Infrared emission and star formation in the central regions of the galaxy IC 342
Abstract
The face-on Scd galaxy IC 342 has been studied at infrared wavelengths between 1.2 μm and 250 μm and at centimeter radio wavelengths. At 10 μm the nucleus is bright and extended on a scale of 200 pc, with a double structure unlike that of the stars seen at 2 μm. The infrared emission between 8 and 250 μm probably arises from heated dust grains in star formation regions in the disk of the galaxy. The radio emission comes from a region with many of the same spatial features as the 10 μm source; it appears to include both thermal and nonthermal sources. IC 342 is intermediate in luminosity between the Galaxy and NGC 253; the difference can probably be accounted for by a difference in the current rate of star formation at their centers.
Additional Information
© 1980. The American Astronomical Society. Received 1979 July 20; accepted 1979 September 10. We thank H. Ables for lending us a plate of IC 342, S. Beckwith and our night assistants, G. Tuton, J. Carrasco, and J. Frazier, for help with the ground-based observations, A. Harper, R. Loewenstein, and the members of the Kuiper Airborne Observatory for help with the aircraft observations, J. Shakeshaft for help with the radio observations, and M. Morris for bringing this object to our attention. This work was supported by NASA grants NGR 05-005-281, NGL 05-002-207, NASW 3159, and NSF grants AST 77-20516 and AST 7826028.Attached Files
Published - 1980ApJ___236__441B.pdf
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Additional details
- Eprint ID
- 75331
- Resolver ID
- CaltechAUTHORS:20170322-161717840
- NGR 05-005-281
- NASA
- NGL 05-002-207
- NASA
- NASW 3159
- NASA
- AST 77-20516
- NSF
- AST 78-26028
- NSF
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2017-03-23Created from EPrint's datestamp field
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2021-11-15Created from EPrint's last_modified field