A Brighter Past: Galaxy Luminosity Function At High Redshifts
  Using the conditional luminosity function -- the luminosity distribution of galaxies in a dark matter halo as a function of the halo mass -- we present an empirical model to describe the redshift evolution of the rest B-band galaxy luminosity function (LF). The model is compared to measured LFs out to a redshift of 3.5, including LFs of galaxy types separated to red and blue galaxies. The increase in the number density of luminous galaxies, at the bright-end of the LF, can be explained as due to a brightening of the luminosity of galaxies present in dark matter halo centers, relative to the luminosity of central galaxies in similar mass halos today. The lack of strong evolution in the faint-end of the LF, however, argues against a model involving pure luminosity evolution at all halo mass scales. The increase in luminosity at the bright-end compensates the rapid decline in the number density of massive halos as the redshift is increased. The decline in group to cluster-mass dark matter halos out to a redshift of ~ 2 is not important as the central galaxy luminosity flattens at halo masses around 10^13 M_sun At redshifts ~ 2 to 3, however, the density of bright galaxies begins to decrease due to the rapid decline in the number density of dark matter halos at mass scales around and below 10^13 M_sun. We compare our predictions to the UV LF of galaxies at redshifts 3 to 6 and the galaxy clustering bias measurements at redshifts ~ 3, and use our models to establish the dark matter halo mass scales of galaxies observed at high redshifts. In general, to explain high-redshift LFs, galaxies in dark matter halos around 10^12 M_sun must increase in luminosity by a factor of ~ 4 to 6 between today and redshift of 6. 
Asantha Cooray