O vi absorption in the Milky Way along the Large Magellanic Cloud lines of sight

Abstract

We have used Far Ultraviolet Spectroscopic Explorer (FUSE) observations of the Large Magellanic Cloud (LMC) to determine the O VI column densities in the Milky Way (MW) towards 6 LMC lines of sight. The mean column density of O VI in the MW is found to be log N(O VI)=14.257 +0.096 −0.084 . The results confirm the patchiness of O VI absorption in the MW and the column densities are higher or comparable to the LMC.

The distribution and kinematics of interstellar O vi in the Milky Way

“…Most of the large IVCs and HVCs are located in the inner Galactic halo at distances d 20 kpc (Wakker et al 2007;Thom et al 2006; except the "Magellanic Stream" (MS) which is at ∼50 kpc (Gardiner & Noguchi 1996). The accretion of gas from the two Magellanic Clouds by the MW has been considered as the origin of Magellanic Stream (Wannier, & Wrixon 1972;Fox et al 2010;, 2014Richter et al 2013).…”