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Published 2003 | Submitted
Book Section - Chapter Open

Mg II/CIV Kinematics vs. Stellar Kinematics in Galaxies

Abstract

Comparisons of the kinematics of MgII 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 are dynamically coupled to the stellar matter. A strong correlation exists between the overall kinematic spread of MgII absorbing gas and CIV 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 galaxies in our sample are few in number, there are no clear examples that suggest the gas is accreting/infalling isotropically about the galaxies from the intergalactic medium.

Additional Information

© 2003 Springer Science+Business Media Dordrecht. Supported in part by NASA NAG5 6399, NSF AST 95-96229 and AST 00-70773, HST GO 08672.01-A, GO 05984.01-94A, and GO 06577.01-95A, and the David & Lucile Packard Foundation. We also thank K. Adelberger, J. Charlton, M. Dickinson, B. Jannuzi, J. Maserio, M. Pettini, J. Rigby, A. Shapley, and S. Vogt.

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