Kinematics and Cloud to Cloud Abundance Ratios: A Rosetta Stone for Disk and Halo Components in Mg II Absorbers

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dc.creatorChurchill, Christopher W.
dc.creatorCharlton, Jane C.
dc.date1997-11-17
dc.date.accessioned2026-07-07T02:25:07Z
dc.date.available2026-07-07T02:25:07Z
dc.descriptionBased upon QSO absorption line studies, galaxies at 0.3 < z < 1.0 are seen to have extended gaseous "halos". When the absorption lines are observed at high resolution, the velocity distribution of the absorbing gas gives clues as to where this gas actually arises in and around the galaxies. Cloud to cloud abundance ratios provide further clues, given that the ionization conditions and chemical evolution histories of outer halos clouds, spiral disk clouds, and clouds in elliptical galaxies are different. The key to interpreting the high redshift data is the Milky Way galaxy, the absorption line "Rosetta stone."
dc.description3 pages; Latex; paspconf.sty; figures included; To appear in the Proceedings of the UC Santa Cruz Workshop on Galactic Halos (ed. D. Zaritsky)
dc.identifierhttps://arxiv.org/abs/astro-ph/9711181
dc.identifierhttp://arxiv.org/abs/astro-ph/9711181
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/11810
dc.subjectAstrophysics
dc.titleKinematics and Cloud to Cloud Abundance Ratios: A Rosetta Stone for Disk and Halo Components in Mg II Absorbers
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