Possible Detection of OVI from the LMC Superbubble N70

Abstract

We present FUSE observations toward four stars in the LMC superbubble N70 and compare these spectra to those of four comparison targets located in nearby field and diffuse regions. The N70 sight lines show OVI 1032 absorption that is consistently stronger than the comparison sight lines by ~60%. We attribute the excess column density (logN_OVI=14.03 cm^-2) to hot gas within N70, potentially the first detection of OVI associated with a superbubble. In a survey of 12 LMC sight lines, Howk et al. (2002a) concluded that there was no correlation between ISM morphology and N_OVI. We present a reanalysis of their measurements combined with our own and find a clear difference between the superbubble and field samples. The five superbubbles probed to date with FUSE show a consistently higher mean N_OVI than the 12 non-superbubble sight lines, though both samples show equivalent scatter from halo variability. Possible ionization mechanisms for N70 are discussed, and we conclude that the observed OVI could be the product of thermal conduction at the interface between the hot, X-ray emitting gas inside the superbubble and the cooler, photoionized material making up the shell seen prominently in Halpha. We calculate the total hydrogen density n_H implied by our OVI measurements and find a value consistent with expectations. Finally, we discuss emission-line observations of OVI from N70.

arXiv comment9 pages in emulateapj style. Accepted to ApJ

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• HST/COS Observations of Ionized Gas Accretion at the Disk-halo Interface of M33
• Down-the-barrel and transverse observations of the Large Magellanic Cloud: evidence for a symmetrical galactic wind on the near and far sides of the galaxy
• The Surprisingly Constant Strength of O VI Absorbers over Cosmic Time
• Multi-frequency observations of a superbubble in the LMC: The case of LHA 120-N 70
• Survey of O VI absorption in the Large Magellanic Cloud
• The Dark Energy Camera Magellanic Clouds Emission-Line Survey
• Towards Resolving the Evolution of Multi-Supernova Superbubbles
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