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arXiv · astro-ph/0405626

IRAC Observations of M81

S. P. Willner·M. L. N. Ashby·P. Barmby·G. G. Fazio·M. Pahre·H. A. Smith·R. C. Kennicutt, Jr.·D. Calzetti·D. A. Dale·B. T. Draine·M. W. Regan·S. Malhotra·M. D. Thornley·P. N. Appleton·D. Frayer·G. Helou·S. Stolovy·L. Storrie-Lombardi
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Abstract

IRAC images of M81 show three distinct morphological constituents: a smooth distribution of evolved stars with bulge, disk, and spiral arm components; a clumpy distribution of dust emission tracing the spiral arms; and a pointlike nuclear source. The bulge stellar colors are consistent with M-type giants, and the disk colors are consistent with a slightly younger population. The dust emission generally follows the blue and ultraviolet emission, but there are large areas that have dust emission without ultraviolet and smaller areas with ultraviolet but little dust emission. The former are presumably caused by extinction, and the latter may be due to cavities in the gas and dust created by supernova explosions. The nucleus appears fainter at 8 um than expected from ground-based 10 um observations made four years ago.

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S. P. Willner, M. L. N. Ashby, P. Barmby, G. G. Fazio, M. Pahre, H. A. Smith, R. C. Kennicutt, Jr., D. Calzetti, D. A. Dale, B. T. Draine, M. W. Regan, S. Malhotra, M. D. Thornley, P. N. Appleton, D. Frayer, G. Helou, S. Stolovy, L. Storrie-Lombardi. 2004-06-21. IRAC Observations of M81. https://doi.org/10.1086/422913

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