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Growth of Galactic Bulges by Mergers: I. Dense Satellites | | J. A. L. Aguerri
; M. Balcells & R. F. Peletier
; | | Date: |
7 Dec 2000 | | Subject: | astro-ph | | Abstract: | Andredakis, Peletier & Balcells (1995) fit Sersic’s law $mu(r) sim r^{1/n}$ to the bulges of the Balcells & Peletier (1994) galaxy sample, and infer that $n$ drops with morphological type T from $n approx$ 4--6 for S0 to $n=1$ (exponential) for Sc’s. We use collisionless N body simulations to test the assumption that initially the surface brightness profiles of all bulges were exponential, and that the steepening of the profiles toward the early-types is due to satellite accretion. The results are positive. After the accretion of a satellite, bulge-disk fits show that the bulge grows and that the bulge profile index $n$ increases proportional to the satellite mass. For a satellite as massive as the bulge, $n$ rises from 1 to 4. We present kinematic diagnostics on the remnants and disk thickening. The latter suggests that the bulge growth must have occurred before the last formation of a thin disk in the galaxy. The thick disks created by the merger are reminiscent of thick disks seen in early-type edge-on galaxies. The efficiency of the process suggests that present day bulges of late-type spirals showing exponential profiles cannot have grown significantly by collisionless mergers. | | Source: | arXiv, astro-ph/0012156 | | Services: | Forum | Review | PDF | Favorites | |
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