HerMES: dust attenuation and star formation activity in ultraviolet-selected samples from z ∼ 4 to ∼1.5

被引：104

作者：

Heinis, S. ^{[1
,2
]}

Buat, V. ^{[1
]}

Bethermin, M. ^{[3
,4
,5
]}

Bock, J. ^{[6
,7
]}

Burgarella, D. ^{[1
]}

Conley, A. ^{[8
]}

Cooray, A. ^{[6
,9
]}

Farrah, D. ^{[1
,10
]}

Ilbert, O.

Magdis, G. ^{[3
]}

Marsden, G. ^{[11
]}

Oliver, S. J. ^{[12
]}

Rigopoulou, D. ^{[13
,14
]}

Roehlly, Y. ^{[1
]}

Schulz, B. ^{[6
,15
]}

Symeonidis, M. ^{[12
,16
]}

Viero, M. ^{[6
]}

Xu, C. K. ^{[6
,15
]}

Zemcov, M. ^{[6
,7
]}

机构：

[1] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

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

[3] Univ Paris Diderot, CNRS, CEA DSM Irfu, Lab AIM Paris Saclay,CE Saclay, F-91191 Gif Sur Yvette, France

[4] Univ Paris 11, IAS, F-91405 Orsay, France

[5] CNRS, UMR 8617, F-91405 Orsay, France

[6] CALTECH, Pasadena, CA 91125 USA

[7] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[8] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA

[9] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[10] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA

[11] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

[12] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England

[13] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England

[14] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

[15] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA

[16] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 437卷 / 02期

关键词：

methods: statistical; galaxies: star formation; infrared: galaxies; ultraviolet: galaxies; INITIAL MASS FUNCTION; LYMAN BREAK GALAXIES; CHEMO-SPECTROPHOTOMETRIC EVOLUTION; FAR-INFRARED PROPERTIES; HIGH-REDSHIFT GALAXIES; FORMATION RATE DENSITY; UV-SELECTED GALAXIES; LESS-THAN; FORMING GALAXIES; STELLAR MASS;

D O I：

10.1093/mnras/stt1960

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the link between observed ultraviolet (UV) luminosity, stellar mass and dust attenuation within rest-frame UV-selected samples at z similar to 4, similar to 3 and similar to 1.5. We measure by stacking at 250, 350 and 500 mu m in the Herschel/Spectral and Photometric Imaging Receiver images from the Herschel Multi-Tiered Extragalactic Survey (HerMES) program the average infrared luminosity as a function of stellar mass and UV luminosity. We find that dust attenuation is mostly correlated with stellar mass. There is also a secondary dependence with UV luminosity: at a given UV luminosity, dust attenuation increases with stellar mass, while at a given stellar mass it decreases with UV luminosity. We provide new empirical recipes to correct for dust attenuation given the observed UV luminosity and the stellar mass. Our results also enable us to put new constraints on the average relation between star formation rate (SFR) and stellar mass at z similar to 4, similar to 3 and similar to 1.5. The SFR-stellar mass relations are well described by power laws (SFR proportional to M-*(0.7)), with the amplitudes being similar at z similar to 4 and similar to 3, and decreasing by a factor of 4 at z similar to 1.5 at a given stellar mass. We further investigate the evolution with redshift of the specific SFR. Our results are in the upper range of previous measurements, in particular at z similar to 3, and are consistent with a plateau at 3 < z < 4. Current model predictions (either analytic, semi-analytic or hydrodynamic) are inconsistent with these values, as they yield lower predictions than the observations in the redshift range we explore. We use these results to discuss the star formation histories of galaxies in the framework of the main sequence of star-forming galaxies. Our results suggest that galaxies at high redshift (2.5 < z < 4) stay around 1 Gyr on the main sequence. With decreasing redshift, this time increases such that z = 1 main-sequence galaxies with 10(8) < M-*/M-circle dot < 10(10) stay on the main sequence until z = 0.

引用

页码：1268 / 1283

页数：16

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