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dc.contributor.authorHennig, C.pt_BR
dc.contributor.authorMohr, Joseph J.pt_BR
dc.contributor.authorZenteno, Alfredopt_BR
dc.contributor.authorDesai, S.pt_BR
dc.contributor.authorDietrich, Jörg P.pt_BR
dc.contributor.authorBocquet, Sebastianpt_BR
dc.contributor.authorStrazzullo, Veronicapt_BR
dc.contributor.authorSaro, Alexandropt_BR
dc.contributor.authorAbbott, Timothy M. C.pt_BR
dc.contributor.authorAbdalla, Filipe B.pt_BR
dc.contributor.authorBayliss, Matthew B.pt_BR
dc.contributor.authorBenoit-Lévy, Aurélienpt_BR
dc.contributor.authorBernstein, Gary M.pt_BR
dc.contributor.authorBertin, Emmanuelpt_BR
dc.contributor.authorBrooks, D.pt_BR
dc.contributor.authorCapasso, Raffaellapt_BR
dc.contributor.authorCapozzi, Diegopt_BR
dc.contributor.authorCarnero Rosell, Aureliopt_BR
dc.contributor.authorCarrasco Kind, Matíaspt_BR
dc.contributor.authorCarretero Palacios, Jorgept_BR
dc.contributor.authorChiu, I. Non Timpt_BR
dc.contributor.authorD'Andrea, Christopher B.pt_BR
dc.contributor.authorCosta, Luiz N. dapt_BR
dc.contributor.authorDiehl, H. Thomaspt_BR
dc.contributor.authorDoel, Peterpt_BR
dc.contributor.authorEifler, Timpt_BR
dc.contributor.authorEvrard, August E.pt_BR
dc.contributor.authorFausti Neto, Angelopt_BR
dc.contributor.authorFosalba Vela, Pablopt_BR
dc.contributor.authorFrieman, Joshua A.pt_BR
dc.contributor.authorGangkofner, C.pt_BR
dc.contributor.authorGonzalez, Anthonypt_BR
dc.contributor.authorGruen, Danielpt_BR
dc.contributor.authorGruendl, Robert A.pt_BR
dc.contributor.authorGupta, Nayantarapt_BR
dc.contributor.authorGutierrez, Gaston R.pt_BR
dc.contributor.authorHonscheid, K.pt_BR
dc.contributor.authorHlavacek-Larrondo, Juliept_BR
dc.contributor.authorJames, David J.pt_BR
dc.contributor.authorKuehn, Kylerpt_BR
dc.contributor.authorKuropatkin, Nikolay P.pt_BR
dc.contributor.authorLahav, Oferpt_BR
dc.contributor.authorMarch, Marisa Cristinapt_BR
dc.contributor.authorMarshall, Jennifer L.pt_BR
dc.contributor.authorMartini, Paulpt_BR
dc.contributor.authorMcDonald, Michael Kennethpt_BR
dc.contributor.authorMelchior, Peter M.pt_BR
dc.contributor.authorMiller, Christopher J.pt_BR
dc.contributor.authorMiquel, Ramonpt_BR
dc.contributor.authorNeilsen, Eric H.pt_BR
dc.contributor.authorNord, Brian Dennispt_BR
dc.contributor.authorOgando, Ricardo L.C.pt_BR
dc.contributor.authorPlazas Malagón, Andrés Alejandropt_BR
dc.contributor.authorReichardt, Christian L.pt_BR
dc.contributor.authorRomer, Anita K.pt_BR
dc.contributor.authorRozo, Eduardopt_BR
dc.contributor.authorRykoff, Elipt_BR
dc.contributor.authorSanchez-Alvaro, Eusebiopt_BR
dc.contributor.authorSantiago, Basilio Xavierpt_BR
dc.contributor.authorSchubnell, Michaelpt_BR
dc.contributor.authorSevilla Noarbe, Ignaciopt_BR
dc.contributor.authorSmith, Robert Christopherpt_BR
dc.contributor.authorSoares-Santos, Marcellept_BR
dc.contributor.authorSobreira, Fláviapt_BR
dc.contributor.authorStalder, Brianpt_BR
dc.contributor.authorStanford, Spencer Adampt_BR
dc.contributor.authorSuchyta, Ericpt_BR
dc.contributor.authorSwanson, Molly E. C.pt_BR
dc.contributor.authorTarle, Gregorypt_BR
dc.contributor.authorThomas, D.pt_BR
dc.contributor.authorVikram, Vinupt_BR
dc.contributor.authorWalker, Alistairpt_BR
dc.contributor.authorZhang, Yuanyuanpt_BR
dc.date.accessioned2017-06-20T02:33:11Zpt_BR
dc.date.issued2017pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/159774pt_BR
dc.description.abstractWe study the galaxy populations in 74 Sunyaev–Zeldovich effect selected clusters from the South Pole Telescope survey, which have been imaged in the science verification phase of the Dark Energy Survey. The sample extends up to z ∼ 1.1 with 4 × 1014M ≤ M200 ≤ 3 × 1015M . Using the band containing the 4000 Å break and its redward neighbour, we study the colour–magnitude distributions of cluster galaxies to ∼m∗ + 2, finding that: (1)The intrinsic rest frame g − r colour width of the red sequence (RS) population is ∼0.03 out to z ∼ 0.85 with a preference for an increase to ∼0.07 at z = 1, and (2) the prominence of the RS declines beyond z ∼ 0.6. The spatial distribution of cluster galaxies is well described by the NFW profile out to 4R200 with a concentration of cg = 3.59+0.20 −0.18, 5.37+0.27 −0.24 and 1.38+0.21 −0.19 for the full, the RS and the blue non-RS populations, respectively, but with ∼40 per cent to 55 per cent cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region N200 exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The RS fraction within R200 is (68 ± 3) per cent at z = 0.46, varies from ∼55 per cent at z = 1 to ∼80 per cent at z = 0.1 and exhibits intrinsic variation among clusters of ∼14 per cent. We discuss a model that suggests that the observed redshift trend in RS fraction favours a transformation time-scale for infalling field galaxies to become RS galaxies of 2–3 Gyr.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the Royal Astronomical Society. Oxford. Vol. 467, no. 4 (June 2017), p. 4015–4035pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxies clusters generalen
dc.subjectGaláxias ativaspt_BR
dc.subjectGalaxies clusters individualen
dc.subjectAglomerados globularespt_BR
dc.subjectGalaxies evolutionen
dc.subjectPopulacoes estelarespt_BR
dc.subjectGalaxies formationen
dc.subjectGalaxies luminosity functionen
dc.subjectGalaxies mass functionen
dc.titleGalaxy populations in massive galaxy clusters to z = 1.1 : colour distribution, concentration, halo occupation number and red sequence fractionpt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001022162pt_BR
dc.type.originEstrangeiropt_BR


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