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Mg II/CIV Kinematics vs. Stellar Kinematics in Galaxies

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Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 281))

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.

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© 2003 Springer Science+Business Media Dordrecht

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Churchill, C., Steidel, C. (2003). Mg II/CIV Kinematics vs. Stellar Kinematics in Galaxies. In: Rosenberg, J.L., Putman, M.E. (eds) The IGM/Galaxy Connection. Astrophysics and Space Science Library, vol 281. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0115-1_26

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  • DOI: https://doi.org/10.1007/978-94-010-0115-1_26

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-010-3978-9

  • Online ISBN: 978-94-010-0115-1

  • eBook Packages: Springer Book Archive

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