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

A video summarizing the results of Sameer et al. (2022, MNRAS, 510, 5796)

Published onFeb 04, 2022
Probing the physicochemical properties of the Leo Ring and the Leo I group

This video presents an absorption line study by Sameer et al. (2022)[1] of the physical and chemical properties of the Leo HI Ring and the Leo I Group as traced by 11 quasar sightlines. Using HST/COS G130/G160 archival observations as constraints, we couple cloud-by-cloud, multiphase, Bayesian ionization modeling with galaxy property information to determine the plausible origin of the absorbing gas along these sightlines. We find absorption plausibly associated with the Leo Ring towards five sightlines. Along three other sightlines, we find absorption likely to be associated with individual galaxies, intragroup gas, and/or large scale filamentary structure. The absorption along these five sightlines is stronger in metal lines than expected from individual galaxies, indicative of multiple contributions, and of the complex kinematics of the region. We also identify three sightlines in the vicinity of the Leo Ring, along which we do not find any absorption. We find that the metallicities associated with the Leo Ring are generally high, with values between solar and several times solar. The inferred high metallicities are consistent with an origin of the ring as tidal debris from a major galaxy.

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