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Two-micron spectrophotometry of the galaxy NGC 253

Wynn-Williams, C. G. and Becklin, E. E. and Matthews, K. and Neugebauer, G. (1979) Two-micron spectrophotometry of the galaxy NGC 253. Monthly Notices of the Royal Astronomical Society, 189 (2). pp. 163-169. ISSN 0035-8711. doi:10.1093/mnras/189.2.163.

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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.

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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.
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NASANGL 05-002-207
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Official Citation:C. G. Wynn-Williams, E. E. Becklin, K. Matthews, G. Neugebauer, Two-micron spectrophotometry of the galaxy NGC 253, Monthly Notices of the Royal Astronomical Society, Volume 189, Issue 2, November 1979, Pages 163–169,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104469
Deposited By: Tony Diaz
Deposited On:21 Jul 2020 15:53
Last Modified:16 Nov 2021 18:32

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