A Fast Bar in the Post-Interaction Galaxy NGC 1023
Astrophysics
2009-11-07 v1
Abstract
We measured the bar pattern speed, , of the SB0 galaxy NGC 1023 using the Tremaine-Weinberg (1984) method with stellar-absorption slit spectroscopy. The morphology and kinematics of the \hi gas outside NGC 1023 suggest it suffered a tidal interaction, sometime in the past, with one of its dwarf companions. At present, however, the optical disc is relaxed. If the disc had been stabilized by a massive dark matter halo and formed its bar in the interaction, then the bar would have to be slow. We found \kmsa, so that the bar ends near its co-rotation radius. It is therefore rotating rapidly and must have a maximum disc.
Cite
@article{arxiv.astro-ph/0112288,
title = {A Fast Bar in the Post-Interaction Galaxy NGC 1023},
author = {Victor P. Debattista and Enrico Maria Corsini and J. A. L. Aguerri},
journal= {arXiv preprint arXiv:astro-ph/0112288},
year = {2009}
}
Comments
13 pages, 10 figures. Accepted for publication at MNRAS