Issue |
A&A
Volume 579, July 2015
|
|
---|---|---|
Article Number | A26 | |
Number of page(s) | 19 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/201525834 | |
Published online | 22 June 2015 |
Evolution of the luminosity-to-halo mass relation of LRGs from a combined analysis of SDSS-DR10+RCS2⋆
1
Argelander-Institut für Astronomie,
Auf dem Hügel 71,
53121
Bonn,
Germany
e-mail:
vuitert@astro.uni-bonn.de
2
Leiden Observatory, Leiden University,
Niels Bohrweg 2, 2333 CA
Leiden, The
Netherlands
Received: 6 February 2015
Accepted: 30 March 2015
We study the evolution of the luminosity-to-halo mass relation of luminous red galaxies (LRGs). We selected a sample of 52 000 LOWZ and CMASS LRGs from the Baryon Oscillation Spectroscopic Survey (BOSS) SDSS-DR10 in the ~450 deg2 that overlaps with imaging data from the second Red-sequence Cluster Survey (RCS2), grouped them into bins of absolute magnitude and redshift and measured their weak-lensing signals. The source redshift distribution has a median of 0.7, which allowed us to study the lensing signal as a function of lens redshift. We interpreted the lensing signal using a halo model, from which we obtained the halo masses as well as the normalisations of the mass-concentration relations. The concentration of haloes that host LRGs is consistent with dark-matter-only simulations once we allow for miscentering or satellites in the modelling. The slope of the luminosity-to-halo mass relation has a typical value of 1.4 and does not change with redshift, but we find evidence for a change in amplitude: the average halo mass of LOWZ galaxies increases by 25-14+16% between z = 0.36 and 0.22 to an average value of (6.43 ± 0.52) × 1013 h70-1M⊙. If we extend the redshift range using the CMASS galaxies and assume that they are the progenitors of the LOWZ sample, the average mass of LRGs increases by 80+39-28\% between z = 0.6 and 0.2.
Key words: galaxies: halos / galaxies: evolution / methods: observational / gravitational lensing: weak
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2015
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