Diffuse infrared emission from the galaxy. I - Solar neighborhood
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Abstract
A large-scale study of the infrared emission originating in the solar neighborhood, based on the analysis of IRAS data, is presented. Basic properties of the infrared emission from the interstellar medium are derived from this study. Away from heating sources and outside molecular clouds the infrared emission from the interstellar medium is well correlated with the column density of H I gas. This correlation proves that the interstellar radiation field and the dust abundance are roughly uniform on scales of the order of 100 pc. The origin of the infrared emission from the solar neighborhood is investigated. It is shown that stars younger than a few 108yr are responsible for two-thirds of the infrared emission from the solar neighborhood, but that most of this emission comes from interstellar matter not associated with current star formation. A study of the Orion region emphasizes this result. The authors show the existence of 12 and 25 μm emission form the Galaxy at |b| >10°, and demonstrate that this emission comes from dust heated by the average interstellar radiation field of the Galaxy. After subtraction of the zodiacal light and the Galactic emission the authors find at 100 μm a residual background in the range 1.2 - 1.8 MJy sr-1; they suggest several explanations for this emission.
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