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IRAS observations of the nuclear bulge of M31
Soifer, B. T.; Rice, W. L.; Mould, J. R.; Gillett, F. C.; Rowan-Robinson, M.; Habing, H. J.
AA(California Institute of Technology, Pasadena), AB(California Institute of Technology, Pasadena), AC(California Institute of Technology, Pasadena), AD(Kitt Peak National Observatory, Tucson, AZ), AE(Queen Mary College, London, England)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 304, May 15, 1986, p. 651-656. Research supported by the Nederlands Instituut voor Vliegtuigontwikkeling en Ruimtevaart, NASA, SERC, and NSF. (ApJ Homepage)
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NASA/STI Keywords:
Andromeda Galaxy, Astronomical Spectroscopy, Galactic Bulge, Galactic Nuclei, Galactic Structure, Infrared Spectra, Spaceborne Astronomy, Spiral Galaxies, Cosmic Dust, Emission Spectra, Infrared Astronomy Satellite, Interstellar Gas, Late Stars, Stellar Envelopes, Stellar Mass Ejection
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IRAS observations of the nuclear bulge of M31 are reported. The 12-micron and 25-micron emission is attributed to circumstellar dust emission from late-type stars, while the 60 and 100-micron emission is attributed to interstellar dust emission. The total input rate of circumstellar gas and dust into the interstellar medium is estimated to be 0.015 solar masses/yr. The mass of dust in the interstellar medium estimated from the far-infared flux is about 1500 solar masses. The color temperature of the far-infrared-emitting dust is 45 K. The time required to accumulate the observed mass in interstellar dust is about 10 million yr. Either supernova-generated winds or star formation can deplete this gas without violating the observations.

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