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Title: LUMINOUS SATELLITES. II. SPATIAL DISTRIBUTION, LUMINOSITY FUNCTION, AND COSMIC EVOLUTION

Abstract

We infer the normalization and the radial and angular distributions of the number density of satellites of massive galaxies (log{sub 10}[M*{sub h}/M{sub Sun }] > 10.5) between redshifts 0.1 and 0.8 as a function of host stellar mass, redshift, morphology, and satellite luminosity. Exploiting the depth and resolution of the COSMOS Hubble Space Telescope images, we detect satellites up to 8 mag fainter than the host galaxies and as close as 0.3 (1.4) arcsec (kpc). Describing the number density profile of satellite galaxies to be a projected power law such that P(R){proportional_to}R{sup {gamma}{sub p}}, we find {gamma}{sub p} = -1.1 {+-} 0.3. We find no dependency of {gamma}{sub p} on host stellar mass, redshift, morphology, or satellite luminosity. Satellites of early-type hosts have angular distributions that are more flattened than the host light profile and are aligned with its major axis. No significant average alignment is detected for satellites of late-type hosts. The number of satellites within a fixed magnitude contrast from a host galaxy is dependent on its stellar mass, with more massive galaxies hosting significantly more satellites. Furthermore, high-mass late-type hosts have significantly fewer satellites than early-type galaxies of the same stellar mass, possibly indicating that they residemore » in more massive halos. No significant evolution in the number of satellites per host is detected. The cumulative luminosity function of satellites is qualitatively in good agreement with that predicted using SubHalo Abundance Matching techniques. However, there are significant residual discrepancies in the absolute normalization, suggesting that properties other than the host galaxy luminosity or stellar mass determine the number of satellites.« less

Authors:
;  [1];  [2];  [3];  [4];  [5]
  1. Department of Physics, University of California, Santa Barbara, CA 93106 (United States)
  2. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB30HA (United Kingdom)
  3. Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH (United Kingdom)
  4. Department of Physics, University of California, Davis, CA 95616 (United States)
  5. Institute for Theoretical Physics, University of Zuerich, Zuerich (Switzerland)
Publication Date:
OSTI Identifier:
22037038
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 752; Journal Issue: 2; Other Information: 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; ANGULAR DISTRIBUTION; ASTRONOMY; ASTROPHYSICS; DENSITY; GALACTIC EVOLUTION; GALAXIES; GRAVITATIONAL LENSES; IMAGES; LUMINOSITY; MASS; MORPHOLOGY; NONLUMINOUS MATTER; RED SHIFT; SPATIAL DISTRIBUTION; UNIVERSE; VISIBLE RADIATION

Citation Formats

Nierenberg, A. M., Treu, T., Auger, M. W., Marshall, P. J., Fassnacht, C. D., and Busha, Michael T., E-mail: amn01@physics.ucsb.edu. LUMINOUS SATELLITES. II. SPATIAL DISTRIBUTION, LUMINOSITY FUNCTION, AND COSMIC EVOLUTION. United States: N. p., 2012. Web. doi:10.1088/0004-637X/752/2/99.
Nierenberg, A. M., Treu, T., Auger, M. W., Marshall, P. J., Fassnacht, C. D., & Busha, Michael T., E-mail: amn01@physics.ucsb.edu. LUMINOUS SATELLITES. II. SPATIAL DISTRIBUTION, LUMINOSITY FUNCTION, AND COSMIC EVOLUTION. United States. doi:10.1088/0004-637X/752/2/99.
Nierenberg, A. M., Treu, T., Auger, M. W., Marshall, P. J., Fassnacht, C. D., and Busha, Michael T., E-mail: amn01@physics.ucsb.edu. Wed . "LUMINOUS SATELLITES. II. SPATIAL DISTRIBUTION, LUMINOSITY FUNCTION, AND COSMIC EVOLUTION". United States. doi:10.1088/0004-637X/752/2/99.
@article{osti_22037038,
title = {LUMINOUS SATELLITES. II. SPATIAL DISTRIBUTION, LUMINOSITY FUNCTION, AND COSMIC EVOLUTION},
author = {Nierenberg, A. M. and Treu, T. and Auger, M. W. and Marshall, P. J. and Fassnacht, C. D. and Busha, Michael T., E-mail: amn01@physics.ucsb.edu},
abstractNote = {We infer the normalization and the radial and angular distributions of the number density of satellites of massive galaxies (log{sub 10}[M*{sub h}/M{sub Sun }] > 10.5) between redshifts 0.1 and 0.8 as a function of host stellar mass, redshift, morphology, and satellite luminosity. Exploiting the depth and resolution of the COSMOS Hubble Space Telescope images, we detect satellites up to 8 mag fainter than the host galaxies and as close as 0.3 (1.4) arcsec (kpc). Describing the number density profile of satellite galaxies to be a projected power law such that P(R){proportional_to}R{sup {gamma}{sub p}}, we find {gamma}{sub p} = -1.1 {+-} 0.3. We find no dependency of {gamma}{sub p} on host stellar mass, redshift, morphology, or satellite luminosity. Satellites of early-type hosts have angular distributions that are more flattened than the host light profile and are aligned with its major axis. No significant average alignment is detected for satellites of late-type hosts. The number of satellites within a fixed magnitude contrast from a host galaxy is dependent on its stellar mass, with more massive galaxies hosting significantly more satellites. Furthermore, high-mass late-type hosts have significantly fewer satellites than early-type galaxies of the same stellar mass, possibly indicating that they reside in more massive halos. No significant evolution in the number of satellites per host is detected. The cumulative luminosity function of satellites is qualitatively in good agreement with that predicted using SubHalo Abundance Matching techniques. However, there are significant residual discrepancies in the absolute normalization, suggesting that properties other than the host galaxy luminosity or stellar mass determine the number of satellites.},
doi = {10.1088/0004-637X/752/2/99},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 752,
place = {United States},
year = {2012},
month = {6}
}