Interaction and Emission Morphology
A simple comparison between broad V-band images and narrow band images tuned to the redshifted wavelength of Hα enables us to make a quick survey of the distribution of emission in galaxies. The appearance of interacting systems can then be contrasted with that of isolated objects. Those systems for which data are presently available seem to split into three classes: (i) nothing happening, despite apparent connections, (ii) emission distributed either smoothly or lumpily throughout, (iii) a central peak of emission in an otherwise smooth profile, for one or more of the galaxies. If this picture is confirmed by further observations, the next stage will be to try to distinguish the dynamical structures and possible gas flow patterns separating the different categories.
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- Keel, W.C., Kennicutt, R.C., Hummel, F. & van der Hulst, J.M. 1985. Astron.J., in press.Google Scholar