The Properties of Highly Ionized High Velocity Gas in the Distant Galactic Corona and Local Group

Details The Properties of Highly Ionized High Velocity Gas in the Distant Galactic Corona and Local Group The Properties of Highly Ionized High Velocity Gas in the Distant Galactic Corona and Local Group

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9802s&link_type=abstract

HST Proposal ID #9802

Computer Science

Hst Proposal Id #9802 Ism And Circumstellar Matter

Scientific paper

We propose to observe two bright AGNs {NGC7469 and Mrk 335} with the E140M grating of STIS to study the properties of highly ionized high velocity O VI absorption systems associated with the Magellanic Stream and several Local Group clouds. Unlike most high velocity cloud studies, we know that these absorbers are located at large distances from the Sun. The observations will allow us to perform detailed studies of the ionization properties of the O VI absorbers and discriminate between competing models for the production of the highly ionized gas. We will analyze the component velocity structure of the absorption to quantify the relationship of the highly ionized gas and the neutral gas in this region of the sky, and determine if the properties of the high velocity gas are consistent with an origin in interfaces between warm clouds and a low-density hot {T > 10^6 K} Galactic corona or Local Group medium. The results of this investigation are directly relevant to studies of high velocity clouds, the production of hot gas associated with galaxies, the intergalactic medium, and the formation and evolution of galaxies. Secondary science programs that will be undertaken with the proposed observations include a study of the Galactic halo, analysis of the intergalactic absorption along the sight lines, and an investigation of the intrinsic AGN absorption in NGC 7469.

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