Survey of O VI absorption in the Large Magellanic Cloud

Abstract

We present a survey of interstellar O VI absorption in the Large Magellanic Cloud (LMC) towards 70 lines of sight based on Far Ultraviolet Spectroscopic Explorer (FUSE) observations. The survey covers O VI absorption in a large number of objects in different environmental conditions of the LMC. Overall, a high abundance of O VI is present in active and inactive regions of the LMC with mean log[N(O VI)] = 14.23 atoms cm${}^{-2}$. There is no correlation observed between O VI absorption and emissions from the hot gas (X-ray surface brightness) or the warm gas (H${}_{\alpha }$ surface brightness). O VI absorption in the LMC is patchy and the properties are similar to that of the Milky Way (MW). In comparison to the Small Magellanic Cloud (SMC), O VI is lower in abundance even though SMC has a lower metallicity compared to the LMC and the MW. We present observations in 10 superbubbles of the LMC of which we detect O VI absorption in 5 superbubbles for the first time and the superbubbles show an excess O VI absorption of about 40% compared to non-superbubble lines of sight. We have also studied the properties of O VI absorption in the 30 Doradus region. Even though O VI does not show any correlation with X-ray emission for the LMC, a good correlation between log[N(O VI)] and X-ray surface brightness for 30 Doradus region is present. We also find that O VI abundance decreases with increasing distance from the star cluster R136.

25 pages, 9 figures. Accepted for publication in MNRAS

References in corpus (5)

• The Far Ultraviolet Spectroscopic Explorer Survey of OVI Absorption in the Disk of the Milky Way
• CalFUSE v3: A Data-Reduction Pipeline for the Far Ultraviolet Spectroscopic Explorer
• An Extended FUSE Survey of Diffuse O VI Emission in the Interstellar Medium
• Possible Detection of OVI from the LMC Superbubble N70
• Far Ultraviolet Diffuse Emission from the Large Magellanic Cloud

Cited by in corpus (8)

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• 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
• Mapping the Supernovae Driven Winds of the Large Magellanic Cloud in H$\alpha$ Emission I
• The Diffuse Ionized Gas of the Large Magellanic Cloud
• On the discrepancy between the X-ray and UV absorption measurements of OVI in the local ISM
• The distribution and kinematics of interstellar O~{\small VI} in the Milky Way}
• O~{\small VI} absorption in the Milky Way along the Large Magellanic Cloud lines of sight