J/A+A/562/A86ivo://CDS.VizieR/J/A+A/562/A86doi:10.26093/cds/vizier.35620086CDSJouvel S.Host O.Lahav O.Seitz S.Molino A.Coe D.Postman M.,Moustakas L.Benitez N.Rosati P.Balestra I.Grillo C.Bradley L.,Fritz A.Kelson D.Koekemoer A.M.Lemze D.Medezinski E.Mercurio A.,Moustakas J.Nonino M.Scodeggio M.Zheng W.Zitrin A.Bartelmann M.,Bouwens R.Broadhurst T.Donahue M.Ford H.Graves G.Infante L.,Jimenez-Teja Y.Lazkoz R.Melchior P.Meneghetti M.Merten J.Ogaz S.,Umetsu K.2017-07-06T06:25:57Z2014-02-11T08:14:00ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesphotometryredshiftedhst-photometryThe Cluster Lensing And Supernovae survey with Hubble (CLASH) is a Hubble Space Telescope (HST) Multi-Cycle Treasury programme that observes 25 massive galaxy clusters, 20 of which were X-ray-selected to preferably choose dynamically relaxed clusters, and 5 additional "high magnification" clusters, which were selected based on their optical lensing properties. CLASH aims to study the dark matter distribution of the clusters and find magnified high-redshift galaxies behind them. CLASH observations were carried out in 16 bands from UV to NIR to derive accurate and reliable estimates of photometric redshifts. We present the CLASH photometric redshifts using 16 HST bands and study the photometric redshift accuracy including a detailed comparison between photometric and spectroscopic redshifts for the strong lensing arcs using the measurements from the cluster MACSJ1206.2-0847.2014A&A...562A..86Jhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/562/A86CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/hst : HST Archived Exposures Catalog (STScI, 2007)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/562/A86https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/562/A86http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/562/A86https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/562/A86https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/562/A86http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/562/A86GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/562/A86/macs1206 (The MACS1206 photometric redshift catalogue)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/562/A86/macs1206?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/562/A86/macs1206?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/562/A86/macs1206?GETtext/xml+votable180.050000true181.53667-8.76174440.0055555555555555566/254511.0590977079788917e-19 7.605786964834612e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/562/A86?format=asciiOpticaldefaultJ/A+A/562/A86/macs1206The MACS1206 photometric redshift cataloguee_FF814W? F814W isophotal flux uncertainty (1.111 factor applied here as well) (f814w_fluxerr)stat.errorfloatnullablef_FF814W[i] i when error is infinitymeta.codecharF814WsF814W detection significance (f814w_sig)stat.fit.goodnessfloatF850LP?=-99 F850LP isophotal magnitude (ZP=24.8425) (f850lp_mag)magphot.mag;em.opt.Idoublenullablee_F850LP?=0 F850LP isophotal (edges vulnerable to cosmic rays) (f850lp_magerr)magstat.errordoublenullableFF850LP?=0 F850LP isophotal flux (multiplied by 1.089 to correct for extinction (-0.093mag)) (f850lp_flux)phot.mag;em.opt.Idoublenullablee_FF850LP? F850LP isophotal flux uncertainty (1.089 factor applied here as well) (f850lp_fluxerr)stat.errorfloatnullablef_FF850LP[i] i when error is infinitymeta.codecharF850LPsF850LP detection significance (f850lp_sig)stat.fit.goodnessfloatF105W?=-99 F105W isophotal magnitude (ZP=26.2707) (f105w_mag)magphot.mag;em.IR.Jdoublenullablee_F105W?