Computer Science
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt........23d&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF TORONTO (CANADA), 1982.Source: Dissertation Abstracts International, Volume: 43-03, Section: B, pa
Computer Science
Scientific paper
We have observed a magnitude-limited sample of interacting and isolated field galaxies in the 21 cm line of HI with the NRAO 43 and 91 m telescopes and the Arecibo 305 m. The 21 cm data was combined with a homogeneous set of optical data on angular diameters, axial ratios, magnitudes and colours and integral properties were derived for galaxies in both samples. A subset of the interacting sample was partially mapped with the Arecibo telescope. Although the majority of interacting spirals obey, to first order, the scaling relations and type dependences determined for the isolated sample, systematic differences do exist between the two samples. The interacting sample has a higher population of galaxies with unusual log oH, log MH/LB and log MH/MT than the isolated sample. There are more high blue surface brightness galaxies in the interacting sample than the isolated sample. Interacting type 3 to 10 spirals are overluminous for their log MT values with respect to the isolated sample. The quantity log MH/LB decreases with increasing luminosity for the interacting galaxies, but is independent of luminosity for the isolated sample. For galaxies with comparable profile widths, the interacting type 3 to 10 spirals are overluminous with respect to the isolated galaxies. The interacting galaxies are both bluer and more scattered in the (U-B)(')T-B(B -V)(')T plane than the isolated galaxies in agreement with previous authors. The interacting sample has a higher fraction of Markarian and Seyfert galaxies than the isolated sample. Gas consumption time scales calculated from our HI data and the models of Larson and Tinsley (1978) show that some interacting galaxies have larger than average timescales. For the isolated galaxies good correlation exist between the (U-B)(')T and (B-V)(')T colours and log vo, log MH/MT and log MT/LB. These correlations are either more scattered or nonexistent for the isolated sample. The results are consistent with available models of galaxies undergoing star formation bursts and with the idea that some interacting systems possess extended HI haloes. The Arecibo mapping results, combined with existing data in the literature, show that extended HI distributions occur in > 25% of all systems.
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