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Interacting Nuclei in Distant Galaxies

Published online by Cambridge University Press:  12 April 2016

Wei Zheng  and
Steven A. Grandi
Wei Zheng
Affiliation:
University of Alabama, U.S.A.
Steven A. Grandi
Affiliation:
National Optical Astronomy Observatories, U. S. A.

Extract

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The interaction of galaxies not only occurs in galactic scales, but also may be linked to the binary cores in active galactic galaxies. The presence of a binary in the center of galaxies was suggested by Begelman, Blandford and Rees (1980). Gaskell (1983) suggests that supermassive binaries may account for the observed structure of emission line profiles such as double peaks displaced by a significant velocity difference. Collin-Souffrin, et al. (1986) argue that line emission may be formed in the outer part of an accretion disk. The resultant profile, as expected from rotational motion, would be very broad and often possess a double-horn shape. However, the emission line profiles in most active galactic nuclei do not share such a resemblance, and there are only two reported cases, 3C390.3 (Pérez et al. 1987) and Arp102B (Chen, Halpern and Filippenko 1989), in which the broad Balmer line profile may be of such a shape. Therefore, the assumption for accretion disk is to be verified with care.

Type
III. Observations of Related Objects
Information
International Astronomical Union Colloquium , Volume 124: Paired and Interacting Galaxies , 1990 , pp. 251 - 253
Copyright
Copyright © NASA 1990

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