HerMES: deep number counts at 250 μm, 350 μm and 500 μm in the COSMOS and GOODS-N fields and the build-up of the cosmic infrared background

被引：149

作者：

Bethermin, M. ^{[1
,2
,3
]}

Le Floc'h, E. ^{[1
]}

Ilbert, O. ^{[4
]}

Conley, A. ^{[5
]}

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

Amblard, A. ^{[6
]}

Arumugam, V. ^{[7
]}

Aussel, H. ^{[1
]}

Berta, S. ^{[8
]}

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

Boselli, A. ^{[4
]}

Buat, V. ^{[4
]}

Casey, C. M. ^{[11
]}

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

Cava, A. ^{[14
]}

Clements, D. L. ^{[15
]}

Cooray, A. ^{[9
,16
]}

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

Eales, S. ^{[17
]}

Farrah, D. ^{[18
]}

Franceschini, A. ^{[19
]}

Glenn, J. ^{[5
,20
]}

Griffin, M. ^{[17
]}

Hatziminaoglou, E. ^{[21
]}

Heinis, S. ^{[4
]}

Ibar, E. ^{[22
]}

Ivison, R. J. ^{[7
,22
]}

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

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

Magdis, G. ^{[1
]}

Marchetti, L. ^{[19
]}

Marsden, G. ^{[24
]}

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

O'Halloran, B. ^{[15
]}

Oliver, S. J. ^{[18
]}

Omont, A. ^{[25
]}

Page, M. J. ^{[26
]}

Panuzzo, P. ^{[1
]}

Papageorgiou, A. ^{[17
]}

Pearson, C. P. ^{[27
,28
]}

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

Pohlen, M. ^{[17
]}

Rigopoulou, D. ^{[27
,29
]}

Roseboom, I. G. ^{[7
,18
]}

Rowan-Robinson, M. ^{[15
]}

Salvato, M. ^{[30
,31
]}

Schulz, B. ^{[9
,32
]}

Scott, D. ^{[24
]}

Seymour, N. ^{[26
,33
]}

Shupe, D. L. ^{[9
,32
]}

机构：

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

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

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

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

[5] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA

[6] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

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

[8] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany

[9] CALTECH, Pasadena, CA 91125 USA

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

[11] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[12] IAC, Tenerife 38200, Spain

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

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

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

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

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

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

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

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

[21] ESO, D-85748 Garching, Germany

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

[23] Natl Opt Astron Observ, Tucson, AZ 85719 USA

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

[25] UPMC Univ Paris 6, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

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

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

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

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

[30] Max Planck Inst Plasma Phys, D-85748 Garching, Germany

[31] Excellence Cluster, D-85748 Garching, Germany

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

[33] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia

[34] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

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

[36] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa

来源：

ASTRONOMY & ASTROPHYSICS | 2012年 / 542卷

基金：

英国科学技术设施理事会;

关键词：

cosmology: observations; diffuse radiation; galaxies: statistics; galaxies: photometry; submillimeter: galaxies; submillimeter: diffuse background; HERSCHEL-SPIRE INSTRUMENT; LESS-THAN; 2; STAR-FORMATION; LUMINOSITY FUNCTION; DUSTY GALAXIES; SCUBA GALAXIES; SUBMILLIMETER; EVOLUTION; SPITZER; BLAST;

D O I：

10.1051/0004-6361/201118698

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The Spectral and Photometric Imaging REceiver (SPIRE) onboard the Herschel space telescope has provided confusion limited maps of deep fields at 250 mu m, 350 mu m, and 500 mu m, as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). Unfortunately, due to confusion, only a small fraction of the cosmic infrared background (CIB) can be resolved into individually-detected sources. Our goal is to produce deep galaxy number counts and redshift distributions below the confusion limit at SPIRE wavelengths (similar to 20 mJy), which we then use to place strong constraints on the origins of the cosmic infrared background and on models of galaxy evolution. Methods. We individually extracted the bright SPIRE sources (>20 mJy) in the COSMOS field with a method using the positions, the flux densities, and the redshifts of the 24 mu m sources as a prior, and derived the number counts and redshift distributions of the bright SPIRE sources. For fainter SPIRE sources (<20 mJy), we reconstructed the number counts and the redshift distribution below the confusion limit using the deep 24 mu m catalogs associated with photometric redshift and information provided by the stacking of these sources into the deep SPIRE maps of the GOODS-N and COSMOS fields. Finally, by integrating all these counts, we studied the contribution of the galaxies to the CIB as a function of their flux density and redshift. Results. Through stacking, we managed to reconstruct the source counts per redshift slice down to similar to 2 mJy in the three SPIRE bands, which lies about a factor 10 below the 5s confusion limit. Our measurements place tight constraints on source population models. None of the pre-existing models are able to reproduce our results at better than 3-sigma. Finally, we extrapolate our counts to zero flux density in order to derive an estimate of the total contribution of galaxies to the CIB, finding 10.1 (+2.6)(2.3) nW m(-2) sr(-1), 6.5 (+1.7)(1.6) nW m(-2) sr(-1), and 2.8 (+0.9)(0.8) nW m(-2) sr(-1) at 250 mu m, 350 mu m, and 500 mu m, respectively. These values agree well with FIRAS absolute measurements, suggesting our number counts and their extrapolation are sufficient to explain the CIB. We find that half of the CIB is emitted at z = 1.04, 1.20, and 1.25, respectively. Finally, combining our results with other works, we estimate the energy budget contained in the CIB between 8 mu m and 1000 mu m: 26(-3)(+7) nW m(-2) sr(-1).

引用

页数：23

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