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We present an absorption line study of the physical and chemical propertiesof the Leo HI Ring and the Leo I Group as traced by 11 quasar sightlines spreadover a 600 kpc X 800 kpc region. Using HST/COS G130/G160 archival observationsas constraints, we couple cloud-by-cloud, multiphase, Bayesian ionizationmodeling with galaxy property information to determine the plausible origin ofthe absorbing gas along these sightlines. We search for absorption in the range600 km/s - 1400 km/s consistent with the kinematics of the Leo Ring/Group. Wefind absorption plausibly associated with the Leo Ring towards five sightlines.Along three other sightlines, we find absorption likely to be associated withindividual galaxies, intragroup gas, and/or large-scale filamentary structure.The absorption along these five sightlines is stronger in metal lines thanexpected from individual galaxies, indicative of multiple contributions, and ofthe complex kinematics of the region. We also identify three sightlines withina 7-degree X 6-degree field around the Leo Ring, along which we do not find anyabsorption. We find that the metallicities associated with the Leo Ring aregenerally high, with values between solar and several times solar. The inferredhigh metallicities are consistent with the origin of the ring as tidal debrisfrom a major galaxy merger.

Probing the physicochemical properties of the Leo Ring and the Leo I group