[O~{\small VI} from the SBs of the LMC

TL;DR

This study measures O VI absorption in 10 superbubbles of the Large Magellanic Cloud, revealing significant variation and excess compared to non-superbubble regions, aiding understanding of hot gas in these structures.

Contribution

First detailed O VI absorption measurements in LMC superbubbles, showing variability and excess, enhancing knowledge of hot gas in stellar feedback regions.

Findings

O VI abundance varies across superbubbles

46% excess of O VI in SBs compared to non-SB lines

O VI column density varies by a factor of 2 to 2.5 within SBs

Abstract

We have presented the observations of O {\small VI} absorption at 1032 \AA\ towards 22 sightlines in 10 superbubbles (SBs) of the Large Magellanic Cloud (LMC) using the data obtained from the {\em Far Ultraviolet Spectroscopic Explorer (FUSE)}. The estimated abundance of O {\small VI} in the SBs varies from a minimum of (1.09 $\pm$0.22)$\times10^{14}$ atoms/cm$^{2}$ in SB N206 to a maximum of (3.71$\pm$0.23)$\times10^{14}$ atoms/cm$^{2}$ in SB N70. We find about a 46% excess in the abundance of O {\small VI} in the SBs compared to the non-SB lines of sight. Even inside a SB, O {\small VI} column density (N(O {\small VI})) varies by about a factor of 2 to 2.5. These data are useful in understanding the nature of the hot gas in SBs.