J/MNRAS/446/2144ivo://CDS.VizieR/J/MNRAS/446/2144doi:10.26093/cds/vizier.74462144CDSTaylor E.N.Hopkins A.M.Baldry I.K.Bland-Hawthorn J.Brown M.J.I.,Colless M.Driver S.Norberg P.Robotham A.S.G.Alpaslan M.Brough S.,Cluver M.E.Gunawardhana M.Kelvin L.S.Liske J.Conselice C.J.,Croom S.Foster C.Jarrett T.H.Lara-Lopez M.Loveday J.2024-08-14T20:18:46Z2019-10-22T12:57:25ZCDS support team

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

cds-question@unistra.frgalaxiesstellar-massestwo-color-diagramssurveysastronomical-modelsWe measure the mass functions for generically red and blue galaxies, using a z<0.12 sample of logM_*_>8.7 field galaxies from the Galaxy And Mass Assembly (GAMA) survey. Our motivation is that, as we show, the dominant uncertainty in existing measurements stems from how "red" and "blue" galaxies have been selected/defined. Accordingly, we model our data as two naturally overlapping populations, each with their own mass function and colour-mass relation, which enables us characterize the two populations without having to specify a priori which galaxies are "red" and "blue". Our results then provide the means to derive objective operational definitions for the terms "red" and "blue", which are based on the phenomenology of the colour-mass diagrams. Informed by this descriptive modelling, we show that (1) after accounting for dust, the stellar colours of "blue" galaxies do not depend strongly on mass; (2) the tight, flat "dead sequence" does not extend much below logM_*_~10.5; instead, (3) the stellar colours of "red" galaxies vary rather strongly with mass, such that lower mass "red" galaxies have bluer stellar populations; (4) below logM_*_~9.3, the "red" population dissolves into obscurity, and it becomes problematic to talk about two distinct populations; as a consequence, (5) it is hard to meaningfully constrain the shape, including the existence of an upturn, of the "red" galaxy mass function below logM_*_~9.3. Points 1-4 provide meaningful targets for models of galaxy formation and evolution to aim for.2015MNRAS.446.2144Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/446/2144CatalogResearchIsServedByTAP VizieR generic servicerelated-toII/294 : The SDSS Photometric Catalog, Release 7J/MNRAS/413/971 : Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)J/MNRAS/452/2087 : Galaxy And Mass Assembly (GAMA): DR2 (Liske+, 2015)J/MNRAS/456/2221 : Optically red galaxies in H-ATLAS/GAMA (Dariush+, 2016)J/MNRAS/474/3875 : Galaxy And Mass Assembly (GAMA): DR3 (Baldry+, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/446/2144https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/446/2144http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/446/2144https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/446/2144https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/446/2144http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/446/2144GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/446/2144/fig8Results of our fits for the (g-i) colour-mass relations (CMRs)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM[8.725/12.175] Log mass (in dex) (logM)phys.massfloat(g-i)R[0.509614/1.19776] Rest-frame (g-i) colour for the "red" (R) population (cmrR_locus) (1)magphot.colordoublee_(g-i)R[0.001645/0.048823] Uncertainty in (g-i)R (cmrR_locus_unc)magstat.errordoubleCMRR-scat[0/0.13605] Scatter around the R CMR (cmrR_scatter)magstat.stdevdoublee_CMRR-scat[0/0.019473] Uncertainty in CMRR-scat (cmrR_scatter_unc)magstat.errordoubleCorrR[-0.865219/0.207213]? Correlation coefficient for the R population (cmrR_locus_scat_corrcoef)stat.correlationdoublenullable(g-i)B[0.32972/1.15571] Rest-frame (g-i) colour for the "blue" (B) population (cmrB_locus) (1)magphot.colordoublee_(g-i)B[0.001943/0.285534] Uncertainty in (g-i)B (cmrB_locus_unc)magstat.errordoubleCMRB-scat[2e-05/0.273328] Scatter around the B CMR (cmrB_scatter)magstat.stdevdoublee_CMRB-scat[0.000446/0.048309] Uncertainty in CMRB-scat (cmrB_scatter_unc)magstat.errordoubleCorrB[0.031897/0.818761] Correlation coefficient for the B population (cmrB_locus_scat_corrcoef)stat.correlationdoubleJ/MNRAS/446/2144/fig9Results of our fits for the (g*-i*) CMRsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM[8.725/12.175] Log mass (in dex) (logM)phys.massfloat(g-i)R[0.509614/1.19776] Rest-frame (g-i) colour for the "red" (R) population (cmrR_locus) (1)magphot.colordoublee_(g-i)R[0.001645/0.048823] Uncertainty in (g-i)R (cmrR_locus_unc)magstat.errordoubleCMRR-scat[0/0.13605] Scatter around the R CMR (cmrR_scatter)magstat.stdevdoublee_CMRR-scat[0/0.019473] Uncertainty in CMRR-scat (cmrR_scatter_unc)magstat.errordoubleCorrR[-0.865219/0.207213]? Correlation coefficient for the R population (cmrR_locus_scat_corrcoef)stat.correlationdoublenullable(g-i)B[0.32972/1.15571] Rest-frame (g-i) colour for the "blue" (B) population (cmrB_locus) (1)magphot.colordoublee_(g-i)B[0.001943/0.285534] Uncertainty in (g-i)B (cmrB_locus_unc)magstat.errordoubleCMRB-scat[2e-05/0.273328] Scatter around the B CMR (cmrB_scatter)magstat.stdevdoublee_CMRB-scat[0.000446/0.048309] Uncertainty in CMRB-scat (cmrB_scatter_unc)magstat.errordoubleCorrB[0.031897/0.818761] Correlation coefficient for the B population (cmrB_locus_scat_corrcoef)stat.correlationdoubleJ/MNRAS/446/2144/fig10Results of our fits to the (g-i) colour-mass diagrams (CMDs)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM*[8.70003/12.406] Log stellar mass (in dex) (logmstar)phys.massdoublee_logM*[0.018282/0.515653] Uncertainty in logM* (in dex) (dellogmstar)stat.errordouble(g-i)[-0.375918/2.99356]? Rest-frame (g-i) colour (only in Fig 10) (gminusi)magphot.colordoublenullablee_(g-i)[0.02154/0.532467]? Uncertainty in (g-i) (only in Fig 10) (delgminusi)magstat.errordoublenullablerhoxy[-0.496506/0.989224] Pearson correlation coefficient {rho}_xy_ (xycorrcoef) (1)stat.correlationdoubleVmax[76036.1/2.28108e+06] Maximum volume (Vmax)Mpc**3meta.bib.volumedoubleWred[0/0.986884] Red classification (Wred) (2)stat.likelihooddoubleWblue[0/0.986845] Blue classification (Wblue) (2)stat.likelihooddoublelnLi[-42.9734/4.5752] Log scalar likelihood (lnLi) (3)stat.likelihood;arith.zpdoubleJ/MNRAS/446/2144/fig11Results of our fits to the (g*-i*) CMDsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM*[8.70003/12.406] Log stellar mass (in dex) (logmstar)phys.massdoublee_logM*[0.018282/0.515653] Uncertainty in logM* (in dex) (dellogmstar)stat.errordouble(g*-i*)[-0.382121/1.4821]? Intrinsic (g*-i*) stellar colour (only in Fig 11) (gminusi_stars)magphot.colordoublenullablee_(g*-i*)[0.001227/0.098258]? Uncertainty in (g*-i*) (only in Fig 11) (delgminusi_stars)magstat.errordoublenullablerhoxy[-0.496506/0.989224] Pearson correlation coefficient {rho}_xy_ (xycorrcoef) (1)stat.correlationdoubleVmax[76036.1/2.28108e+06] Maximum volume (Vmax)Mpc**3meta.bib.volumedoubleWred[0/0.986884] Red classification (Wred) (2)stat.likelihooddoubleWblue[0/0.986845] Blue classification (Wblue) (2)stat.likelihooddoublelnLi[-42.9734/4.5752] Log scalar likelihood (lnLi) (3)stat.likelihood;arith.zpdoubleJ/MNRAS/446/2144/fig12The mass functions (MFs) for the B and R galaxy populations, as derived from our fits to the rest-frame (g-i) CMDrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM[8.725/12.175] Log mass (in dex) (logM)phys.massfloatMF[0/0.0134463] Mass function (mf)Mpc**-3phys.massdoubleMFB[0/0.011534] Mass function for the B population (mfB)Mpc**-3phys.massdoubleMFR[0/0.00353686] Mass function for the R population (mfR)Mpc**-3phys.massdoublefitMFB[9.80701e-19/0.0124547] Fit mass function for the B population (fitmfB)Mpc**-3phys.massdoublefitMFR[6.78082e-14/0.0030983] Fit mass function for the R population (fitmfR)Mpc**-3phys.massdoublefitMF[1.57981e-13/0.0146083] Fit mass function (fitmf)Mpc**-3phys.massdoublee_MF[1e-10/0.012716] Mass function 68% confidence interval, lower value (mf_m1sig)Mpc**-3stat.error;stat.mindoubleE_MF[1e-10/0.0142113] Mass function 68% confidence interval, upper value (mf_p1sig)Mpc**-3stat.error;stat.maxdoublee_MFB[1e-10/0.0109082] Mass function for the B population 68% confidence interval, lower value (mfB_m1sig)Mpc**-3stat.error;stat.mindoubleE_MFB[1e-10/0.0121684] Mass function for the B population 68% confidence interval, upper value (mfB_p1sig)Mpc**-3stat.error;stat.maxdoublee_MFR[1e-10/0.00305143] Mass function for the R population 68% confidence interval, lower value (mfR_m1sig)Mpc**-3stat.error;stat.mindoubleE_MFR[1e-10/0.00415728] Mass function for the R population 68% confidence interval, upper value (mfR_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMFB-m1[7.5207e-29/0.0120975] Fit mass function for the B population 68% confidence interval, lower value (fitmfB_m1sig)Mpc**-3stat.error;stat.mindoubleE_fitMFB-p1[3.3722e-13/0.012779] Fit mass function for the B population 68% confidence interval, upper value (fitmfB_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMFR-m1[1.83859e-14/0.00270516] Fit mass function for the R population 68% confidence interval, lower value (fitmfR_m1sig)Mpc**-3stat.error;stat.mindoubleE_fitMFR-p1[2.27661e-13/0.00354406] Fit mass function for the R population 68% confidence interval, upper value (fitmfR_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMF-m1[4.42432e-14/0.0143785] Fit mass function 68% confidence interval, lower value (fitmf_m1sig)Mpc**-3stat.error;stat.mindoubleE_fitMF-p1[5.94442e-13/0.0148499] Fit mass function 68% confidence interval, upper value (fitmf_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMFB-m3[0/0.0108847] Fit mass function for the B population 99% confidence interval, lower value (fitmfB_m3sig)Mpc**-3stat.error;stat.mindoubleE_fitMFB-p3[2.0761e-10/0.013448] Fit mass function for the B population 99% confidence interval, upper value (fitmfB_p3sig)Mpc**-3stat.error;stat.maxdoublee_fitMFR-m3[7.46471e-16/0.0023102] Fit mass function for the R population 99% confidence interval, lower value (fitmfR_m3sig)Mpc**-3stat.error;stat.mindoubleE_fitMFR-p3[2.30511e-12/0.00443756] Fit mass function for the R population 99% confidence interval, upper value (fitmfR_p3sig)Mpc**-3stat.error;stat.maxdoublee_fitMF-m3[3.91104e-15/0.0140094] Fit mass function 99% confidence interval, lower value (fitmf_m3sig)Mpc**-3stat.error;stat.mindoubleE_fitMF-p3[2.07611e-10/0.0153574] Fit