The Evolution of the Global Stellar Mass Density at 0 < z < 3
  The build-up of stellar mass in galaxies is the consequence of their past star formation and merging histories. Here we report measurements of rest-frame optical light and calculations of stellar mass at high redshift based on an infrared-selected sample of galaxies from the Hubble Deep Field North. The bright envelope of rest-frame B-band galaxy luminosities is similar from 0<z<3, and the co-moving luminosity density is constant to within a factor of 3 over that redshift range. However, galaxies at higher redshifts are bluer, and stellar population modeling indicates that they had significantly lower mass-to-light ratios than those of present-day L* galaxies. This leads to a global stellar mass density, Omega_*(z), which rises with time from z=3 to the present. This measurement essentially traces the integral of the cosmic star formation history that has been the subject of previous investigations. 50-75% of the present-day stellar mass density had formed by z ~ 1, but at z ~= 2.7 we find only 3-14% of today's stars were present. This increase in Omega_* with time is broadly consistent with observations of the evolving global star formation rate once dust extinction is taken into account, but is steeper at 1<z<3 than predicted by some recent semi-analytic models of galaxy formation. The observations appear to be inconsistent with scenarios in which the bulk of stars in present-day galactic spheroids formed at z>>2. 
Mark Dickinson (STScI), Casey Papovich (Steward Observatory), Henry C.   Ferguson (STScI), and Tamas Budavari (JHU)