THE PAN-STARRS1 MEDIUM-DEEP SURVEY: THE ROLE OF GALAXY GROUP ENVIRONMENT IN THE STAR FORMATION RATE VERSUS STELLAR MASS RELATION AND QUIESCENT FRACTION OUT TO z ∼ 0.8

被引：80

作者：

Lin, Lihwai ^{[1
]}

Jian, Hung-Yu ^{[2
]}

Foucaud, Sebastien ^{[1
,3
]}

Norberg, Peder ^{[4
]}

Bower, R. G. ^{[4
]}

Cole, Shaun

Arnalte-Mur, Pablo ^{[4
]}

Chen, Chin-Wei ^{[1
]}

Coupon, Jean ^{[1
,5
]}

Hsieh, Bau-Ching ^{[1
]}

Heinis, Sebastien ^{[6
]}

Phleps, Stefanie ^{[7
]}

Chen, Wen-Ping ^{[8
]}

Lee, Chien-Hsiu ^{[7
,9
]}

Burgett, William ^{[10
]}

Chambers, K. C. ^{[10
]}

Denneau, L. ^{[10
]}

Draper, P. ^{[4
]}

Flewelling, H. ^{[10
]}

Hodapp, K. W. ^{[10
]}

Huber, M. E. ^{[10
]}

Kaiser, N. ^{[10
]}

Kudritzki, R. -P. ^{[10
]}

Magnier, E. A. ^{[10
]}

Metcalfe, N. ^{[4
]}

Price, Paul A. ^{[11
]}

Tonry, J. L. ^{[10
]}

Wainscoat, R. J. ^{[10
]}

Waters, C. ^{[10
]}

机构：

[1] Acad Sinica, Inst Astron Astrophys, Taipei 106, Taiwan

[2] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan

[3] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 11677, Taiwan

[4] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England

[5] Univ Geneva, Dept Astron, CH-1290 Versoix, Switzerland

[6] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[7] Max Planck Inst Extraterrestr Phy, D-85748 Garching, Germany

[8] Natl Cent Univ, Grad Inst Astron, Chungli 32054, Taiwan

[9] Univ Observ Munich, D-81679 Munich, Germany

[10] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[11] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 782卷 / 01期

基金：

美国国家科学基金会; 美国国家航空航天局; 欧洲研究理事会;

关键词：

galaxies: evolution; galaxies: groups: general; galaxies: high-redshift; large-scale structure of universe; DIGITAL SKY SURVEY; FORMATION-DENSITY RELATION; REDSHIFT SURVEY; FORMING GALAXIES; PHOTOMETRIC REDSHIFTS; SPECTROSCOPIC SURVEY; FORMATION HISTORIES; LUMINOSITY FUNCTION; CLUSTER SURVEY; COSMOS SURVEY;

D O I：

10.1088/0004-637X/782/1/33

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using a large optically selected sample of field and group galaxies drawn from the Pan-STARRS1 Medium-Deep Survey (PS1/MDS), we present a detailed analysis of the specific star formation rate (SSFR)-stellar mass (M-*) relation, as well as the quiescent fraction versus M-* relation in different environments. While both the SSFR and the quiescent fraction depend strongly on stellar mass, the environment also plays an important role. Using this large galaxy sample, we confirm that the fraction of quiescent galaxies is strongly dependent on environment at a fixed stellar mass, but that the amplitude and the slope of the star-forming sequence is similar between the field and groups: in other words, the SSFR-density relation at a fixed stellar mass is primarily driven by the change in the star-forming and quiescent fractions between different environments rather than a global suppression in the star formation rate for the star-forming population. However, when we restrict our sample to the cluster-scale environments (M > 10(14) M-circle dot), we find a global reduction in the SSFR of the star-forming sequence of 17% at 4 sigma confidence as opposed to its field counterpart. After removing the stellar mass dependence of the quiescent fraction seen in field galaxies, the excess in the quiescent fraction due to the environment quenching in groups and clusters is found to increase with stellar mass, although deeper and larger data from the full PS1/MDS will be required to draw firm conclusions. We argue that these results are in favor of galaxy mergers to be the primary environment quenching mechanism operating in galaxy groups whereas strangulation is able to reproduce the observed trend in the environment quenching efficiency and stellar mass relation seen in clusters. Our results also suggest that the relative importance between mass quenching and environment quenching depends on stellar mass-the mass quenching plays a dominant role in producing quiescent galaxies for more massive galaxies, while less massive galaxies are quenched mostly through the environmental effect, with the transition mass around 1-2 x 10(10) M-circle dot in the group/cluster environment.

引用

页数：16

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