Kinematics of the OVI Circumgalactic Medium: Halo Mass Dependence and
  Outflow Signatures
  We probe the high-ionization circumgalactic medium by examining absorber
kinematics, absorber-galaxy kinematics, and average absorption profiles of 31
OVI absorbers from the "Multiphase Galaxy Halos" Survey as a function of halo
mass, redshift, inclination, and azimuthal angle. The galaxies are isolated at
$0.12<z_{\rm gal}<0.66$ and are probed by a background quasar within $D\approx
200$ kpc. Each absorber-galaxy pair has Hubble Space Telescope images and COS
quasar spectra, and most galaxy redshifts have been accurately measured from
Keck/ESI spectra. Using the pixel-velocity two-point correlation function
(TPCF) method, we find that OVI absorber kinematics have a strong halo mass
dependence. Absorbers hosted by $\sim L^{\ast}$ galaxies have the largest
velocity dispersions, which we interpret to be that the halo virial temperature
closely matches the temperature at which the collisionally ionized OVI fraction
peaks. Lower mass galaxies and group environments have smaller velocity
dispersions. Total column densities follow the same behavior, consistent with
theoretical findings. After normalizing out the observed mass dependence, we
studied absorber-galaxy kinematics with a modified TPCF and found
non-virialized motions due to outflowing gas. Edge-on minor axis gas has large
optical depths concentrated near the galaxy systemic velocity as expected for
bipolar outflows, while face-on minor axis gas has a smoothly decreasing
optical depth distribution out to large normalized absorber-galaxy velocities,
suggestive of decelerating outflowing gas. Accreting gas signatures are not
observed due to "kinematic blurring" in which multiple line-of-sight structures
are observed. These results indicate that galaxy mass dominates OVI properties
over baryon cycle processes.
