We characterize the luminosity distribution, halo mass dependence, and redshift evolution of red galaxies in galaxy clusters using the SDSS Data Release 8 redMaPPer cluster sample. We propose a simple prescription for the relationship between the luminosity of both central and satellite galaxies and the mass of their host halos, and show that this model is well-fit by the data. Using a larger galaxy cluster sample than previously employed in the literature, we find that the luminosities of central galaxies scale as hlog Li ∝ AL log(M200b), with AL = 0.39 ± 0.04, and that the scatter of the central-galaxy luminosity at fixed M200b (σlog L|M) is 0.23+0−0..0504 dex, with the error bar including systematics due to miscentering of the cluster finder, photometry, and photometric redshift estimation. Our data prefers a positive correlation between the luminosity of central galaxies and the observed richness of clusters at a fixed halo mass, with an effective correlation coefficient deff = 0.36+0−0..1716. The characteristic luminosity of satellites becomes dimmer from z = 0.3 to z = 0.1 by ∼ 20% after accounting for passive evolution. We estimate the fraction of galaxy clusters where the brightest galaxy is not the central to be PBNC ∼ 20%. We discuss implications of these findings in the context of galaxy evolution and the galaxy-halo connection.
|Original language||English (US)|
|State||Published - Oct 3 2019|
- Galaxy clusters
- Galaxy dark matter halos
- Galaxy evolution
- Large-scale structure of universe
ASJC Scopus subject areas