Comparisons of the kinematics of Mg II absorbing gas and the stellar rotation curves in 0.5 < z < 1.0 spiral galaxies suggests that, at least in some cases, the extended gaseous envelopes may be dynamically coupled to the stellar matter. A strong correlation exists between the overall kinematic spread of Mg II absorbing gas and C IV absorption strength, and therefore kinematics of the higher-ionization gas. Taken together, the data may suggest a "halo/disk connection" between z~1 galaxies and their extended gaseous envelopes. Though the number of galaxies in our sample are few, there are no clear examples that suggest the gas is accreting/infalling isotropically about the galaxies from the intergalactic medium.
@article{arxiv.astro-ph/0209256,
title = {Mg II & C IV Kinematics vs. Stellar Kinematics in Galaxies},
author = {Chris Churchill and Chuck Steidel},
journal= {arXiv preprint arXiv:astro-ph/0209256},
year = {2016}
}
Comments
6 pages; 3 figures; to appear in the proceedings for "The IGM/Galaxy Connection" conference held in Boulder, Colorado, August 8-10, 2002