  We present observations of HI and OVI absorption systems proximate to a
galaxy at z_gal = 0.3529. The absorption was detected serendipitously in Cosmic
Origins Spectrograph observations of the low-z QSO J0943+0531 (z_qso = 0.564).
The data show two separate clouds along the sightline at an impact parameter of
95kpc from the galaxy. The first is likely low-metallicity gas falling onto the
galaxy. This assessment is based on the high velocity offset of the cloud from
the galaxy (delta_v = 365kms) and the weak metal line absorption, combined with
photoionization modeling. The second cloud, with only a modest velocity
separation from the galaxy (delta_v = 85kms), exhibits very strong OVI
absorption qualitatively similar to OVI absorption seen in the Milky Way halo.
Collisional ionization equilibrium models are ruled out by the metal line
column density ratios. Photoionization modeling implies a length-scale for the
OVI cloud of ~0.1-1.2Mpc, which indicates the absorbing gas most likely resides
within the local filamentary structure. This system emphasizes that kinematic
association alone is not sufficient to establish a physical connection to
galaxies, even at small impact parameters and velocity separations.
Observations such as these, connecting galaxies with their gaseous
environments, are becoming increasingly important for understanding galaxy
evolution and provide constraints for cosmological simulations.
