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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

Béthermin, M. and Bock, J. and Cooray, A. and Dowell, C. D. and Levenson, L. and Nguyen, H. T. and Schulz, B. and Shupe, D. L. and Vieira, J. D. and Viero, M. and Xu, C. K. and Zemcov, M. (2012) 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. Astronomy and Astrophysics, 542 . Art. No. A58. ISSN 0004-6361. doi:10.1051/0004-6361/201118698.

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Aims. The Spectral and Photometric Imaging REceiver (SPIRE) onboard the Herschel space telescope has provided confusion limited maps of deep fields at 250 μm, 350 μm, and 500 μm, 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 (~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 μm 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 μm 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 ~2 mJy in the three SPIRE bands, which lies about a factor 10 below the 5σ 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-σ. 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_(-2.3)^(+2.6) nW m^(-2) sr^(-1), 6.5_(-1.6)^(+1.7) nW m^(-2) sr^(-1), and 2.8_(-0.8)^(+0.9) nW m^(-2) sr^(-1) at 250 μm, 350 μm, and 500 μm, 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 μm and 1000 μm: 26_(-3)^(+7) nW m^(-2) sr^(-1).

Item Type:Article
Related URLs:
URLURL TypeDescription
Béthermin, M.0000-0002-3915-2015
Bock, J.0000-0002-5710-5212
Cooray, A.0000-0002-3892-0190
Shupe, D. L.0000-0003-4401-0430
Xu, C. K.0000-0002-1588-6700
Zemcov, M.0000-0001-8253-1451
Additional Information:© 2012 ESO. Received 21 December 2011. Accepted 9 March 2012. Published online: 6 June 2012. We thank the COSMOS and GOODS teams for releasing publicly their data. Thanks to Georges Helou for suggesting that the distribution of the colors is more likely log-normal than normal. MB thank Hervé Dole for his advices about stacking, and Elizabeth Fernandez for providing a mock catalog from the Béthermin et al. model. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). MB acknowledge financial support from ERC-StG grant UPGAL 240039. SJO acknowledge support from the Science and Technology Facilities Council [grant number ST/F002858/1] and [grant number ST/I000976/1]. M.V. was supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (
Funding AgencyGrant Number
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
Science and Technology Facilities Council (STFC)ST/F002858/1
Science and Technology Facilities Council (STFC)ST/1000976/1
Agenzia Spaziale Italiana (ASI)I/005/07/0
Subject Keywords:cosmology: observations, diffuse radiation, galaxies: statistics, galaxies: photometry, submillimeter: galaxies, submillimeter: diffuse background
Record Number:CaltechAUTHORS:20120801-084702053
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Official Citation: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 A58 M. Béthermin, E. Le Floc’h, O. Ilbert, A. Conley, G. Lagache, A. Amblard, V. Arumugam, H. Aussel, S. Berta, J. Bock, et al. (51 more) Published online: 6 June 2012 DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:32827
Deposited By: Ruth Sustaita
Deposited On:01 Aug 2012 16:39
Last Modified:09 Nov 2021 21:30

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