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 \mbox { SFR } - \mbox { $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 M _ { 50 } above which 50 % of galaxies are quenched coincides with sSFR/sMAR \sim 1 , where sMAR is the specific halo mass accretion rate .
( 2 ) M _ { 50 } 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 \mbox { $M _ { vir } $ } \sim 2 \times 10 ^ { 11 } \mbox { M$ { } _ { \odot } $ } .
( 4 ) The stellar mass density within 1 kpc , \Sigma _ { 1 } , is a good indicator of the galactic global sSFR .
( 5 ) Galaxies are statistically quenched after they reach a maximum in \Sigma _ { 1 } , 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 d \log \mbox { $R _ { eff } $ } / d \log \mbox { $M _ { * } $ } \sim 0.35 to \sim 2.5 , could be the result of dry minor mergers .