J/A+A/613/A67ivo://CDS.VizieR/J/A+A/613/A67doi:10.26093/cds/vizier.36130067CDSSarron F.Martinet N.Durret F.Adami C.2018-09-18T13:05:29Z2018-06-04T07:31:09ZCDS support team

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

cds-question@unistra.frgalaxy-clustersredshiftedObtaining large samples of galaxy clusters is important for cosmology: cluster counts as a function of redshift and mass can constrain the parameters of our Universe. They are also useful in order to understand the formation and evolution of clusters. We develop an improved version of the Adami & MAzure Cluster FInder (AMACFI), now the Adami, MAzure & Sarron Cluster FInder (AMASCFI), and apply it to the 154deg^2^ of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) to obtain a large catalogue of 1371 cluster candidates with mass M_200_>10^14^M{_sun}_ and redshift z<=0.7. We derive the selection function of the algorithm from the Millennium simulation, and cluster masses from a richness-mass scaling relation built from matching our candidates with X-ray detections. We study the evolution of these clusters with mass and redshift by computing the i'-band galaxy luminosity functions (GLFs) for the early-type (ETGs) and late-type galaxies (LTGs). This sample is 90% pure and 70% complete, and therefore our results are representative of a large fraction of the cluster population in these redshift and mass ranges. We find an increase in both the ETG and LTG faint populations with decreasing redshift (with Schechter slopes {sigma}_ETG_=-0.65+/-0.03 and {sigma}_LTG_=-0.95+/-0.04 at z=0.6, and {sigma}_ETG_=-0.79+/-0.02 and {sigma}_LTG_=-1.26+/-0.03 at z=0.2) and also a decrease in the LTG (but not the ETG) bright end. Our large sample allows us to break the degeneracy between mass and redshift, finding that the redshift evolution is more pronounced in high-mass clusters, but that there is no significant dependence of the faint end on mass for a given redshift. These results show that the cluster red sequence is mainly formed at redshift z>0.7, and that faint ETGs continue to enrich the red sequence through quenching of brighter LTGs at z<=0.7. The efficiency of this quenching is higher in large-mass clusters, while the accretion rate of faint LTGs is lower as the more massive clusters have already emptied most of their environment at higher redshifts.2018A&A...613A..67Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/613/A67CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/509/A81 : Candidate clusters detected in six CFHTLS fields (Adami+, 2010)J/A+A/535/A65 : Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/613/A67https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/613/A67http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/613/A67https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/613/A67https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/613/A67http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/613/A67GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/613/A67/catalog (*Candidate clusters detected using the AMASCFI algorithm in the 4 Wide fields of CFHTLS T0007)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/613/A67/catalog?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/613/A67/catalog?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/613/A67/catalog?GETtext/xml+votable180.050000true33.0468979-10.898634910.0055555555555555564/714 1104 1191 2298 2559 5/2687 2851 2854 2860-2862 2944-2945 4372-4373 4375 4420-4422 4424-4425 4758-4759 9151 9198 10230 10233 10235 6/10741-10743 10745-10747 11092-11093 11398-11399 11401-11403 11422-11423 11452 11788 11792 17497 17525 17692-17694 17705 17708-17710 17712-17714 17730 19021 19023 19025-19028 19030-19031 19047 19053 19153 19156-19157 19208 19232 19240 19242 21829 21840-21841 21843-21844 36599 36603 36747 36750 36784 36786 36798-36799 40909-40911 40926 40929 40931https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/613/A67?format=asciidefaultJ/A+A/613/A67/catalog*Candidate clusters detected using the AMASCFI algorithm in the 4 Wide fields of CFHTLS T0007recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIdClusCluster Identification in the catalogmeta.id;meta.tablecharRAJ2000Cluster right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Cluster declination (J2000)degpos.eq.dec;meta.mainzclusCluster redshiftsrc.redshift;pos.heliocentricfloatS/NCluster signal-to-noise ratiostat.snrfloatR-AMASCFI? Cluster richness (as computed by AMASCFI, see paper for details)src.class.richnessfloatnullablee_R-AMASCFI? Error on cluster richness (as computed by AMASCFI)stat.errorfloatnullableM200? Median M200, mass contained in a radius r200, inside which the density is 200 times the critical density of the Universe (1)phys.mass;stat.mediandoublenullablee_M200? 68% lower confidence limit on M200 (1)stat.error;stat.mindoublenullableE_M200? 68% upper confidence limit on M200 (1)stat.error;stat.maxdoublenullable