The Physical Nature of Weak MgII Quasar Absorption Line Systems.

Details The Physical Nature of Weak MgII Quasar Absorption Line Systems. The Physical Nature of Weak MgII Quasar Absorption Line Systems.

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.7204n&link_type=abstract

American Astronomical Society, AAS Meeting #211, #72.04; Bulletin of the American Astronomical Society, Vol. 39, p.863

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In a span of four decades, quasar absorption line spectroscopy has emerged as one of the most efficient methods for probing HI gas and associated metals in a wide range of environments, from redshifts corresponding to the most distant quasars up to the present. The connection between strong MgII quasar absorption systems and the disks/halos of galaxies of various morphologies is fairly well established. In contrast, the physical nature of weak MgII absorbers is not sufficiently understood. In this talk, I will present results from my dissertation work, which is a study of weak MgII quasar absorption line systems at 01), could be gas clouds in the extended halos of galaxies, analogous to the Milky Way high velocity clouds. The gas might correspond to material expelled from rapidly star-forming galaxies in correlated supernova events. Some fraction of the population of weak MgII clouds can also arise along sight lines that intercept tidally stripped interstellar gas, residing in circumgalactic environments. The `iron-rich’ weak MgII clouds, which are prevalent at lower redshifts (z<1), must be tracing Type Ia enriched gas in sites that have been previously enriched by star formation, most likely in dwarf galaxies. These scenarios will be reviewed in my presentation.
This work is supported by NSF. I thankfully acknowledge the Zaccheus Daniel Foundation and Sigma Xi for providing generous travel support.

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