=0 F105W uncertainty (f105w_magerr)magstat.errorfloatnullableFF105W?=0 F105W isophotal flux (multiplied by 1.060 to correct for extinction (-0.064mag)) (f105w_flux)phot.mag;em.IR.Jdoublenullablee_FF105W? F105W isophotal flux uncertainty (1.060 factor applied here as well) (f105w_fluxerr)stat.errorfloatnullablef_FF105W[i] i when error is infinitymeta.codecharF105WsF105W detection significance (f105w_sig)stat.fit.goodnessfloatF110W?=-99 F110W isophotal magnitude (ZP=26.8251) (f110w_mag)magphot.mag;em.IR.Jdoublenullablee_F110W?=0 F110W uncertainty (f110w_magerr)magstat.errordoublenullableFF110W?=0 F110W isophotal flux (multiplied by 1.052 to correct for extinction (-0.055mag)) (f110w_flux)phot.mag;em.IR.Jdoublenullablee_FF110W? F110W isophotal flux uncertainty (1.052 factor applied here as well) (f110w_fluxerr)stat.errorfloatnullablef_FF110W[i] i when error is infinitymeta.codecharF110WsF110W detection significance (f110w_sig)stat.fit.goodnessfloatF125W?=-99 F125W isophotal magnitude (ZP=26.2474) (f125w_mag)magphot.mag;em.IR.Jdoublenullablee_F125W?=0 F125W uncertainty (f125w_magerr)magstat.errordoublenullableFF125W?=0 F125W isophotal flux (multiplied by 1.045 to correct for extinction (-0.048mag)) (f125w_flux)phot.mag;em.IR.Jdoublenullablee_FF125W? F125W isophotal flux uncertainty (1.045 factor applied here as well) (f125w_fluxerr)stat.errorfloatnullablef_FF125W[i] i when error is infinitymeta.codecharF125WsF125W detection significance (f125w_sig)stat.fit.goodnessfloatF140W?=-99 F140W isophotal magnitude (ZP=26.4645) (f140w_mag)magphot.mag;em.IR.Hdoublenullablee_F140W?=0 F140W uncertainty (f140w_magerr)magstat.errordoublenullableFF140W?=0 F140W isophotal flux (multiplied by 1.036 to correct for extinction (-0.038mag)) (f140w_flux)phot.mag;em.IR.Hdoublenullablee_FF140W? F140W isophotal flux uncertainty (1.036 factor applied here as well) (f140w_fluxerr)stat.errorfloatnullablef_FF140W[i] i when error is infinitymeta.codecharF160W?=-99 F160W isophotal magnitude (ZP=25.9559) (f160w_mag)magphot.mag;em.IR.Hdoublenullablee_F160W?=0 F160W uncertainty (f160w_magerr)magstat.errordoublenullableFF160W?=0 F160W isophotal flux (multiplied by 1.028 to correct for extinction (-0.030mag)) (f160w_flux)phot.mag;em.IR.Hdoublenullablee_FF160W? F160W isophotal flux uncertainty (1.028 factor applied here as well) (f160w_fluxerr)stat.errorfloatnullablef_FF160W[i] i when error is infinitymeta.codecharF160WsF160W detection significance (f160w_sig)stat.fit.goodnessfloatzb[0.01/9.99] BPZ most likely redshiftsrc.redshift.photfloatb_zbLower limit (95% confidence) (zbmin)stat.fit.paramfloatB_zbUpper limit (95% confidence) (zbmax)stat.fit.paramfloattb[1/11] BPZ most likely T typemeta.notefloatodds[0/1] P(z) contained within zb+/-2*0.02*(1+z)stat.fit.goodnessfloatchisqPoorness of BPZ fit: observed vs. model fluxesstat.fit.chi2floatchisq2Modified chisq: model fluxes given error barsstat.fit.chi2doubleM0? Magnitude used as a priormagphot.mag;meta.modelleddoublenullablezml[0.01/9.99] Maximum Likelihood redshiftsrc.redshift.photfloattml[1/11] Maximum Likelihood most likely T typemeta.notefloatzlpLe Phare most likely redshift (Z_BEST)src.redshift.photfloatb_zlpLower limit (68% confidence) (Z_BEST68_LOW)stat.fit.paramfloatB_zlpUpper limit (68% confidence) (Z_BEST68_HIGH)stat.fit.paramfloatzMLLe Phare maximum likelihood redshift (Z_ML)src.redshift.photfloatb_zMLLower limit (90% confidence) (Z_BEST90_LOW)stat.fit.paramfloatB_zMLUpper limit (90% confidence) (Z_BEST90_HIGH)stat.fit.paramfloatb_z95Lower