Abstract
Elliptical galaxies with dust lanes (Bertola and Galletta, 1978) are interpreted as the result of the acquisition of gaseous and dusty material. This material forms a disk by settling into the symmetry plane of the elliptical galaxy, if oblate or prolate (Tubbs, 1980; Simonson, 1982) or into one of the two permitted planes (defined by the major and intermediate axis and by the minor and intermediate axis) if the galaxy is triaxial and not tumbling (Steiman-Cameron, 1984). An inspection of the structure of the dust lanes in the ellipticals of the selected list published by Bertola (1987) indicates that we are looking at these disks almost edge-on, at an angle not exceeding 10°. This situation is the most favourable one for detecting the dust lane, since the region absorbed divides the galaxy into two parts which are absorption free. As soon as the viewing angle increases the contrast diminishes and the effect of the dust becomes less appreciable. In this case the best way to detect the acquired disk is to look at the elliptical galaxy through an interference filter centered on an emission line emitted by the gas component. Given the relatively high number of ellipticals with dust lanes (Sadler and Gerhard, 1985) it is therefore expected to detect acquired gaseous disks in the majority of ellipticals with emission lines. The purpose of this paper is to define and study the properties of these disks.
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© 1992 Springer Science+Business Media Dordrecht
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Bertola, F. (1992). Gaseous Disks in Elliptical Galaxies. In: Longo, G., Capaccioli, M., Busarello, G. (eds) Morphological and Physical Classification of Galaxies. Astrophysics and Space Science Library, vol 178. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-2522-2_9
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DOI: https://doi.org/10.1007/978-94-011-2522-2_9
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