The role of massive halos in the star formation history of the Universe

被引：20

作者：

Popesso, P. ^{[1
,2
]}

Biviano, A. ^{[3
]}

Finoguenov, A. ^{[2
]}

Wilman, D. ^{[2
]}

Salvato, M. ^{[2
]}

Magnelli, B. ^{[2
]}

Gruppioni, C. ^{[4
]}

Pozzi, F. ^{[5
]}

Rodighiero, G. ^{[6
]}

Ziparo, F. ^{[2
]}

Berta, S. ^{[2
]}

Elbaz, D. ^{[7
]}

Dickinson, M. ^{[7
]}

Lutz, D. ^{[2
]}

Altieri, B. ^{[9
]}

Aussel, H. ^{[8
]}

Cimatti, A. ^{[6
]}

Fadda, D. ^{[10
]}

Ilbert, O. ^{[11
]}

Le Floch, E. ^{[8
]}

Nordon, R. ^{[2
]}

Poglitsch, A. ^{[2
]}

Genel, S. ^{[12
]}

Xu, C. K. ^{[13
]}

机构：

[1] Excellence Cluster Universe, D-85748 Garching, Germany

[2] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany

[3] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

[4] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy

[5] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[6] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy

[7] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[8] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France

[9] ESA, European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain

[10] Caltech 100 22, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA

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

[12] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[13] Caltech 100 22, IPAC, Pasadena, CA 91125 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 579卷

关键词：

galaxies: evolution; galaxies: star formation; galaxies: groups: general; INFRARED LUMINOSITY FUNCTIONS; DEEP-FIELD-SOUTH; HIERARCHICAL GALAXY FORMATION; GALACTIC NUCLEUS FEEDBACK; SUPERMASSIVE BLACK-HOLES; REST-FRAME ULTRAVIOLET; X-RAY GROUPS; FORMING GALAXIES; COSMOS FIELD; SPITZER VIEW;

D O I：

10.1051/0004-6361/201424715

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The most striking feature of the cosmic star formation history (CSFH) of the Universe is a dramatic drop in the star formation (SF) activity after z similar to 1. Aims. In this work we investigate whether the very same process of assembly and growth of structures is one of the major drivers of the observed decline in the Universe's SF activity. Methods. We study the contribution to the CSFH of galaxies in halos of different masses. This is done by studying the total SF ratehalo mass-redshift plane from redshift 0 to redshift similar to 1.6 in a sample of 57 groups and clusters by using the deepest available mid- and far-infrared surveys conducted with Spitzer MIPS and Herschel PACS and SPIRE, on blank (ECDFS, CDFN, and the COSMOS) and cluster fields. Results. Our results show that low mass groups (M-halo similar to 6 x 10(12) - 6 x 10(13) M-circle dot) provide a 60-80% contribution to the CSFH at z similar to 1. This contribution has declined faster than the CSFH in the past 8 billion years to less than 10% at z < 0.3, where the overall SF activity is sustained by lower mass halos. More massive systems (M-halo > 6 x 10(13) M-circle dot) provide only a marginal contribution (<10%) at any epoch. A simplified abundance-matching method shows that the large contribution of low mass groups at z similar to 1 is due to a large fraction (>50%) of very massive, highly star-forming main sequence galaxies. Below z similar to 1 a quenching process must take place in massive halos to cause the observed faster suppression of their SF activity. Such a process must be a slow one, though, since most of the models implementing a rapid quenching of the SF activity in accreting satellites significantly underpredict the observed SF level in massive halos at any redshift. This would rule out short time-scale mechanisms such as ram pressure stripping. Instead, starvation or the satellite's transition from cold to hot accretion would provide a quenching timescale of 1 to few Gyr that is more consistent with the observations. Conclusions. Our results suggest a scenario in which, owing to the structure formation process, more and more galaxies experience the group environment and the associated quenching process in the past 8 billion years. This leads to the progressive suppression of their SF activity so that it shapes the CSFH below z similar to 1.

引用

页数：17

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