Observations Of OVI Absorption In The Lmc: Superbubble Vs Non-superbubble Sight Lines

Details Observations Of OVI Absorption In The Lmc: Superbubble Vs Non-superbubble Sight Lines Observations Of OVI Absorption In The Lmc: Superbubble Vs Non-superbubble Sight Lines

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113809l&link_type=abstract

American Astronomical Society, AAS Meeting #211, #138.09; Bulletin of the American Astronomical Society, Vol. 39, p.985

Astronomy and Astrophysics

Astronomy

Scientific paper

Superbubbles (SBs) are nebulae formed by stellar winds and shock waves from young OB star associations. This superheated gas extends to scales > 50 pc and can be further energized by supernova explosions as the OB stars age and die. The OVI absorption line at 1032 A, in the midst of the FUSE bandpass, can in principle be used as a probe of the hot gas content (T = 10^5 - 10^6) of these structures, although the use of this diagnostic is complicated by a halo of OVI gas that surrounds the entire Large Magellanic Cloud (LMC).
In this work, we build on a pilot program on the SB N70 reported by Danforth & Blair (2006, ApJ, 646, 212), expanding the analysis to include the use of a more extensive group of FUSE observations now available in the FUSE archive. These observations allow us to compare the OVI content inside the SBs to that outside for at least 10 and perhaps as many as 16 SBs, using multiple sight lines both inside and outside the SBs. The observations can also be combined in a global sense, providing an overall comparison of sight lines within SBs to those that do not intersect SBs. We present a preliminary analysis of these sight lines and compare our findings to those of Howk et al. (2002, ApJ, 569, 214) and Danforth & Blair.

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