limit (95% confidence) (Z_BEST95_LOW)stat.fit.paramfloatB_z95Upper limit (95% confidence) (Z_BEST95_HIGH)stat.fit.paramfloatchilpPoorness of Le Phare fit: observed vs. model fluxes (CHI_BEST)stat.fit.chi2floattlp[1/31] Le Phare most likely T type (MOD_BEST)meta.noteintEBVlpLe Phare most likely extinction (EBV_BEST)magphys.absorptionfloatMAGlp[-26/-10] Le Phare absolute magnitude in F814W (MAG_ABS_BEST)magphys.magAbsfloatoddlp[1/101] P(z) contained within zlp+/-0.05 (PDZ_BEST)%stat.fit.goodnessfloatzlp2?=-99 Le Phare second redshift solution (if any) (Z_SEC)src.redshift.photfloatnullablechilp2?=0.1e+10 Poorness of the second solution (CHI_SEC)stat.fit.chi2floatnullabletlp2[1/31]?=-999 Le Phare second spectral type solution (MOD_SEC)src.spTypeintnullablee_F775W?=0 F775W uncertainty (edges vulnerable to cosmic rays) (f775w_magerr)magstat.errordoublenullableID[6/6712] Object ID Numbermeta.id;meta.mainintprimaryRAJ2000Right Ascension in decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Declination in decimal degrees (J2000)degpos.eq.dec;meta.mainFWHMFull width at half maximum (arcsec)arcsecspect.line.widthfloatAreaIsophotal aperture area (pixels)pixphys.area;instrintS/GSExtractor "stellarity" (1=star; 0=galaxy)src.class.starGalaxyfloatellEllipticity = 1-b/asrc.ellipticityfloatf5s[0/2] 0 = probably real; 1 = probable CR; 2 = no 5-{sigma} detection (flag5sig)meta.codeintn5s[1/16] Number of filters with a 5-{sigma} detection (nf5sig)meta.numberintn5cr[0/11] Number of CR-vulnerable filters with a 5-{sigma} detection (nfcr5sig)meta.numberintnf[2/16] Number of filters observed (not in chip gap, etc.) (nfobs)meta.numberintF225W?=-99 F225W isophotal magnitude (ZP=24.0966) (f225w_mag)magphot.mag;em.UV.200-300nmdoublenullablee_F225W?=0 F225W uncertainty (edges vulnerable to cosmic rays) (f225w_magerr)magstat.errorfloatnullableFF225W?=0 F225W isophotal flux (multiplied by 1.541 to correct for extinction (-0.470mag)) (f225w_flux)phot.mag;em.UV.200-300nmdoublenullablee_FF225W? F225W isophotal flux uncertainty (1.541 factor applied here as well) (f225w_fluxerr)stat.errorfloatnullablef_FF225W[i] i when error is infinitymeta.codecharF225WsF225W detection significance (f225w_sig)stat.fit.goodnessfloatF275W?=-99 F275W isophotal magnitude (ZP=24.1742) (f275w_mag)magphot.mag;em.UV.200-300nmdoublenullablee_F275W?=0 F275W uncertainty (edges vulnerable to cosmic rays) (f275w_magerr)magstat.errorfloatnullableFF275WF275W isophotal flux (multiplied by 1.427 to correct for extinction (-0.386mag)) (f275w_flux)phot.mag;em.UV.200-300nmdoublee_FF275W? F275W isophotal flux uncertainty (1.427 factor applied here as well) (f275w_fluxerr)stat.errorfloatnullablef_FF275W[i] i when error is infinitymeta.codecharF275WsF275W detection significance (f275w_sig)stat.fit.goodnessfloatF336W?=-99 F336W isophotal magnitude (ZP=24.6453) (f336w_mag)magphot.mag;em.opt.Udoublenullablee_F336W?=0 F336W uncertainty (edges vulnerable to cosmic rays) (f336w_magerr)magstat.errordoublenullableF140WsF140W detection significance (f140w_sig)stat.fit.goodnessfloatFF336W?=0 F336W isophotal flux (multiplied by 1.343 to correct for extinction (-0.320mag)) (f336w_flux)phot.mag;em.opt.Udoublenullablee_FF336W? F336W isophotal flux uncertainty (1.343 factor applied here as well) (f336w_fluxerr)stat.errorfloatnullablef_FF336W[i] i when error is infinitymeta.codecharF336WsF336W detection significance (f336w_sig)stat.fit.goodnessfloatF390W?=-99 F390W isophotal magnitude (ZP=25.3714) (f390w_mag)magphot.mag;em.opt.Bdoublenullablee_F390W?