Evolution of Star-formation Properties of High-redshift Cluster Galaxies since $z=2$

Abstract

Using a stellar mass limited sample of $\sim 46,600$ galaxies ($M_{\ast }>10^{9.1}{M}_{\odot }$) at $0.5<z<2$, we show that the tellar mass, rather than the environment, is the main parameter controlling quenching of star formation in galaxies with $M_{\ast }>10^{10}{M}_{\odot }$ out to $z=2$. On the other hand, the environmental quenching becomes efficient at $z<1$ regardless of galaxy mass, and it serves as a main star formation quenching mechanism for lower mass galaxies. Our result is based on deep optical and near-infrared imaging data over 2800 arcmin${}^2$, enabling us to negate cosmic variance and identify 46 galaxy cluster candidates with $M\sim 10^{14}{M}_{\odot }$. From $M_{\ast }\sim 10^{9.5}$ to $10^{10.5}{M}_{\odot }$, the fraction of quiescent galaxies increases by a factor of $\sim 10$ over the entire redshift range, but the difference between cluster and field environment is negligible. Rapid evolution in the quiescent fraction is seen from $z=2$ to $z=1.3$ for massive galaxies suggesting a build-up of massive quiescent galaxies at $z>1.3$. For galaxies with $M_{\ast }<10^{10}{M}_{\odot }$ at $z<1.0$, the quiescent fraction is found to be as much as a factor of 2 larger in clusters than in field, showing the importance of environmental quenching in low mass galaxies at low redshift. Most high mass galaxies are already quenched at $z>1$, therefore environmental quenching does not play a significant role for them, although the environmental quenching efficiency is nearly identical between high and low mass galaxies.

18 pages, 22 figures, 1 table, Accepted for publication in ApJ

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