THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS

By S. Hansen, Erin Sheldon, Risa Wechsler, Benjamin P. Koester. 2007

194 citations recorded by the source corpus.

Imaging data from the Sloan Digital Sky Survey are used to characterize the population of galaxies in groups and clusters detected with the MaxBCG algorithm. We investigate the dependence of brightest cluster galaxy (BCG) luminosity, and the distributions of satellite galaxy luminosity and satellite color, on cluster properties over the redshift range 0.1 ⩽ z ⩽ 0.3. The size of the data set allows us to make measurements in many bins of cluster richness, radius and redshift. We find that, within r200 of clusters with mass above 3 × 1013h−1M☉, the luminosity function (LF) of both red and blue satellites is only weakly dependent on richness. We further find that the shape of the satellite LF does not depend on cluster-centric distance for magnitudes brighter than 0.25Mi − 5log10h =−19. However, the mix of faint red and blue galaxies changes dramatically. The satellite red fraction is dependent on cluster-centric distance, galaxy luminosity, and cluster mass, and also increases by ∼5% between redshifts 0.28 and 0.2, independent of richness. We find that BCG luminosity is tightly correlated with cluster richness, scaling as LBCG ∼ M0.3200, and has a Gaussian distribution at fixed richness, with σlogL ∼ 0.17 for massive clusters. The ratios of BCG luminosity to total cluster luminosity and characteristic satellite luminosity scale strongly with cluster richness: in richer systems, BCGs contribute a smaller fraction of the total light, but are brighter compared to typical satellites. This study demonstrates the power of cross-correlation techniques for measuring galaxy populations in purely photometric data.

Subfields: Astronomy and Astrophysics, Ecology, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/0f362e08116a63f1f56f48d0694980abbc8f0d51

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Citations in the corpus

Dependence of galaxy quenching on halo mass and distance from its centre (2012, result): “Our result that quenching of satellites correlates with Mh and anticorrelates with D is consistent with the results of Blanton & Berlind (2007) and Hansen et al. (2009) (who use group luminosity and group richness rather than Mh).”
Star formation and AGN activity in SDSS cluster galaxies (2009, background): “1013.5M⊙, Hansen et al. 2009), as well as at higher redshift (Poggiantiet al. 2006).”
What determines satellite galaxy disruption (2009, methodology): “We compare the luminosity function of satellites within galaxy clusters in our simulation with that determined from the SDSS MaxBCG catalog (Hansen et al. 2009).”
Galaxy evolution in groups and clusters: star formation rates, red sequence fractions and the persistent bimodality (2011, methodology): “An enhanced red/quenched fraction has been noted in examining galaxies out to 2–4 Rvir around massive clusters (Hansen et al. 2009; von der Linden et al. 2010).”
THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0–8 (2012, background): “Comparisons to other data sets atz ≤ 1.0 (Moster et al. 2010; Guo et al. 2010; Wang & Jing 2010; Zheng et al. 2007a; Yang et al. 2009a; Hansen et al. 2009; Lin & Mohr 2004) are discussed extensively in Behroozi et al. (2010), so we do not repeat that discussion here.”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, background): “The CSMF (or CLF) is a useful measurement for understanding both galaxy properties and cosmology (Yang et al. 2003, 2009; Cacciato et al. 2009; Hansen et al. 2009).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “…how much stellar mass is stored within the central galaxies of the dark matter halos (De Lucia & Blaizot 2007; von der Linden et al. 2007), and how is the rest distributed among the satellite galaxies within their larger host halos (Hansen et al. 2009; Yang et al. 2009; Leauthaud et al. 2012a)?”
Are Brightest Halo Galaxies Central Galaxies (2010, methodology): “…(e.g., Weinmann et al. 2006; Skibba et al. 2007; von der Linden et al. 2007; van den Bosch et al. 2008; Pasquali et al. 2009, 2010; Skibba 2009; Hansen et al. 2009) and halo model analyses of galaxy clustering (e.g., Skibba et al. 2006; Cooray 2006; van den Bosch et al. 2007; Skibba & Sheth…”
redMaPPer. I. ALGORITHM AND SDSS DR8 CATALOG (2013, unknown): “For the luminosity filter, we similarly follow R09 and R12 and adopt a Schechter function (e.g., Hansen et al. 2009), written as φ(mi) ∝ 10−0.4(mi−m∗)(α+1) exp ( −10−0.4(mi−m∗) ) .”
The accretion of galaxies into groups and clusters (2009, background): “Indeed, as previously mentioned, low-redshift observations show that the fraction of red galaxies in clusters is essentially uniform, for clusters with M > 1013.8 h−1 M (Hansen et al. 2009).”
Evidence for Significant Growth in the Stellar Mass of Brightest Cluster Galaxies over the Past 10 Billion Years (2012, methodology): “We do not adopt the relation found in Hansen et al. (2009).”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, methodology): “We emphasize that our goal is to find a high fidelity mass tracer, and we leave an analysis of the complete census of cluster galaxies to separate work (e.g., Hansen et al. 2009).”
MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION. II. THE QUENCHING OF SATELLITE GALAXIES AS THE ORIGIN OF ENVIRONMENTAL EFFECTS (2011, background): “…recent observational analyses have therefore distinguished between satellites and centrals (e.g. Weinmann et al. 2006 & 2009; von der Linden et al. 2007; van den Bosch et al. 2008a & 2008b; Yang et al. 2009a & 2009b; Pasquali et al. 2009 & 2010; Skibba 2009; Hansen et al. 2009; Kimm et al. 2009).”
A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4 (2010, background): “A second approach is to identify groups and clusters of galaxies either through optical or X-ray selected cluster catalogs,and then directly measure their galaxy content (e.g., Lin & Mohr 2004; Hansen et al. 2009; Yang et al. 2007).”
THE BLANCO COSMOLOGY SURVEY: DATA ACQUISITION, PROCESSING, CALIBRATION, QUALITY DIAGNOSTICS, AND DATA RELEASE (2012, background): “Interesting studies of the galaxy properties and their evolution within clusters include studies of the blue fraction and the halo occupation distribution (e.g. Butcher & Oemler 1984; Lin et al. 2003; Lin & Mohr 2004; Lin et al. 2006; Hansen et al. 2009; Zenteno et al. 2011).”
Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, background): “…et al. 2000; Ellingson et al. 2001; De Propris et al. 2004; Weinmann et al. 2006; Blanton & Berlind 2007; Kimm et al. 2009; van den Bosch et al. 2008; Hansen et al. 2009; Kimm et al. 2009; Pasquali et al. 2009; von der Linden et al. 2010; Prescott et al. 2011; Peng et al. 2012; Wetzel et al. 2012;…”