The Relative Kinematics of Gaseous Halos Around z=0.1 Galaxies

Details The Relative Kinematics of Gaseous Halos Around z=0.1 Galaxies The Relative Kinematics of Gaseous Halos Around z=0.1 Galaxies

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21535804k&link_type=abstract

American Astronomical Society, AAS Meeting #215, #358.04; Bulletin of the American Astronomical Society, Vol. 42, p.542

Astronomy and Astrophysics

Astronomy

Scientific paper

We present new results of a kinematic study of an unbiased volume-limited sample of z˜0.1 MgII absorption selected galaxies. We have obtained detailed halo gas and galaxy kinematics for six systems. MgII absorption has been detected in background quasar spectra using the LRIS-B spectrograph on the Keck telescope [EW(2796)>3 Angstroms]. Moderate resolution, spatially resolved galaxy spectra were obtained using the DIS spectrograph on the Apache Point Observatory 3.5m telescope. From these spectra we have derived accurate galaxy redshifts relative to the absorption systems along with their rotations curves. We find that all six of the absorption systems reside to one side of the galaxy systemic velocity, similar to those observed at z˜0.6. In all cases, a rotating thick-disk model cannot reproduce the full spread of observed MgII absorption velocities. Combined with the knowledge of the star formation rates and environments, even if some of the absorbing gas arises from a thick disk some additional dynamical processes (infall/outflow) must be invoked to explain the full range of halo gas absorption velocities.

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