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Clustering properties of BzK-selected galaxies in GOODS-N: environmental quenching and triggering of star formation at z ~ 2 | | Lihwai Lin
; Mark Dickinson
; Hung-Yu Jian
; A. I. Merson
; C. M. Baugh
; Douglas Scott
; Sebastien Foucaud
; Wei-Hao Wang
; Chi-Hung Yan
; Hao-Jing Yan
; Yi-Wen Cheng
; Yicheng Guo
; John Helly
; Franz Kirsten
; David C. Koo
; Claudia del P. Lagos
; Nicole Meger
; Alexandra Pope
; Luc Simard
; Norman A. Grogin
; Hugo Messias
; Shiang-Yu Wang
; | | Date: |
9 Nov 2011 | | Abstract: | Using a sample of $ extit{BzK}$-selected galaxies at $z sim 2$ identified
from the CFHT/WIRCAM near-infrared survey of GOODS-North, we discuss the
relation between star formation rate (SFR), specific star formation rate
(SSFR), and stellar mass (sm), and the clustering of galaxies as a function of
these parameters. For star-forming galaxies ( extit{sBzK}s), the UV-based SFR,
corrected for extinction, scales with the stellar mass as SFR $propto$
sm$^{alpha}$ with $alpha = 0.74pm0.20$, indicating a weak dependence on the
stellar mass of the star formation rate efficiency. We also measure the angular
correlation function and hence infer the correlation length for extit{sBzK}
galaxies as a function of sm, SFR, and SSFR, as well as $K$-band apparent
magnitude. We show that passive galaxies ( extit{pBzK}s) are more strongly
clustered than extit{sBzK} galaxies at a given stellar mass. We also find
that the correlation length of extit{sBzK} galaxies ranges from 4 to 17 mpc,
being a strong function of $M_{K}$, sm, and SFR. On the other hand, the
clustering dependence on SSFR changes abruptly at $2 imes 10^{-9}$ yr$^{-1}$,
which is the typical value for ’’main sequence’’ star-forming galaxies at $z
sim 2$. We show that the correlation length reaches a minimum at this
characteristic value, and is larger for galaxies with both smaller and larger
SSFRs; a dichotomy that is only marginally implied from the predictions of the
semi-analytical models. Our results suggest that there are two types of
environmental effects: stronger clustering for relatively quiescent galaxies
implies that the environment has started playing a role in quenching or
reducing star formation at $z sim 2$, while the interpretation for galaxies
with elevated SSFRs (’’starbursts’’) might be attributed to galaxy mergers
and/or other mechanisms which are also associated with dense environments. | | Source: | arXiv, 1111.2135 | | Services: | Forum | Review | PDF | Favorites | |
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