Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 456, Issue 3, Pages 3265-3281Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2871
Keywords
methods: data analysis; methods: statistical; surveys; galaxies: evolution; galaxies: fundamental parameters; galaxies: statistics
Categories
Funding
- US Department of Energy, Office of Science, Office of High Energy Physics [DE-SC0010331]
- Center for High Performance Computing at the University of Utah
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- University of Florida
- French Participation Group
- German Participation Group
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- U.S. Department of Energy (DOE) [DE-SC0010331] Funding Source: U.S. Department of Energy (DOE)
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We measure the intrinsic relation between velocity dispersion (sigma) and luminosity (L) for massive, luminous red galaxies at redshift z similar to 0.55. We achieve unprecedented precision by using a sample of 600 000 galaxies with spectra from the Baryon Oscillation Spectroscopic Survey of the third Sloan Digital Sky Survey (SDSS-III), covering a range of stellar masses M-* greater than or similar to 10(11) M-circle dot. We deconvolve the effects of photometric errors, limited spectroscopic signal-to-noise ratio, and red-blue galaxy confusion using a novel hierarchical Bayesian formalism that is generally applicable to any combination of photometric and spectroscopic observables. For an L-sigma relation of the form L proportional to sigma(beta), we find beta = 7.8 +/- 1.1 for sigma corrected to the effective radius, and a very small intrinsic scatter of s = 0.047 +/- 0.004 in log(10)sigma at fixed L. No significant redshift evolution is found for these parameters. The evolution of the zero-point within the redshift range considered is consistent with the passive evolution of a galaxy population that formed at redshift z = 2-3, assuming single stellar populations. An analysis of previously reported results seems to indicate that the passively evolved high-mass L-s relation at z similar to 0.55 is consistent with the one measured at z = 0.1. Our results, in combination with those presented in the LF work of Montero-Dorta et al., provide a detailed description of the high-mass end of the red sequence (RS) at z similar to 0.55. This characterization, in the light of previous literature, suggest that the high-mass RS distribution corresponds to the 'core' elliptical population.
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