Computer Science
Scientific paper
Jan 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992phdt.........9x&link_type=abstract
PhD Dissertation, York Univ. Ontario Canada
Computer Science
1
Broadband, Interacting Galaxies, Seyfert Galaxies, Imaging Techniques, Color, Observation, Photometry, Occultation
Scientific paper
The nature of activity in Seyfert galaxies, the possible connection between interactions and/or mergers by companion galaxies, and distortions in the host galaxies and the effect of orientation on the classification of the different Seyfert types are studied observationally. If tidal interaction by a companion is the main cause of Seyfert activity, then how can the nuclear activity in isolated Seyfert galaxies be explained. V CCD surface photometry of eight isolated Seyfert galaxies is used in the first part of the thesis to search for a possible explanation. The observations reveal that all of the galaxies in the sample show either an internal perturbation in the form of bars, rings, etc. and/or an external distortion in the form of jets, plumes, etc. These types of asymmetries may be interpreted as the gross effects of past interactions with companion galaxies that have either merged with the host galaxy or escaped to large distances. Since the classification of Seyfert galaxies into type 1 and type 2, many models have been suggested to explain the differences between the types. Two of the models that have drawn much attention lately are the evolutionary model and the "Unified" model where viewing angle and dust obscuration cause one population to appear as multiple types. VRI CCD surface photometry of 27 Seyfert galaxies (8 Seyfert 1, 14 Seyfert 2 and 5 Intermediate types) is used in the second part of the thesis to examine possible differences in their broadband properties. This part of the work is an extension of the previous work to a larger sample of nearby Seyferts where the non-interaction criterion has been relaxed. The purpose is now also to test how present interactions are affecting the morphology of these galaxies. The results seem to support a common origin. Both Seyfert types occupy host galaxies representing almost the same Hubble classification while at the same time Seyfert 2 galaxies appear more inclined and redder. A strong separation of the two classes of Seyfert galaxies is readily apparent in the colour of the nuclear components. Seyfert 1 galaxies have bluer nuclei than Seyfert 2s. Both types have same disk colors. Intermediate type Seyfert galaxies have intermediate properties or properties closer to Seyfert 1s.
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