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We characterize the mass-dependent evolution in a large sample of more than8,000 galaxies using spectroscopic redshifts drawn from the DEEP2 GalaxyRedshift Survey in the range 0.4 < z < 1.4 and stellar masses calculated fromK-band photometry obtained at Palomar Observatory. Using restframe (U-B) colorand [OII] equivalent widths, we distinguish star-forming from passivepopulations in order to explore the nature of "downsizing''--a pattern in whichthe sites of active star formation shift from high mass galaxies at early timesto lower mass systems at later epochs. Over the redshift range probed, weidentify a mass limit, M_Q, above which star formation appears to be quenched.The physical mechanisms responsible for downsizing can thus be empiricallyquantified by charting the evolution in this threshold mass. We find that M_Qdecreases with time by a factor of ~3 across the redshift range sampledaccording with a redshift dependence of (1+z)^3.5. To further constrainpossible quenching mechanisms, we investigate how this downsizing signaldepends on local galaxy environment. For the majority of galaxies in regionsnear the median density, there is no significant correlation between downsizingand environment. However, a trend is observed in the comparison between moreextreme environments that are more than 3 times overdense or underdenserelative to the median. Here, we find that downsizing is accelerated inoverdense regions which host higher numbers of massive, early-type galaxies andfewer late-types as compared to the underdense regions. Our resultssignificantly constrain recent suggestions for the origin of downsizing andindicate that the process for quenching star formation must, primarily, beinternally driven. (Abridged)Comment: Accepted to ApJ, revised version addressing referee's comments, 23  pages, 13 figure

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