Published November 1, 1979
| Published
Journal Article
Open
Two-micron spectrophotometry of the galaxy NGC 253
Chicago
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Abstract
A very strong Brackett-γ hydrogen emission line, and the 2.3-µm CO stellar absorption feature have been measured in NGC 253. The presence and strength of the CO feature indicates that late-type giant stars produce most of the 2 .2-µm continuum emission, while the rate of ionization implied by strength of the Brackett-γ line indicates that much, perhaps all, of the luminosity detected at far-infrared wavelengths originates from a large number of OB stars. As compared to the corresponding region of the Galaxy, the number of massive young stars in the central 200 pc of NGC 253 is 30 times greater, but the total mass of stars is roughly the same.
Additional Information
© 1979 Royal Astronomical Society. Provided by the NASA Astrophysics Data System. Received 1979 March 6; in original form 1979 January 16; Published: 01 November 1979. We thank the director and staff of the Cerro Tololo Observatory, especially C. Poblete, J. Rios, O. Saa, P. Schaller, R. Venegas and M. Zemelman. We also thank G. Forrester for his assistance at Caltech, and Brent Tully and Ian Gatley for discussions. This work was supported in part by NSF grant AST77-20516 and NASA grant NGL 05-002-207.Attached Files
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Additional details
- Eprint ID
- 104469
- Resolver ID
- CaltechAUTHORS:20200721-072029543
- NSF
- AST77-20516
- NASA
- NGL 05-002-207
- Created
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2020-07-21Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field