HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES

被引：153

作者：

Lapi, A. ^{[1
,2
]}

Gonzalez-Nuevo, J. ^{[2
]}

Fan, L. ^{[2
,3
]}

Bressan, A. ^{[2
,4
]}

De Zotti, G. ^{[2
,4
]}

Danese, L. ^{[2
]}

Negrello, M. ^{[5
]}

Dunne, L. ^{[6
]}

Eales, S. ^{[7
]}

Maddox, S. ^{[6
]}

Auld, R. ^{[7
]}

Baes, M. ^{[8
]}

Bonfield, D. G. ^{[9
]}

Buttiglione, S. ^{[4
]}

Cava, A. ^{[10
]}

Clements, D. L. ^{[11
]}

Cooray, A. ^{[12
]}

Dariush, A. ^{[7
,11
]}

Dye, S. ^{[7
]}

Fritz, J. ^{[8
]}

Herranz, D. ^{[13
]}

Hopwood, R. ^{[11
]}

Ibar, E. ^{[14
]}

Ivison, R. ^{[14
,15
]}

Jarvis, M. J. ^{[9
,16
]}

Kaviraj, S. ^{[7
]}

Lopez-Caniego, M. ^{[13
]}

Massardi, M. ^{[17
]}

Michallowski, M. J. ^{[15
]}

Pascale, E. ^{[7
]}

Pohlen, M. ^{[7
]}

Rigby, E. ^{[6
]}

Rodighiero, G. ^{[18
]}

Serjeant, S. ^{[5
]}

Smith, D. J. B. ^{[9
]}

Temi, P. ^{[19
]}

Wardlow, J. ^{[12
]}

van der Werf, P. ^{[20
]}

机构：

[1] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

[2] SISSA, Astrophys Sect, I-34136 Trieste, Italy

[3] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China

[4] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[5] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

[6] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

[7] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[8] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium

[9] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England

[10] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain

[11] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England

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

[13] Inst Fis Cantabria CSIC UC, Santander 39005, Spain

[14] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[15] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[16] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa

[17] INAF IRA, I-40129 Bologna, Italy

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

[19] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA

[20] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 742卷 / 01期

关键词：

galaxies: evolution; galaxies: formation; galaxies: high-redshift; submillimeter: galaxies; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; 250; MU-M; SUBMILLIMETER NUMBER COUNTS; FAR-INFRARED PROPERTIES; DARK-MATTER HALOS; STAR-FORMATION; STELLAR MASS; COSMIC EVOLUTION;

D O I：

10.1088/0004-637X/742/1/24

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Exploiting the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 mu m and at several redshifts z greater than or similar to 1, for bright submillimeter galaxies with star formation rates (SFRs) greater than or similar to 100 M-circle dot yr(-1). We find that the evolution of the comoving LF is strong up to z approximate to 2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of dust-enshrouded star formation in massive halos (M-H greater than or similar to 3 x 10(12) M-circle dot) amounts to similar to 7 x 10(8) yr. Given the SFRs, which are in the range of 10(2)-10(3) M-circle dot yr(-1), this timescale implies final stellar masses of the order of 10(11)-10(12) M-circle dot. The corresponding stellar mass function matches the observed mass function of passively evolving galaxies at z greater than or similar to 1. The comparison of the statistics for submillimeter and UV-selected galaxies suggests that the dust-free, UV bright phase is greater than or similar to 10(2) times shorter than the submillimeter bright phase, implying that the dust must form soon after the onset of star formation. Using a single reference spectral energy distribution (SED; the one of the z approximate to 2.3 galaxy SMM J2135-0102), our simple physical model is able to reproduce not only the LFs at different redshifts >1 but also the counts at wavelengths ranging from 250 mu m to approximate to 1 mm. Owing to the steepness of the counts and their relatively broad frequency range, this result suggests that the dispersion of submillimeter SEDs of z > 1 galaxies around the reference one is rather small.

引用

页数：21

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