The Properties of Gaseous Halos Around Disk Galaxies

Details The Properties of Gaseous Halos Around Disk Galaxies The Properties of Gaseous Halos Around Disk Galaxies

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8186b&link_type=abstract

HST Proposal ID #8186

Computer Science

Hst Proposal Id #8186 Galaxy Structure And Dynamics

Scientific paper

Gaseous halos are key components in the structure and evolution of spiral galaxies and here we propose to advance our understanding of these phenomena through absorption line studies of the halo gas around the LMC and the edge-on galaxy NGC 891. In the LMC we will determine the spatial extent of the halo and the mass of highly ionized gas by measuring the CIV line strength against three bright background AGNs at different disk locations. For the edge-on system NGC 891, we will observe an AGN that we discovered whose sightline passes through the X-ray, radio, and HAlpha halos, only 5 kpc from the disk. By observing the Mg II and Fe II resonance absorption lines, we will measure the filling factor, density, and pressure of this halo material and determine the mass of gas that cools at this height above the disk.

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