Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-27T00:29:16.719Z Has data issue: false hasContentIssue false
  • English
  • Français

The Diffuse Near- and Mid-Infrared Emission from the Galaxy

Published online by Cambridge University Press:  13 May 2016

Martin Cohen
Martin Cohen*
Affiliation:
Radio Astronomy Laboratory, 601 Campbell Hall, University of California, Berkeley, CA 94720, USA

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.

Recognition of an isotropic cosmic near-infrared (NIR) and mid-infrared (MIR) background involves the removal of the zodiacal foreground (both scattered and reradiated), of the truly diffuse Galactic foreground (dominated by fluorescent bands of polcyclic aromatic hydrocarbons), and of resolved and unresolved Galactic point sources. I discuss model simulations of the near- and mid-infrared point source sky from which one can assess its particular contribution to the diffuse Galactic infrared foreground. I will also indicate the transitional stage which characterizes our knowledge of fundamental stellar parameters that are essential inputs to any such models. Using the latest version of the SKY model (Wainscoat et al. 1992; Cohen 1993; Cohen 1994; Cohen et al. 1994; Cohen 1995; Ruphy et al. 1997), I will demonstrate matches to deep point source counts for a variety of passbands and galactic latitudes, and will try to quantify the uncertainties achievable in model predictions of the integrated surface brightness due to the smearing of all these foreground point sources.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 204: The Extragalactic Infrared Background and its Cosmological Implication , 2001 , pp. 35 - 46
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Arendt, R. et al. 1998, ApJ, 508, 74 CrossRefGoogle Scholar
Burgdorf, M. et al. 2000, A&A, in press.Google Scholar
Chan, K.-W., Roellig, T. L., Onaka, T., Yamamura, I., & Tanabe, T. 1998, ApJ, 505, L31 Google Scholar
Cohen, M. 1993, AJ, 105, 1860 CrossRefGoogle Scholar
Cohen, M. 1994, AJ, 107, 582 Google Scholar
Cohen, M. 1995 ApJ, 444, 874 Google Scholar
Cohen, M., Sasseen, T., & Bowyer, S. 1994, ApJ, 427, 848 Google Scholar
Cohen, M., Walker, R. G., Carter, B., Hammersley, P. L., Kidger, M. R., & Noguchi, K. 1999, AJ, 117, 1864 Google Scholar
Egan, M. P. et al. 1999, The Midcourse Space Experiment Point Source Catalog Version 1.2 Explanatory Guide, Air Force Research Laboratory Technical Report, AFRL-VS-TR 1999-1522 Google Scholar
Garzón, F., Hammersley, P. L., Mahoney, T., Calbet, X., Selby, M. J., Hepburn, I., 1993, MNRAS, 264, 773 Google Scholar
Giard, M. 1989, A&A, 215, 92 Google Scholar
Gorjian, V., Wright, E. L., & Chary, R. 2000, ApJ, 536, 550 Google Scholar
Hall, P. B., Green, R. F., & Cohen, M. 1998, ApJS, 119, 1 Google Scholar
Hammersley, P. L. 1998, priv. comm.Google Scholar
Hammersley, P. L., Cohen, M., Garzón, F., Mahoney, T., & Lopez-Corredoira, M. 1999, MNRAS, 308, 333, 1999 Google Scholar
Kuemmel, M. W., & Wagner, S. J. 2000, A&A, 353, 867 Google Scholar
Meadows, V. S. 1994, Ph.D. thesis, Univ. of Sydney, Sydney, N.S.W, Australia.Google Scholar
Minezaki, T., Cohen, M., Kobayashi, Y., Yoshii, Y., & Peterson, B. A. 1998, AJ, 115, 229 CrossRefGoogle Scholar
Onaka, T., Yamamura, I., Tanabe, T., Roellig, T. L., & Yuen, L. 1996, PASJ, 48, 59 Google Scholar
Ristorcelli, I. et al. 1994, A&A, 286, L23 Google Scholar
Roellig, T. L., Onaka, T., McMahon, T. J., & Tanabe, T. 1994, ApJ, 428, 370 Google Scholar
Ruphy, S. R. et al. 1997, A&A, 326, 597 Google Scholar
Saracco, P. et al. 1997, AJ, 114, 887 Google Scholar
Vaisanen, P., Tollestrup, E., Willner, S. P., & Cohen, M. 2000, ApJ, 540, 593 Google Scholar
Wainscoat, R. J., Cohen, M., Volk, K., Walker, H. J. & Schwartz, D. E. 1992, ApJS, 83, 111 Google Scholar
Wright, E. L. & Reese, E. D. 2000, astro-ph/9912523 Google Scholar