The Distribution of Disk-Halo H I Clouds in the Inner Milky Way

Details The Distribution of Disk-Halo H I Clouds in the Inner Milky Way The Distribution of Disk-Halo H I Clouds in the Inner Milky Way

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aspc..438..163f&link_type=abstract

The Dynamic Interstellar Medium: A Celebration of the Canadian Galactic Plane Survey. Proceedings of a conference held at the Na

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Using data from the Galactic All-Sky Survey, we have compared the properties and distribution of H I clouds in the disk-halo transition at the tangent points in mirror-symmetric regions of the first quadrant (QI) and fourth quadrant (QIV) of the Milky Way. Individual clouds are found to have identical properties in the two quadrants. However, there are three times as many clouds in QI as in QIV, their scale height is twice as large, and their radial distribution is more uniform. We attribute these major asymmetries to the formation of the clouds in the spiral arms of the Galaxy, and suggest that the clouds are related to star formation in the form of gas that has been lifted from the disk by superbubbles and stellar feedback, and fragments of shells that are falling back to the plane.

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