The Hot Gas Content of LMC Superbubble N70

Details The Hot Gas Content of LMC Superbubble N70 The Hot Gas Content of LMC Superbubble N70

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aspc..348..325d&link_type=abstract

Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE ASP Conference Series, Vol. 348, Proceedings of the Confe

Astronomy and Astrophysics

Astrophysics

Scientific paper

Superbubbles (SBs) are thought to form by the combined stellar winds of an OB association and supernovae shocks from their former members. These shocks, as well as thermal conduction, should produce a host of highly ionized species including O VI, N V, and C IV in the walls of the SB. Unfortunately, such ions are also found within the hot halos of galaxies in such quantities as to overwhelm the signature from hot SB gas.
In this project, we attempt to disentangle the halo and SB hot gas signatures by observing a bright SB at the eastern edge of the LMC. Sight lines through the periphery of the LMC halo should intersect a smaller pathlength of hot halo gas than those through the central regions of the galaxy and make detection of SB hot gas easier.

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