The Mass Assembly History of Field Galaxies: Detection of an Evolving Mass Limit for Star‐Forming Galaxies

We characterize the mass-dependent evolution of galaxies in a large sample of more than 8, 000 galaxies using spectroscopic redshifts drawn from the DEEP2 Galaxy Redshift Survey in the range 0. 4 < z < 1. 4 and stellar masses calculated from K-band photometry obtained at Palomar Observatory. Using restframe (U-B) color and OII line widths, we distinguish star-forming from passive populations in order to explore the nature of "downsizing"--a pattern in which the sites of active star formation shift from high mass galaxies at early times to lower mass systems at later epochs. Over the redshift range probed, we identify a mass limit, MQ, above which star formation appears to be quenched. The physical mechanisms responsible for downsizing can thus be empirically quantified by charting the evolution in this threshold mass. We find that MQ decreases with time by a factor of ~5 across the redshift range sampled with a redshift dependence of (1+z) ⁴. 5. To further constrain possible quenching mechanisms, we investigate how this downsizing signal depends on local galaxy environment. For the majority of galaxies in regions near the median density, there is no significant correlation between downsizing and environment. However, a weak trend is observed in the comparison between more extreme environments that are more than 3 times overdense or underdense. Here, we find that downsizing is accelerated in overdense regions which host higher numbers of early-type galaxies and fewer late-types as compared to the underdense regions. Our results significantly constrain recent suggestions for the origin of downsizing and indicate that the process for quenching star formation must, primarily, be internally drive. Our survey provides a valuable benchmark for models incorporating baryon physics. (Abridged)