The size function of massive satellites from the R<SUB>e</SUB>-R<SUB>h</SUB> and M<SUB>star</SUB>-M<SUB>h</SUB> relations: constraining the role of environment

Zanisi, L.; Shankar, F.; Bernardi, M.; Mei, S.; Huertas-Company, M.
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Monthly Notices of the Royal Astronomical Society

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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 (Re) via a linear and tight Re-Rh relation can faithfully reproduce the size function of local Sloan Digital Sky Survey (SDSS) central galaxies and the strong size evolution of massive galaxies (MGs; Mstar > 1011.2 M⊙). 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 star-forming 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 are predicted to form before infall. The Re-Rh relation appears to be fundamental to connect galaxies and their host haloes.
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Traces of Galaxy Formation: Stellar populations, Dynamics and Morphology
We are a large, diverse, and very active research group aiming to provide a comprehensive picture for the formation of galaxies in the Universe. Rooted in detailed stellar population analysis, we are constantly exploring and developing new tools and ideas to understand how galaxies came to be what we now observe.
Martín Navarro