O VI Emission from the Magellanic Cloud System

Details O VI Emission from the Magellanic Cloud System O VI Emission from the Magellanic Cloud System

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1156..252s&link_type=abstract

THE LOCAL BUBBLE AND BEYOND II: Proceedings of the International Conference. AIP Conference Proceedings, Volume 1156, pp. 252-2

Physics

Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus, Supernova Remnants, X-Ray Sources, X-Ray Bursts, Galactic Center, Bar, Circumnuclear Matter, And Bulge

Scientific paper

We present O VI λ 1032 emission line measurements along several sight lines towards the Large Magellanic Cloud (LMC) and the Magellanic Interface region, obtained with the Far Ultraviolet Spectroscopic Explorer. The LMC targets include supernova remnants, superbubbles and diffuse interstellar regions. The observed O VI surface brightnesses form a near-continuous distribution spanning two-and-a-half orders of magnitude, with the diffuse gas at the faint end, and the strongly interacting supernova remnants at the bright end. The O VI emission detected from the Magellanic Interface region is evidence that the H I bearing gas is interacting with its surroundings. This, in turn, suggests that hot gas is present in the vicinity of the Magellanic Bridge, about 40 kpc away from the Galaxy.

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