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Gas in the Nucleus and Disk of M31

Published online by Cambridge University Press:  14 August 2015

Vera C. Rubin  and
W. Kent Ford Jr.
Vera C. Rubin
Affiliation:
Dept. of Terrestrial Magnetism, Carnegie Institution of Washington
W. Kent Ford Jr.
Affiliation:
Dept. of Terrestrial Magnetism, Carnegie Institution of Washington

Abstract

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Image tube spectra of emission regions in M31 have been studied to determine relative line strengths and abundances. Lines of H, He, [NII], [SII], [Oi], [Oii], [Oiii] are observed. The analysis indicates: (1) that there are ions whose line strengths, relative to Hα, are a function of the position of the emission region in M31; (2) abundance differences or different excitation mechanisms exist in regions separated by only a few hundred parsecs.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 44: External Galaxies and Quasi-Stellar Objects , 1972 , pp. 49 - 55
Copyright
Copyright © Reidel 1972 

References

Baade, W.: 1963, Evolution of Stars and Galaxies, Harvard University Press, Cambridge, p. 59.CrossRefGoogle Scholar
Baade, W. and Arp, H. C.: 1964, Astrophys. J. 139, 1027.CrossRefGoogle Scholar
Minkowski, R.: 1942, Astrophys. J. 96, 199.CrossRefGoogle Scholar
Parker, R. A. R.: 1964, Astrophys. J. 139, 493.CrossRefGoogle Scholar
Peimbert, M.: 1968, Astrophys. J. 154, 33.CrossRefGoogle Scholar
Peimbert, M. and Costero, R.: 1969, Bol. Obs. Tonantzintla Tacubaya 5, 3.Google Scholar
Rubin, V. C. and Ford, W. K. Jr.: 1970, Astrophys. J. 159, 379.CrossRefGoogle Scholar
Seaton, M. J.: 1960, Rep. Prog. Phys. 23, 313.CrossRefGoogle Scholar
Woltjer, L.: 1958, Bull. Astron. Inst. Neth. 14, 39.Google Scholar