We present observations of H i and O vi absorption systems proximate to a galaxy at z _ { \mbox { gal } } = 0.3529 .
The absorption was detected serendipitously in Cosmic Origins Spectrograph observations of the low- z QSO J 0943+0531 ( z _ { \mbox { qso } } = 0.564 ) .
The data show two separate clouds along the sightline at an impact parameter of 95 \mbox { kpc } 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 = 365 km s ^ { -1 } ) and the weak metal line absorption , combined with photoionization modeling .
The second cloud , with only a modest velocity separation from the galaxy ( \Delta v = 85 km s ^ { -1 } ) , exhibits very strong O vi absorption qualitatively similar to O vi 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 O vi cloud of \sim 0.1 - 1.2 \mbox { Mpc } , 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 of galaxy evolution and provide constraints for cosmological simulations .