mass function 99% confidence interval, upper value (fitmf_p3sig)Mpc**-3stat.error;stat.maxdoubleJ/MNRAS/446/2144/fig13The MFs for B and R galaxy populations, as derived from our fits to the intrinsic (g*-i*) CMDrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM[8.725/12.175] Log mass (in dex) (logM)phys.massfloatMF[0/0.0134463] Mass function (mf)Mpc**-3phys.massdoubleMFB[0/0.011534] Mass function for the B population (mfB)Mpc**-3phys.massdoubleMFR[0/0.00353686] Mass function for the R population (mfR)Mpc**-3phys.massdoublefitMFB[9.80701e-19/0.0124547] Fit mass function for the B population (fitmfB)Mpc**-3phys.massdoublefitMFR[6.78082e-14/0.0030983] Fit mass function for the R population (fitmfR)Mpc**-3phys.massdoublefitMF[1.57981e-13/0.0146083] Fit mass function (fitmf)Mpc**-3phys.massdoublee_MF[1e-10/0.012716] Mass function 68% confidence interval, lower value (mf_m1sig)Mpc**-3stat.error;stat.mindoubleE_MF[1e-10/0.0142113] Mass function 68% confidence interval, upper value (mf_p1sig)Mpc**-3stat.error;stat.maxdoublee_MFB[1e-10/0.0109082] Mass function for the B population 68% confidence interval, lower value (mfB_m1sig)Mpc**-3stat.error;stat.mindoubleE_MFB[1e-10/0.0121684] Mass function for the B population 68% confidence interval, upper value (mfB_p1sig)Mpc**-3stat.error;stat.maxdoublee_MFR[1e-10/0.00305143] Mass function for the R population 68% confidence interval, lower value (mfR_m1sig)Mpc**-3stat.error;stat.mindoubleE_MFR[1e-10/0.00415728] Mass function for the R population 68% confidence interval, upper value (mfR_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMFB-m1[7.5207e-29/0.0120975] Fit mass function for the B population 68% confidence interval, lower value (fitmfB_m1sig)Mpc**-3stat.error;stat.mindoubleE_fitMFB-p1[3.3722e-13/0.012779] Fit mass function for the B population 68% confidence interval, upper value (fitmfB_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMFR-m1[1.83859e-14/0.00270516] Fit mass function for the R population 68% confidence interval, lower value (fitmfR_m1sig)Mpc**-3stat.error;stat.mindoubleE_fitMFR-p1[2.27661e-13/0.00354406] Fit mass function for the R population 68% confidence interval, upper value (fitmfR_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMF-m1[4.42432e-14/0.0143785] Fit mass function 68% confidence interval, lower value (fitmf_m1sig)Mpc**-3stat.error;stat.mindoubleE_fitMF-p1[5.94442e-13/0.0148499] Fit mass function 68% confidence interval, upper value (fitmf_p1sig)Mpc**-3stat.error;stat.maxdoublee_fitMFB-m3[0/0.0108847] Fit mass function for the B population 99% confidence interval, lower value (fitmfB_m3sig)Mpc**-3stat.error;stat.mindoubleE_fitMFB-p3[2.0761e-10/0.013448] Fit mass function for the B population 99% confidence interval, upper value (fitmfB_p3sig)Mpc**-3stat.error;stat.maxdoublee_fitMFR-m3[7.46471e-16/0.0023102] Fit mass function for the R population 99% confidence interval, lower value (fitmfR_m3sig)Mpc**-3stat.error;stat.mindoubleE_fitMFR-p3[2.30511e-12/0.00443756] Fit mass function for the R population 99% confidence interval, upper value (fitmfR_p3sig)Mpc**-3stat.error;stat.maxdoublee_fitMF-m3[3.91104e-15/0.0140094] Fit mass function 99% confidence interval, lower value (fitmf_m3sig)Mpc**-3stat.error;stat.mindoubleE_fitMF-p3[2.07611e-10/0.0153574] Fit mass function 99% confidence interval, upper value (fitmf_p3sig)Mpc**-3stat.error;stat.maxdouble