We present a study of extended galaxy halo gas through H I and O VI absorption over two decades in projected distance at z \approx 0.2 .
The study is based on a sample of 95 galaxies from a highly complete ( > 80 \% ) survey of faint galaxies ( L > 0.1 L _ { * } ) with archival quasar absorption spectra and 53 galaxies from the literature .
A clear anti-correlation is found between H I ( O VI ) column density and virial radius normalized projected distance , d / R _ { h } .
Strong H I ( O VI ) absorption systems with column densities greater than 10 ^ { 14.0 } ( 10 ^ { 13.5 } ) cm ^ { -2 } are found for 48 of 54 ( 36 of 42 ) galaxies at d < R _ { h } indicating a mean covering fraction of \langle \kappa _ { H I } \rangle = 0.89 ( \langle \kappa _ { O VI } \rangle = 0.86 ) .
O VI absorbers are found at d \approx R _ { h } , beyond the extent observed for lower ionization species .
At d / R _ { h } = 1 - 3 strong H I ( O VI ) absorption systems are found for only 7 of 43 ( 5 of 34 ) galaxies ( \langle \kappa _ { H I } \rangle = 0.16 and \langle \kappa _ { O VI } \rangle = 0.15 ) .
Beyond d = 3 R _ { h } , the H I and O VI covering fractions decrease to levels consistent with coincidental systems .
The high completeness of the galaxy survey enables an investigation of environmental dependence of extended gas properties .
Galaxies with nearby neighbors exhibit a modest increase in O VI covering fraction at d > R _ { h } compared to isolated galaxies ( \kappa _ { OVI } \approx 0.13 versus 0.04 ) but no excess H I absorption .
These findings suggest that environmental effects play a role in distributing heavy elements beyond the enriched gaseous halos of individual galaxies .
Finally , we find that differential H I and O VI absorption between early- and late-type galaxies continues from d < R _ { h } to d \approx 3 R _ { h } .