Herschel-ATLAS: Extragalactic number counts from 250 to 500 microns

被引：90

作者：

Clements, D. L. ^{[1
]}

Rigby, E. ^{[2
]}

Maddox, S. ^{[2
]}

Dunne, L. ^{[2
]}

Mortier, A. ^{[1
]}

Pearson, C. ^{[6
,7
]}

Amblard, A. ^{[4
]}

Auld, R. ^{[5
]}

Baes, M. ^{[8
]}

Bonfield, D. ^{[4
]}

Burgarella, D. ^{[9
]}

Buttiglione, S. ^{[10
]}

Cava, A. ^{[15
]}

Cooray, A. ^{[4
]}

Dariush, A. ^{[5
]}

de Zotti, G. ^{[10
]}

Dye, S. ^{[5
]}

Eales, S. ^{[5
]}

Frayer, D. ^{[17
]}

Fritz, J. ^{[8
]}

Gardner, Jonathan P. ^{[20
]}

Gonzalez-Nuevo, J. ^{[18
]}

Herranz, D. ^{[18
]}

Ibar, E. ^{[3
]}

Ivison, R. ^{[3
]}

Jarvis, M. J. ^{[11
]}

Lagache, G. ^{[23
,24
,25
]}

Leeuw, L. ^{[19
]}

Lopez-Caniego, M. ^{[18
]}

Negrello, M. ^{[12
]}

Pascale, E. ^{[5
]}

Pohlen, M. ^{[5
]}

Rodighiero, G. ^{[10
]}

Samui, S. ^{[13
]}

Serjeant, S. ^{[12
]}

Sibthorpe, B. ^{[3
]}

Scott, D. ^{[21
]}

Smith, D. J. B. ^{[5
]}

Temi, P. ^{[19
]}

Thompson, M. ^{[11
]}

Valtchanov, I. ^{[14
]}

van der Werf, P. ^{[22
]}

Verma, A. ^{[16
]}

机构：

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

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

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

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

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

[6] Rutherford Appleton Lab, SSTD, Didcot OX11 0QX, Oxon, England

[7] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada

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

[9] CNRS, UMR6110, Lab Astrophys Marseille, F-13388 Marseille, France

[10] Univ Padua, Dept Astron, I-35122 Padua, Italy

[11] Univ Hertfordshire, Sci & Technol Res Ctr, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

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

[13] Scuola Int Super Studi Avanzati, I-34151 Trieste, Italy

[14] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain

[15] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain

[16] Univ Oxford, Oxford Astrophys, Oxford OX1 3RH, England

[17] Natl Radio Astron Observ, Green Bank, WV 24944 USA

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

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

[20] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Astrophys Sci Div, Greenbelt, MD 20771 USA

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

[22] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[23] IAS, F-91405 Orsay, France

[24] CNRS, F-75700 Paris, France

[25] Univ Paris 11, Orsay, France

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

galaxies: evolution; galaxies: statistics; infrared: galaxies; submillimeter: galaxies; SUBMILLIMETER GALAXIES; STAR-FORMATION; SURVEY SHADES; SPITZER; PREDICTIONS; MODEL; EVOLUTION; UNIVERSE; FIELD; MAPS;

D O I：

10.1051/0004-6361/201014581

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The Herschel-ATLAS survey (H-ATLAS) will be the largest area survey to be undertaken by the Herschel Space Observatory. It will cover 550 sq. deg. of extragalactic sky at wavelengths of 100, 160, 250, 350 and 500 mu m when completed, reaching flux limits (5 sigma) from 32 to 145 mJy. We here present galaxy number counts obtained for SPIRE observations of the first similar to 14 sq. deg. observed at 250, 350 and 500 mu m. Methods. Number counts are a fundamental tool in constraining models of galaxy evolution. We use source catalogs extracted from the H-ATLAS maps as the basis for such an analysis. Correction factors for completeness and flux boosting are derived by applying our extraction method to model catalogs and then applied to the raw observational counts. Results. We find a steep rise in the number counts at flux levels of 100-200 mJy in all three SPIRE bands, consistent with results from BLAST. The counts are compared to a range of galaxy evolution models. None of the current models is an ideal fit to the data but all ascribe the steep rise to a population of luminous, rapidly evolving dusty galaxies at moderate to high redshift.

引用

页数：4

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