=0 F390W uncertainty (edges vulnerable to cosmic rays) (f390w_magerr)magstat.errorfloatnullableFF390WF390W isophotal flux (multiplied by 1.299 to correct for extinction (-0.284mag)) (f390w_flux)phot.mag;em.opt.Bdoublee_FF390W? F390W isophotal flux uncertainty (1.299 factor applied here as well) (f390w_fluxerr)stat.errorfloatnullablef_FF390W[i] i when error is infinitymeta.codecharF390WsF390W detection significance (f390w_sig)stat.fit.goodnessfloatF435W?=-99 F435W isophotal magnitude (ZP=25.6578) (f435w_mag)magphot.mag;em.opt.Bdoublenullablee_F435W?=0 F435W isophotal (edges vulnerable to cosmic rays) (f435w_magerr)magstat.errorfloatnullableFF435W?=0 F435W isophotal flux (multiplied by 1.269 to correct for extinction (-0.259mag)) (f435w_flux)phot.mag;em.opt.Bdoublenullablee_FF435W? F435W isophotal flux uncertainty (1.269 factor applied here as well) (f435w_fluxerr)stat.errorfloatnullablef_FF435W[i] i when error is infinitymeta.codecharF435WsF435W detection significance (f435w_sig)stat.fit.goodnessfloatF475W?=-99 F475W isophotal magnitude (ZP=26.0593) (f475w_mag)magphot.mag;em.opt.Bdoublenullablee_F475W?=0 F475W uncertainty (edges vulnerable to cosmic rays) (f475w_magerr)magstat.errorfloatnullableFF475W?=0 F475W isophotal flux (multiplied by 1.241 to correct for extinction (-0.234mag)) (f475w_flux)phot.mag;em.opt.Bdoublenullablee_FF475W? F475W isophotal flux uncertainty (1.241 factor applied here as well) (f475w_fluxerr)stat.errorfloatnullablef_FF475W[i] i when error is infinitymeta.codecharF475WsF475W detection significance (f475w_sig)stat.fit.goodnessfloatF606W?=-99 F606W isophotal magnitude (ZP=26.5052) (f606w_mag)magphot.mag;em.opt.Rdoublenullablee_F606W?=0 F606W uncertainty (edges vulnerable to cosmic rays) (f606w_magerr)magstat.errordoublenullableFF606WF606W isophotal flux (multiplied by 1.185 to correct for extinction (-0.184mag)) (f606w_flux)phot.mag;em.opt.Rdoublee_FF606W? F606W isophotal flux uncertainty (1.185 factor applied here as well) (f606w_fluxerr)stat.errorfloatnullablef_FF606W[i] i when error is infinitymeta.codecharF606WsF606W detection significance (f606w_sig)stat.fit.goodnessfloatF625W?=-99 F625W isophotal magnitude (ZP=25.9067) (f625w_mag)magphot.mag;em.opt.Rdoublenullablee_F625W?=0 F625W uncertainty (edges vulnerable to cosmic rays) (f625w_magerr)magstat.errordoublenullableFF625W?=0 F625W isophotal flux (multiplied by 1.167 to correct for extinction (-0.168mag)) (f625w_flux)phot.mag;em.opt.Rdoublenullablee_FF625W? F625W isophotal flux uncertainty (1.167 factor applied here as well) (f625w_fluxerr)stat.errorfloatnullablef_FF625W[i] i when error is infinitymeta.codecharF625WsF625W detection significance (f625w_sig)stat.fit.goodnessfloatF775W?=-99 F775W isophotal magnitude (ZP=25.6651) (f775w_mag)magphot.mag;em.opt.IdoublenullableFF775W?=0 F775W isophotal flux (multiplied by 1.124 to correct for extinction (-0.127mag)) (f775w_flux)phot.mag;em.opt.Idoublenullablee_FF775W? F775W isophotal flux uncertainty (1.124 factor applied here as well) (f775w_fluxerr)stat.errorfloatnullablef_FF775W[i] i when error is infinitymeta.codecharF775WsF775W detection significance (f775w_sig)stat.fit.goodnessfloatF814W?=-99 F814W isophotal magnitude (ZP=25.9433) (f814w_mag)magphot.mag;em.opt.Idoublenullablee_F814W?=0 F814W uncertainty (edges vulnerable to cosmic rays) (f814w_magerr)magstat.errordoublenullableFF814W?=0 F814W isophotal flux (multiplied by 1.111 to correct for extinction (-0.115mag)) (f814w_flux)phot.mag;em.opt.Idoublenullable