C IV absorbers tracing cool gas in dense galaxy group/cluster
  environments
  We present analysis on three intervening H I-C IV absorption systems tracing
gas within galaxy group/cluster environments, identified in the $HST$/COS
far-UV spectra of the background quasars PG $1148+549$ ($z_{abs}=0.00346$),
SBS~$1122+594$ ($z_{abs}=0.00402$) and RXJ~$1230.8+0115$ ($z_{abs}=0.00574$).
The ionization models are consistent with the origin of metal lines and H I
from a cool and diffuse photoionized gas phase with $T \lesssim 4 \times
10^{4}$ K and $n_{\mathrm{H}} \lesssim 5 \times 10^{-4}$ cm$^{-3}$. The three
absorbers have $89$, $51$ and $17$ galaxies detected within $1$ Mpc and
$|\Delta v| < 600$ km s$^{-1}$. The RXJ~$1230.8+0115$ sightline traces the
outskirt regions of the Virgo cluster where the absorber is found to have
super-solar metallicity. The detection of metal lines along with H I has
enabled us to confirm the presence of cool, diffuse gas possibly enriched by
outflows and tidal interactions in environments with significant galaxy
density.
