Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980afz....16..431s&link_type=abstract
(Astrofizika, vol. 16, July-Sept. 1980, p. 431-441.) Astrophysics, vol. 16, no. 3, Jan. 1981, p. 255-262. Translation.
Astronomy and Astrophysics
Astrophysics
3
Color, Galactic Structure, Galaxies, Interacting Galaxies, Star Formation, Abundance, Brightness, Elliptical Galaxies, Galactic Nuclei, Interstellar Gas, Quasars, Seyfert Galaxies, Spiral Galaxies
Scientific paper
A comparison is made between 208 galaxies in pairs and groups and isolated galaxies of the same morphological types on the basis of their positions on a two-color diagram. It is noted that the observed difference in the colors of the galaxies in pairs and groups can be explained by assuming that in some of them the rate of star formation is reduced but in others increased. The latter effect is especially noticeable in E, SO, and Ir II galaxies if their companions are brighter spirals. Attention is given to the connection between the relative abundance of gas in galaxies, the rate of star formation in them, and the activity of their nuclei. This connection is found to be especially pronounced in galaxies of early morphological types and in systems of the type Ir II, where the relative abundance of the gas component is appreciably higher than in normal galaxies. It is pointed out that such galaxies, as well as galaxies with ultraviolet excess, Seyfert-like objects, galaxies with emission lines, and quasars, which avoid regions occupied by rich clusters, are frequently found in pairs and groups.
Komberg Boris V.
Smirnov Mikhail A.
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