# C IV absorbers tracing cool gas in dense galaxy group/cluster environments

## TL;DR

This study analyzes three H I-C IV absorption systems in galaxy group/cluster environments, revealing cool, diffuse, and metal-enriched gas possibly influenced by galaxy interactions, using HST/COS spectra.

## Contribution

First detailed analysis of H I-C IV absorbers in dense galaxy environments, linking absorption features to galaxy density and enrichment processes.

## Key findings

- Absorbers are consistent with cool, photoionized gas at T < 4x10^4 K.
- Detected galaxies within 1 Mpc indicating dense environments.
- One absorber shows super-solar metallicity at Virgo cluster outskirts.

## Abstract

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.