The size function of massive satellites from the $R_e-R_h$ and $M_{star}-M_h$ relations: constraining the role of environment

Abstract

In previous work we showed that a semi-empirical model in which galaxies in host dark matter haloes are assigned stellar masses via a stellar mass-halo mass (SMHM) relation and sizes ($R_e$) via a linear and tight $R_e-R_h$ relation, can faithfully reproduce the size function of local SDSS central galaxies and the strong size evolution of massive galaxies (MGs, $M_{\mathrm{star}}>10^{11.2}{M}_{\odot }$). In this third paper of the series, we focus on the population of satellite MGs. We find that without any additional calibration and irrespective of the exact SMHM relation, fraction of quenched galaxies or level of stellar stripping, the same model is able to reproduce the local size function of quiescent satellite MGs in SDSS. In addition, the same model can reproduce the puzzling weak dependence of mean size on host halo mass for both central and satellite galaxies. The model also matches the size function of starforming satellite MGs, after assuming that some of them transform into massive lenticulars in a few Gyr after infalling in the group/cluster environment. However, the vast majority of satellite lenticulars is predicted to form before infall. The $R_e-R_h$ appears to be fundamental to connect galaxies and their host haloes.

Accepted for publication in MNRAS. 5 pages, 3 figures. Comments and suggestions still welcome

References in corpus (10)

• A catalogue of 2D photometric decompositions in the SDSS-DR7 spectroscopic main galaxy sample: preferred models and systematics
• The stellar-to-halo mass relations of local galaxies segregates by color
• The Preferential Tidal Stripping of Dark Matter versus Stars in Galaxies
• Relations Between the Sizes of Galaxies and their Dark Matter Halos at Redshifts $0<z<3$
• The SAMI Galaxy Survey: A Range in S0 Properties Indicating Multiple Formation Pathways
• Galaxy sizes and the galaxy-halo connection -- I: the remarkable tightness of the size distributions
• Structural and dynamical modeling of WINGS clusters. I. The distribution of cluster galaxies of different morphological classes within regular and irregular clusters
• Comparing PyMorph and SDSS photometry. I. Background sky and model fitting effects
• Predicting fully self-consistent satellite richness, galaxy growth and starformation rates from the STastical sEmi-Empirical modeL STEEL
• The evolution of compact massive quiescent and starforming galaxies derived from the $R_e-R_h$ and $M_{\mathrm{star}}-M_h$ relations

Cited by in corpus (4)

• The galaxy-halo size relation of low-mass galaxies in FIRE
• The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 < z < 2.8: larger cluster galaxy sizes
• Environments of red nuggets at z~0.7 from the VIPERS survey
• Testing the key role of the stellar mass-halo mass relation in galaxy merger rates and morphologies via DECODE, a novel Discrete statistical sEmi-empiriCal mODEl