2015/03/30 by Edo van Uitert, Marcello Cacciato, Henk Hoekstra +1 · 21 citations
Engineering · Physics and Astronomy · #Absolute magnitude #Astronomy and Astrophysical Research #Baryon #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Mass distribution #Redshift #Space Technology and Applications #Stellar mass #Weak gravitational lensing #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1051/0004-6361/201525834
published in Astronomy and Astrophysics 579, A26 (EDP Sciences) · 20 pages, 11 figures, accepted for publication in A&A
arxiv created 2015/03/30 · openalex publication_date 2015/04/21 · arxiv updated 2015/06/24 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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.