) in $\mu$Jy (and similarly for 160 mu) \noindent err36, err45, err58, err8, err24, err70, err160 (7f10.2), SWIRE flux errors \noindent am1, am2, am3, am4, am4, am5 (5f8.2), UgriZ magnitudes (AB magnitudes for XMM-LSS, Vega for all the other regions) \noindent em1, em2, em3, em4, em5 (5f8.2), UgriZ magnitude errors \noindent mst (i4), stellar flag (-1 for star, 1 for galaxy, 0 indeterminate) \noindent delmag (f8.3), aperture correction in magnitudes, applied to all bands \noindent j1(i3), optical template type (1-11 galaxies, 13-30 QSOs) for $A_V$ = 0 solution [j1=13-15, 16-18, 19-21, 22-24, 25-27, 28-30, correspond to $L_tor/L_opt$ = 0, 0.2, 0.4, 0.6, 0.8, 1.] \noindent alz(f7.3), $log_{10}(1+z_{phot})$ for $A_V$ = 0 solution \noindent err0(f10.3), reduced $\chi^2$ for $A_V$ = 0 solution \noindent j2(i3), optical template type (1-11 galaxies, 13-30 QSOs) for free $A_V$ solution [j1=13-15, 16-18, 19-21, 22-24, 25-27, 28-30, correspond to $L_tor/L_opt$ = 0, 0.2, 0.4, 0.6, 0.8, 1.] \noindent alz2(f7.3), $log_{10}(1+z_{phot})$ for free $A_V$ solution \noindent av1(f6.2), $A_V$ \noindent err1(f10.3), reduced $\chi^2$ for free $A_V$ solution \noindent n91(i3), total number of photometric bands in solution \noindent nbopt(i3), number of optical bands in solution \noindent amb2(f8.2), $M_B$ (corrected for extinction) for free $A_V$ solution \noindent alb(f8.2), $log_{10} L_B$, in solar units \noindent spectz0(f10.5), spectroscopic redshift \noindent nzclass0 (i4), redshift class (VVDS) \noindent nzref0(i4), reference for spectroscopic redshift [N1,N2: nzref0 = 1-9, as in Rowan-Robinson et al 2003; = 11 Keck redshifts (Berta et al 2007), = 20 WIYN redshifts (Trichas et al 2007), = 25 GMOS redshifts (Trichas et al 2007), = 30 (Swinbank et al 2007); VVDS: nzref0 = 3-14 VVDS quality flag; Lockman: nzref0 = -1, 1 to 4 (Steffen et al 2004), = 5 NED, = 10 WIYN, Keck, Gemini redshifts (Smith et al 2007), = 11 Keck redshifts (Berta et al 2007); XMM, CDFS: nzref0 = 5 NED] \noindent nir(i3), number of bands with infrared excess \noindent alp1(f6.2), relative amplitude of cirrus component at 8 $\mu$m (s.t. alp1+alp2+alp3+alp4=1) \noindent alp2(f6.2), relative amplitude of M82 starburst component at 8 $\mu$m \noindent alp3(f6.2), relative amplitude of A220 component at 8 $\mu$m \noindent alp4(f6.2), relative amplitude of AGN dust torus component at 8 $\mu$m \noindent errir3(f10.3), reduced $\chi_{\nu}^2$ of infrared template fit \noindent alcirr(f8.2), $log_{10} L_{cirr}$ in solar units (1-1000 $\mu$m) \noindent alsb(f8.2), $log_{10} L_{M82}$ in solar units \noindent alagn(f8.2), $log_{10} L_{tor}$ in solar units \noindent al220(f8.2), $log_{10} L_{A220}$ in solar units \noindent alir(f8.2), $log_{10} L_{ir}$ in solar units \noindent nirtem(i3), ir template type (dominated by cirrus(1), M82 starburst(2), A220 starburst(3), AGN dust torus(4), single band excess(5), no excess(6) \noindent als70(f6.2), $log_{10} S70$, predicted, in mJy \noindent als160(f6.2), $log_{10} S160$, predicted, in mJy \noindent als350(f6.2), $log_{10} S350$, predicted, in mJy \noindent als450(f6.2), $log_{10} S450$, predicted, in mJy \noindent als850(f6.2), $log_{10} S850$, predicted, in mJy \noindent als1250(f6.2), $log_{10} S1250$, predicted, in mJy \noindent al36(f8.2), $log_{10} L(3.6\mu)$ in units of $L_{\odot}$ \noindent alm(f8.2) $log_{10} M_*/M_{\odot}$, stellar mass in solar units \noindent alsfr(f8.2) $log_{10} sfr$, star formation rate in $M_{\odot} yr^{-1}$ \noindent almdust(f8.2) $log_{10} M_{dust}/M_{\odot}$, dust mass in solar units \noindent chi2(85f6.2), array of reduced $\chi_{nu}^2$ as function of alz2, minimized over all templates, in bins of 0.01. Optical and infrared templates are given in directory 'templates', with a readme file. MRR 3/12/11