The physical and photometric properties of high-redshift galaxies in cosmological hydrodynamic simulations

We study the physical and photometric properties of galaxies at z = 4 in cosmological hydrodynamic simulations of a Lambda CDM universe. We focus on galaxies satisfying the `` B dropout'' criteria of the Great Observatories Origins DEEP Survey ( GOODS). Our simulations predict that high- redshift galaxies show strong correlations in star formation rate ( SFR) versus stellar mass, and weaker correlations versus environment and age, such that B dropouts are predicted to be the most massive, most rapidly star- forming galaxies at z 4, living preferentially in dense regions. The simulated rest- frame UV luminosity function ( LF) and integrated luminosity density are in broad agreement with observations at z similar to 4. The predicted faint- end slope is intrinsically steep but becomes shallower and is in reasonable agreement with data once GOODS selection criteria are imposed. At the bright end, there may be a modest excess of bright, rapidly star- forming galaxies. The predicted rest- frame optical LF is approximately 1 mag brighter than the rest- frame UV LF. We predict that GOODS B dropouts represent less than 50% of the total stellar mass density formed in galaxies more massive than log ( M (*) / M (circle dot)) > 87 by z = 4, mainly because of brightness limits in the HSTACS bands. Most of these results are somewhat sensitive to the effects of dust extinction. On average, simulated B dropouts are less metal enriched than observed low- redshift galaxies of similar stellar mass by approximate to 0.6 dex. Two simulated B dropouts exhibit SFRs exceeding 1000 M (circle dot) yr (- 1), similar to observed submillimeter galaxies. These galaxies are quite massive but are not undergoing starbursts; their SFRs only mildly exceed ( by similar to 2 - 3 times) the SFRs that would be expected for their stellar mass. Finally, the overall distribution of dust reddening and mean stellar age may be constrained from color- color plots although the specific value for each galaxy cannot.