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DTSTART;TZID=US/Eastern:20130411T160000
DTEND;TZID=US/Eastern:20130411T170000
SUMMARY:Hot Gas in the Galactic Halo -- David Henley
DESCRIPTION:Departmental Colloquium. The Galactic halo, above and below the Galactic disk, is filled with gasat ~1-3 million K. This gas is a major contributor to the diffuse softX-ray background (SXRB) in directions looking out of the Galactic disk. Despite many years of study, the origin of the hot halo gas remainsuncertain. X-ray spectroscopy of the SXRB emission enables us todetermine the physical conditions in the hot gas, providing clues to itsorigin and evolution.We have recently completed a survey of the SXRB using data from the  orbiting XMM-Newton X-ray observatory. I will describe how we use the data from this survey to measure the halo's X-ray emission, and how we  are using these results to test physical models for the origin of thehot gas.
LOCATION:Physics Auditorium (202)
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