The Smooth MgII gas distribution through the
  interstellar/extra-planar/halo interface
  We report the first measurements of MgII absorption systems associated with
spectroscopically confirmed z~0.1 star-forming galaxies at projected distances
of D<6kpc. We demonstrate the data are consistent with the well known
anti-correlation between rest-frame MgII equivalent width, Wr(2796), and impact
parameter, D, represented by a single log-linear relation derived by Nielsen et
al. (MAGIICAT) that converges to ~2A at D=0kpc. Incorporating MAGIICAT, we find
that the halo gas covering fraction is unity below D~25kpc. We also report that
our D<6kpc absorbers are consistent with the Wr(2796) distributions of the
Milky Way interstellar medium (ISM) and ISM+halo. In addition, quasar
sight-lines of intermediate redshift galaxies with 6<D<25kpc have an equivalent
width distribution similar to that of the Milky Way halo, implying that beyond
~6kpc, quasar sight-lines are likely probing halo gas and not the ISM. As
inferred by the Milky Way and our new data, the gas profiles of galaxies can be
fit by a single log-linear Wr(2796)-D relation out to large scales across a
variety of gas-phase conditions and is maintained through the
halo/extra-planar/ISM interfaces, which is remarkable considering their
kinematic complexity. These low redshift, small impact parameter absorption
systems are the first steps to bridge the gap between quasar absorption-line
studies and HI observations of the CGM.
