The Influence of Interactions and Minor Mergers on the Structure of Galactic Disks: II. Results and Interpretations

Details The Influence of Interactions and Minor Mergers on the Structure of Galactic Disks: II. Results and Interpretations The Influence of Interactions and Minor Mergers on the Structure of Galactic Disks: II. Results and Interpretations

2000-07-08

arxiv.org/abs/astro-ph/0007104v1

Astronomy and Astrophysics

Astrophysics

LaTeX, 16 pages, 7 figures, accepted for publication in A&A, complete series of papers incl. all figures in high quality avail

Scientific paper

We present the second part of a detailed statistical study focussed on the effects of tidal interactions and minor mergers on the radial and vertical disk structure of spiral galaxies. In the first part we reported on the sample selection, observations, and applied disk models. In this paper the results are presented, based on disk parameters derived from a sample of 110 highly-inclined/edge-on galaxies. This sample consists of two subsamples of 49 interacting/merging and 61 non-interacting galaxies. Additionally, 41 of these galaxies were observed in the NIR. We find significant changes of the disk structure in vertical direction, resulting in ~1.5 times larger scale heights and thus vertical velocity dispersions. The radial disk structure, characterized by the cut-off radius and the scale length, shows no statistically significant changes. Thus, the ratio of radial to vertical scale parameters, h/z0, is ~1.7 times smaller for the sample of interacting/merging galaxies. The total lack of typical flat disk ratios (h/z0)>7 in the latter sample implies that vertical disk heating is most efficient for (extremely) thin disks. Statistically nearly all galactic disks in the sample (93%) possess non-isothermal vertical luminosity profiles like the sech (60%) and exp (33%) distribution, independent of the sample and passband investigated. This indicates that, in spite of tidal perturbations and disk thickening, the initial vertical distribution of disk stars is not destroyed by interactions or minor mergers.

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