Galaxy Populations in Massive Galaxy Clusters to z=1.1: Color Distribution, Concentration, Halo Occupation Number and Red Sequence Fraction
Creators: name: Hennig, C.
name: Mohr, J. J.
name: Zenteno, A.
name: Desai, S.
name: Dietrich, J. P.
name: Bocquet, S.
name: Strazzullo, V.
name: Saro, A.
name: Abbott, T. M. C.
name: Abdalla, F. B.
name: Bayliss, M.
name: Benoit-Levy, A.
name: Bernstein, R. A.
name: Bertin, E.
name: Brooks, D.
name: Capasso, R.
name: Capozzi, D.
name: Carnero, A.
name: Kind, M. Carrasco
name: Carretero, J.
name: Chiu, I.
name: D'Andrea, C. B.
name: daCosta, L. N.
name: Diehl, H. T.
name: Doel, P.
name: Eifler, T. F.
name: Evrard, A. E.
name: Fausti-Neto, A.
name: Fosalba, P.
name: Frieman, J.
name: Gangkofner, C.
name: Gonzalez, A.
name: Gruen, D.
name: Gruendl, R. A.
name: Gupta, N.
name: Gutierrez, G.
name: Honscheid, K.
name: Hlavacek-Larrondo, J.
name: James, D. J.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lahav, O.
name: March, M.
name: Marshall, J. L.
name: Martini, P.
name: McDonald, M.
name: Melchior, P.
name: Miller, C. J.
name: Miquel, R.
name: Neilsen, E.
name: Nord, B.
name: Ogando, R.
name: Plazas, A. A.
name: Reichardt, C.
name: Romer, A. K.
name: Rozo, E.
name: Rykoff, E. S.
name: Sanchez, E.
name: Santiago, B.
name: Schubnell, M.
name: Sevilla-Noarbe, I.
name: Smith, R. C.
name: Soares-Santos, M.
name: Sobreira, F.
name: Stalder, B.
name: Stanford, S. A.
name: Suchyta, E.
name: Swanson, M. E. C.
name: Tarle, G.
name: Thomas, D.
name: Vikram, V.
name: Walker, A. R.
name: Zhang, Y.
Publisher: name: arXiv
Year: 2016
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We study the galaxy populations in 74 Sunyaev Zeldovich Effect (SZE) selected clusters from the South Pole Telescope (SPT) survey that have been imaged in the science verification phase of the Dark Energy Survey (DES). The sample extends up to $z\sim 1.1$ with $4 \times 10^{14} M_{\odot}\le M_{200}\le 3\times 10^{15} M_{\odot}$. Using the band containing the 4000~Å break and its redward neighbor, we study the color-magnitude distributions of cluster galaxies to $\sim m_*+2$, finding: (1) the intrinsic rest frame $g-r$ color width of the red sequence (RS) population is $\sim$0.03 out to $z\sim0.85$ with a preference for an increase to $\sim0.07$ at $z=1$ and (2) the prominence of the RS declines beyond $z\sim0.6$. The spatial distribution of cluster galaxies is well described by the NFW profile out to $4R_{200}$ with a concentration of $c_{\mathrm{g}} = 3.59^{+0.20}_{-0.18}$, $5.37^{+0.27}_{-0.24}$ and $1.38^{+0.21}_{-0.19}$ for the full, the RS and the blue non-RS populations, respectively, but with $\sim40$\% to 55\% cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region $N_{200}$ 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 red sequence (RS) fraction within $R_{200}$ is $(68\pm3)$\% at $z=0.46$, varies from $\sim$55\% at $z=1$ to $\sim$80\% at $z=0.1$, and exhibits intrinsic variation among clusters of $\sim14$\%. We discuss a model that suggests the observed redshift trend in RS fraction favors a transformation timescale for infalling field galaxies to become RS galaxies of 2 to 3~Gyr.
description: 22 pages, 14 figures, submitted to MNRAS