3-D Structure of the ISM in the Magellanic Clouds

Details 3-D Structure of the ISM in the Magellanic Clouds 3-D Structure of the ISM in the Magellanic Clouds

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001noao.prop..272c&link_type=abstract

NOAO Proposal ID #2001B-0272

Computer Science

Scientific paper

The Magellanic Clouds (MCs) provide an excellent laboratory to study the multi-phase structure and the disk-halo connection of the interstellar medium (ISM). Recent surveys of the MCs have revealed the distribution of the molecular, neutral atomic H I, 10^4 K warm ionized, and 10^6 K hot ionized gas components in two dimensions. The hot ionized gas appears both inside large interstellar shells and in the field. Since hot ionized gas traces the energy feedback from massive stars and drives the evolution of the ISM, it is important to determine whether the hot gas is confined in the disk plane or distributed in a halo above the disk plane. Interstellar O VI absorption observations with the Far Ultraviolet Spectroscopic Explorer (FUSE) offer an opportunity to determine the location of the hot gas relative to the cooler gas components. We propose to obtain high-dispersion echelle observations of the H(alpha) line for the FUSE targets in the MCs. Comparisons between the O VI and H(alpha) velocities allow us to break the degeneracy along the line of sight and determine the 3-D structure of the multi-phase ISM in the MCs.

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