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 .