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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

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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 

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