Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties

2017/03/31 by Aldo Rodríguez-Puebla, Aldo Rodriguez-Puebla, Joel R. Primack +3 · 239 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Halo #Physics #Redshift #Star formation #Stellar mass #Virial theorem #astro-ph.GA

paper · pdf · doi:10.1093/mnras/stx1172

published in Monthly Notices of the Royal Astronomical Society 470(1), 651-687 (Oxford University Press) · 42 pages, 31 Figures. Accepted for publication in MNRAS. Typos corrected. The results presented in this paper are available via an interactive website: https://132.248.1.39/galaxy/galaxy_halo.html

openalex created_date 2017/04/07 · openalex publication_date 2017/05/11 · arxiv created 2017/05/15 · arxiv updated 2017/06/28 · openalex updated_date 2026/08/08

Abstract

We present new determinations of the stellar-to-halo mass relation (SHMR) at z=0-10 that match the evolution of the galaxy stellar mass function, the SFR-M_* relation,and the cosmic star formation rate. We utilize a compilation of 40 observational studies from the literature and correct them for potential biases. Using our robust determinations of halo mass assembly and the SHMR, we infer star formation histories, merger rates, and structural properties for average galaxies, combining star-forming and quenched galaxies. Our main findings: (1) The halo mass M₅₀ above which 50% of galaxies are quenched coincides with sSFR/sMAR∼1, where sMAR is the specific halo mass accretion rate. (2) M₅₀ increases with redshift, presumably due to cold streams being more efficient at high redshift while virial shocks and AGN feedback become more relevant at lower redshifts. (3) The ratio sSFR/sMAR has a peak value, which occurs around M_{\rm vir}∼2×10¹¹M_\odot. (4) The stellar mass density within 1 kpc, Σ₁, is a good indicator of the galactic global sSFR. (5) Galaxies are statistically quenched after they reach a maximum in Σ₁, consistent with theoretical expectations of the gas compaction model; this maximum depends on redshift. (6) In-situ star formation is responsible for most galactic stellar mass growth, especially for lower-mass galaxies. (7) Galaxies grow inside out. The marked change in the slope of the size--mass relation when galaxies became quenched, from dlog R_{\rm eff}/dlog M_*∼0.35 to ∼2.5, could be the result of dry minor mergers.

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