HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

被引：98

作者：

Glenn, J. ^{[1
]}

Conley, A. ^{[1
]}

Bethermin, M. ^{[2
,3
]}

Altieri, B. ^{[4
]}

Amblard, A. ^{[5
]}

Arumugam, V. ^{[6
]}

Aussel, H. ^{[7
]}

Babbedge, T. ^{[8
]}

Blain, A. ^{[9
]}

Bock, J. ^{[9
,10
]}

Boselli, A. ^{[11
]}

Buat, V. ^{[11
]}

Castro-Rodriguez, N. ^{[12
,13
]}

Cava, A. ^{[12
,13
]}

Chanial, P. ^{[8
]}

Clements, D. L. ^{[8
]}

Conversi, L. ^{[4
]}

Cooray, A. ^{[5
,9
]}

Dowell, C. D. ^{[9
,10
]}

Dwek, E. ^{[14
]}

Eales, S. ^{[15
]}

Elbaz, D. ^{[7
]}

Ellsworth-Bowers, T. P. ^{[1
]}

Fox, M. ^{[8
]}

Franceschini, A. ^{[16
]}

Gear, W. ^{[15
]}

Griffin, M. ^{[15
]}

Halpern, M. ^{[17
]}

Hatziminaoglou, E. ^{[18
]}

Ibar, E. ^{[19
]}

Isaak, K. ^{[15
]}

Ivison, R. J. ^{[6
,19
]}

Lagache, G. ^{[2
,3
]}

Laurent, G. ^{[20
]}

Levenson, L. ^{[9
,10
]}

Lu, N. ^{[9
,21
]}

Madden, S. ^{[7
]}

Maffei, B. ^{[22
]}

Mainetti, G. ^{[16
]}

Marchetti, L. ^{[16
]}

Marsden, G. ^{[17
]}

Nguyen, H. T. ^{[9
,10
]}

O'Halloran, B. ^{[8
]}

Oliver, S. J. ^{[23
]}

Omont, A. ^{[24
]}

Page, M. J. ^{[25
]}

Panuzzo, P. ^{[7
]}

Papageorgiou, A. ^{[15
]}

Pearson, C. P. ^{[26
,27
]}

Perez-Fournon, I. ^{[12
,13
]}

机构：

[1] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[2] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France

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

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

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

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

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

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

[9] CALTECH, Pasadena, CA 91125 USA

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

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

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

[13] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain

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

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

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

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

[18] ESO, D-85748 Garching, Germany

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

[20] SW Res Inst, Boulder, CO 80302 USA

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

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

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

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

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

[26] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England

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

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 409卷 / 01期

关键词：

cosmology: observations; submillimetre: diffuse background; submillimetre: galaxies; FIELD; EVOLUTION;

D O I：

10.1111/j.1365-2966.2010.17781.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 mu m); parametrized galaxy number count models are derived to a depth of similar to 2 mJy beam(-1), approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam.

引用

页码：109 / 121

页数：13

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