Hostname: page-component-77c89778f8-m42fx Total loading time: 0 Render date: 2024-07-21T22:19:01.688Z Has data issue: false hasContentIssue false
  • English
  • Français

Models for Infrared and Submillimetre Counts and Backgrounds

Published online by Cambridge University Press:  13 May 2016

Michael Rowan-Robinson
Michael Rowan-Robinson*
Affiliation:
Astrophysics Group, Blackett Laboratory, Imperial College of Science Technology and Medicine, Prince Consort Road, London SW7 2BZ

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A simple and versatile parametrized approach to the star formation history allows a quantitative investigation of the constraints from far infrared and submillimetre counts and background intensity measurements.

The models include four spectral components: infrared cirrus, an M 82-like starburst, an Arp 220-like starburst and an AGN dust torus. The 60 μm luminosity function is determined for each chosen rate of evolution using the PSCz redshift data for 15000 galaxies. The proportions of each spectral type as a function of 60 μm luminosity are chosen for consistency with IRAS and SCUBA colour-luminosity relations, and with the fraction of AGN as a function of luminosity found in 12 μm samples.

A good fit to the observed counts at 0.44, 2.2, 15, 60, 90, 175 and 850 μm can be found with pure luminosity evolution in all 3 cosmological models investigated: Ω0 = 1, Ω0 = 0.3 (Λ = 0), and Ω0 = 0.3, Λ = 0.7. All 3 models also give an acceptable fit to the integrated background spectrum. The total mass-density of stars generated in all 3 cosmological models is consistent with that observed.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 204: The Extragalactic Infrared Background and its Cosmological Implication , 2001 , pp. 265 - 280
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Barger, A. J., Cowie, L. L., & Sanders, D. B., 1999, ApJ, 518, L5 Google Scholar
Bruzual, A. G., & Chariot, S. 1993, ApJ, 405, 538 Google Scholar
Blain, A. W., et al. 1999a, MNRAS, 302, 632 Google Scholar
Blain, A. W., et al. 1999b, ApJ, 512, L87 Google Scholar
Blain, A., et al. 1999c, MNRAS, 309, 715 Google Scholar
Boyle, B. J., Shanks, T., & Peterson, B. A. 1988, MNRAS, 235, 935 Google Scholar
Dole, H., et al. 2000, in ESA SP-427, The Universe as seen by ISO, ed. Cox, P. & Kessler, M. F. (Paris: ESA Special Publications), 1031, astro-ph/0002283 Google Scholar
Dunne, L., et al. 2000, MNRAS, in press, astro-ph/0002234 Google Scholar
Dwek, E., et al. 1998, ApJ, 508, 106 Google Scholar
Eales, S., et al. 1999, ApJ, 515, 518 Google Scholar
Efstathiou, A., Rowan-Robinson, M., & Siebenmorgen, R. 2000, MNRAS, 313, 734 Google Scholar
Elbaz, D., et al. 2000, A&A, in press, astro-ph/9910406 Google Scholar
Fixsen, D. J., et al. 1998, ApJ, 508, 123 Google Scholar
Flores, H., et al. 1999, ApJ, 517, 408 Google Scholar
Fox, M. J., et al. 2000, MNRAS, submitted.Google Scholar
Franceschini, A., et al. 1997, in The Far IR and Submillimetre Universe, ESA SP-401, 159 Google Scholar
Gregorich, D. T., et al. 1995, AJ, 110, 259 Google Scholar
Guiderdoni, B., et al. 1998, MNRAS, 295, 877 Google Scholar
Hacking, P. B., & Houck, J. 1987, ApJS, 63, 311 Google Scholar
Hauser, M. G., et al. 1998, ApJ, 508, 25 CrossRefGoogle Scholar
Hughes, D. H., et al. 1998, Nature, 394, 241 Google Scholar
Kawara, K., et al. 1998, A&A, in press.Google Scholar
Lanzetta, K. M., Yahil, A., & Fernandez-Soto, A. 1996, Nature, 381, 759 Google Scholar
Lilly, S. J., et al. 1996, ApJ, 460, L1 Google Scholar
Lonsdale, C. J., et al. 1990, ApJ, 358, 60 Google Scholar
Loveday, J., et al. 1992, ApJ, 390, 338 Google Scholar
McCracken, H. J., et al. 2000, MNRAS, in press, astro-ph/9904014 Google Scholar
Madau, P., et al. 1996, MNRAS, 283, 1388 Google Scholar
Metcalfe, N., Shanks, T., Fong, R., & Roche, N. 1995, MNRAS, 273, 257 Google Scholar
Meurer, G. R., et al. 1997, AJ, 114, 54 Google Scholar
Meurer, G. R., Heckman, T. M., & Calzetti, D. ApJ, 1999, 521, 64 Google Scholar
Oliver, S., et al. 1997, MNRAS, 289, 471 Google Scholar
Pearson, C., & Rowan-Robinson, M. 1996, MNRAS, 283, 174 Google Scholar
Pettini, M., et al. 1998, ApJ, 508, 539 CrossRefGoogle Scholar
Pozzetti, L., et al. 1998, MNRAS, 298, 1133 CrossRefGoogle Scholar
Puget, J.-L., et al. 1996, A&A, 308, 5 Google Scholar
Rigopoulou, D., Lawrence, A., & Rowan-Robinson, M. 1996, MNRAS, 288, 1049 CrossRefGoogle Scholar
Rowan-Robinson, M. 1995, MNRAS, 272, 737 Google Scholar
Rowan-Robinson, M., et al. 1997, MNRAS, 289, 490 CrossRefGoogle Scholar
Rush, B., Malkan, M. A., & Spinoglio, L., 1993, ApJS, 89, 1 CrossRefGoogle Scholar
Saunders, W., et al. 1990, MNRAS, 242, 318 Google Scholar
Serjeant, S., et al. 2000, MNRAS, 316, 738 Google Scholar
Smail, I., Ivison, R. J., & Blain, A. W. 1997, ApJ, 490, L5 Google Scholar
Steidel, C. C., et al. 1999, ApJ, 519, 1 Google Scholar
Verma, A., 2000, PhD thesis (Univ. of London).Google Scholar
Walker, T. P., et al. 1991, ApJ, 376, 51 Google Scholar
Xu, C., et al. 1998, ApJ, 508, 576 Google Scholar