The main sequence of star-forming galaxies - I. The local relation and its bending

被引：91

作者：

Popesso, P. ^{[1
]}

Concas, A. ^{[1
]}

Morselli, L. ^{[1
]}

Schreiber, C. ^{[2
]}

Rodighiero, G. ^{[3
]}

Cresci, G. ^{[4
]}

Belli, S. ^{[5
]}

Erfanianfar, G. ^{[5
]}

Mancini, C. ^{[2
]}

Inami, H. ^{[6
]}

Dickinson, M. ^{[7
]}

Ilbert, O. ^{[8
]}

Pannella, M. ^{[9
]}

Elbazi, D. ^{[10
]}

机构：

[1] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany

[2] Leiden Univ, Leiden Observ, POB 9500, NL-2300 RA Leiden, Netherlands

[3] Univ Padua, Vicolo Osservatorio, I-35122 Padua, Italy

[4] INAF, Osservatorio Astron Arcetri, Largo Enrico Fermi 5, I-50125 Florence, FI, Italy

[5] Max Planck Extraterr Phys, Giessenbachstr 1, D-85478 Garching, Germany

[6] Univ Lyon 1, Univ Lyon, ENS Lyon, CNRS,Ctr Rech Astrophys Lyon UMR5574, F-69230 St Genis Laval, France

[7] Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA

[8] Lab Astrophys Marseille, 38 Rue Frederic Joliot Curie, F-13388 Marseille, France

[9] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[10] CEA, Serv Astrophys, F-91190 Gif Sur Yvette, France

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 483卷 / 03期

关键词：

galaxies: evolution; galaxies: groups; galaxies: haloes; galaxies: starburst; galaxies: star formation; GALACTIC NUCLEUS FEEDBACK; DIGITAL SKY SURVEY; DATA RELEASE; FORMATION RATES; AGN FEEDBACK; BLACK-HOLES; MASSIVE GALAXIES; STELLAR MASSES; SCALE OUTFLOWS; CATALOG;

D O I：

10.1093/mnras/sty3210

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

By using a set of different star formation rate (SFR) indicators, including Wide-field Infrared Survey Explorer (WISE) mid-infrared and Ha emission, we study the slope of the main sequence (MS) of local star-forming galaxies at stellar masses larger than 10(10)M(circle dot). The slope of the relation strongly depends on the SFR indicator used. In all cases, the local MS shows a bending at high stellar masses with respect to the slope obtained in the low-mass regime. While the distribution of galaxies in the upper envelope of the MS is consistent with a lognormal distribution, the lower envelope shows an excess of galaxies, which increases as a function of the stellar mass but varies as a function of the SFR indicator used. The scatter of the best lognormal distribution increases with stellar mass from similar to 0.3 dex at 10(10)M(circle dot) to similar to 0.45 at 10(11)M(circle dot). The MS high-mass end is dominated by central galaxies of group-sized haloes with a red bulge and a disc redder than the lower mass counterparts. We argue that the MS bending in this region is due to two processes: (i) the formation of a bulge component as a consequence of the increased merger activity in groups, and (ii) the cold gas starvation induced by the hot halo environment, which cuts off the gas inflow on to the disc. Similarly, the increase of the MS scatter at high stellar masses would be explained by the larger spread of star formation histories of central group and cluster galaxies with respect to lower mass systems.

引用

页码：3213 / 3226

页数：14

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