Blain, A. W. and Phillips, T. G. (2002) The 60-μm extragalactic background radiation intensity, dust-enshrouded active galactic nuclei and the assembly of groups and clusters of galaxies. Monthly Notices of the Royal Astronomical Society, 333 (1). pp. 222-230. ISSN 0035-8711. doi:10.1046/j.1365-8711.2002.05398.x. https://resolver.caltech.edu/CaltechAUTHORS:20180404-071358526
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Abstract
Submillimetre- (submm-) wave observations have revealed a cosmologically significant population of high-redshift dust-enshrouded galaxies. The form of evolution inferred for this population can be reconciled easily with COBE FIRAS and DIRBE measurements of the cosmic background radiation (CBR) intensity at wavelengths longer than ~100 μm. At shorter wavelengths, however, the 60-μm CBR intensity reported by Finkbeiner, Davis & Schlegel is less easily accounted for. Lagache et al. have proposed that this excess CBR emission is a warm Galactic component, and the detection of the highest-energy γ-rays from blazars limits the CBR intensity at these wavelengths, but here we investigate possible sources of this excess CBR emission, assuming that it has a genuine extragalactic origin. We propose and test three explanations, each involving additional populations of luminous, evolving galaxies not readily detected in existing submm-wave surveys. First, an additional population of dust-enshrouded galaxies with hot dust temperatures, perhaps dust-enshrouded, Compton-thick active galactic nuclei (AGN) as suggested by recent deep Chandra surveys. Secondly, a population of dusty galaxies with temperatures more typical of the existing submm-selected galaxies, but at relatively low redshifts. These could plausibly be associated with the assembly of groups and clusters of galaxies. Thirdly, a population of low-luminosity, cool, quiescent spiral galaxies. Hot AGN sources and the assembly of galaxy groups can account for the excess 60-μm background. There are significant problems with the cluster assembly scenario, in which too many bright 60-μm IRAS sources are predicted. Spiral galaxies have the wrong spectral energy distributions to account for the excess. Future wide-field far-infrared (IR) surveys at wavelengths of 70 and 250 μm using the SIRTF and Herschel space missions will sample representative volumes of the distant Universe, allowing any hot population of dusty AGNs and forming groups to be detected.
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| Additional Information: | © 2002 RAS. Accepted 2002 February 4. Received 2002 January 25; in original form 2001 April 11. Published: 11 June 2002. We thank Doug Finkbeiner, for discussing his CBR intensity estimates prior to publication, Ian Smail for an insightful referee's report, and Kate Quirk and Neal Trentham for helpful comments on the manuscript. In Cambridge, AWB was supported by the Raymond and Beverly Sackler Foundation as part of the Foundation's Deep Sky Initiative Programme at the IoA. TGP acknowledges the support of NSF through grant no AST 9980846 to the Caltech Submillimeter Observatory (CSO). | |||||||||
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| Subject Keywords: | galaxies: evolution – galaxies: formation – cosmology: observations – cosmology: theory – diffuse radiation – infrared: galaxies | |||||||||
| Issue or Number: | 1 | |||||||||
| DOI: | 10.1046/j.1365-8711.2002.05398.x | |||||||||
| Record Number: | CaltechAUTHORS:20180404-071358526 | |||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20180404-071358526 | |||||||||
| Official Citation: | A. W. Blain, T. G. Phillips; The 60-μm extragalactic background radiation intensity, dust-enshrouded active galactic nuclei and the assembly of groups and clusters of galaxies, Monthly Notices of the Royal Astronomical Society, Volume 333, Issue 1, 11 June 2002, Pages 222–230, https://doi.org/10.1046/j.1365-8711.2002.05398.x | |||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | |||||||||
| ID Code: | 85584 | |||||||||
| Collection: | CaltechAUTHORS | |||||||||
| Deposited By: | Tony Diaz | |||||||||
| Deposited On: | 04 Apr 2018 17:08 | |||||||||
| Last Modified: | 15 Nov 2021 20:30 |
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