HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

被引：182

作者：

Oliver, S. J. ^{[1
]}

Wang, L. ^{[1
]}

Smith, A. J. ^{[1
]}

Altieri, B. ^{[2
]}

Amblard, A. ^{[3
]}

Arumugam, V. ^{[4
]}

Auld, R. ^{[5
]}

Aussel, H. ^{[6
]}

Babbedge, T. ^{[7
]}

Blain, A.

Bock, J. ^{[9
]}

Boselli, A. ^{[10
]}

Buat, V. ^{[10
]}

Burgarella, D. ^{[10
]}

Castro-Rodriguez, N. ^{[11
,12
]}

Cava, A. ^{[11
,12
]}

Chanial, P. ^{[7
]}

Clements, D. L. ^{[7
]}

Conley, A. ^{[13
]}

Conversi, L. ^{[2
]}

Cooray, A. ^{[3
]}

Dowell, C. D. ^{[9
]}

Dwek, E. ^{[14
]}

Eales, S. ^{[5
]}

Elbaz, D. ^{[6
]}

Fox, M. ^{[7
]}

Franceschini, A. ^{[15
]}

Gear, W. ^{[5
]}

Glenn, J. ^{[13
]}

Griffin, M. ^{[5
]}

Halpern, M. ^{[16
]}

Hatziminaoglou, E. ^{[17
]}

Ibar, E. ^{[18
]}

Isaak, K. ^{[5
]}

Ivison, R. J. ^{[4
,18
]}

Lagache, G. ^{[19
,20
]}

Levenson, L. ^{[9
]}

Lu, N. ^{[8
]}

Madden, S. ^{[6
]}

Maffei, B. ^{[21
]}

Mainetti, G. ^{[15
]}

Marchetti, L. ^{[15
]}

Mitchell-Wynne, K. ^{[3
]}

Mortier, A. M. J. ^{[7
]}

Nguyen, H. T. ^{[9
]}

O'Halloran, B. ^{[7
]}

Omont, A. ^{[22
]}

Page, M. J. ^{[23
]}

Panuzzo, P. ^{[6
]}

Papageorgiou, A. ^{[5
]}

机构：

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

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

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

[4] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

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

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

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

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

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

[10] Univ Aix marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France

[11] IAC, Tenerife 38200, Spain

[12] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain

[13] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[14] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA

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

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

[17] ESO, D-85748 Garching, Germany

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

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

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

[21] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[22] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

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

[24] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England

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

[26] Univ Oxford, Oxford OX1 3RH, England

[27] Univ Warwick, Warwick Syst Biol Ctr, Coventry CV4 7AL, W Midlands, England

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

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

galaxies: evolution; submillimeter: galaxies; surveys; STAR-FORMATION HISTORY; DEEP-FIELD-SOUTH; SUBMILLIMETER; MODEL; EVOLUTION; UNIVERSE; SPITZER; MAPS;

D O I：

10.1051/0004-6361/201014697

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to similar to 20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts < 100 mJy. We have directly resolved similar to 15% of the infrared extra-galactic background at the wavelength near where it peaks.

引用

页数：5

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