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Title: THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS

Abstract

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 r {sub 200} of clusters with mass above 3 x 10{sup 13} h {sup -1} M {sub sun}, 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 {sup 0.25} M{sub i} - 5log{sub 10} h =-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 {approx}5% between redshifts 0.28 and 0.2, independent of richness. We find that BCG luminosity is tightly correlated with cluster richness, scaling as L {sub BCG} {approx} Mmore » {sup 0.3} {sub 200}, and has a Gaussian distribution at fixed richness, with {sigma}{sub logL} {approx} 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.« less

Authors:
 [1];  [2];  [3]
  1. UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 (United States)
  2. Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003 (United States)
  3. Kavli Institute for Particle Astrophysics and Cosmology, Physics Department, and Stanford Linear Accelerator Center, Stanford University, Stanford, CA 94305 (United States)
Publication Date:
OSTI Identifier:
21333729
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 699; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/699/2/1333; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ALGORITHMS; COLOR; COSMOLOGY; GALACTIC EVOLUTION; GALAXIES; GALAXY CLUSTERS; GAUSS FUNCTION; LUMINOSITY; MASS; RED SHIFT; SATELLITES

Citation Formats

Hansen, Sarah M, Sheldon, Erin S, Wechsler, Risa H, and Koester, Benjamin P. THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS. United States: N. p., 2009. Web. doi:10.1088/0004-637X/699/2/1333; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Hansen, Sarah M, Sheldon, Erin S, Wechsler, Risa H, & Koester, Benjamin P. THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS. United States. https://doi.org/10.1088/0004-637X/699/2/1333; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)
Hansen, Sarah M, Sheldon, Erin S, Wechsler, Risa H, and Koester, Benjamin P. Fri . "THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS". United States. https://doi.org/10.1088/0004-637X/699/2/1333; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
@article{osti_21333729,
title = {THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS},
author = {Hansen, Sarah M and Sheldon, Erin S and Wechsler, Risa H and Koester, Benjamin P.},
abstractNote = {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 r {sub 200} of clusters with mass above 3 x 10{sup 13} h {sup -1} M {sub sun}, 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 {sup 0.25} M{sub i} - 5log{sub 10} h =-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 {approx}5% between redshifts 0.28 and 0.2, independent of richness. We find that BCG luminosity is tightly correlated with cluster richness, scaling as L {sub BCG} {approx} M {sup 0.3} {sub 200}, and has a Gaussian distribution at fixed richness, with {sigma}{sub logL} {approx} 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.},
doi = {10.1088/0004-637X/699/2/1333; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)},
url = {https://www.osti.gov/biblio/21333729}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 699,
place = {United States},
year = {2009},
month = {7}
}