The distribution and kinematics of interstellar O~{\small VI} in the Milky Way}

We present the results of a survey of interstellar O~{\small VI} absorption in the Milky Way (MW) towards {69} stars in the Large Magellanic Cloud (LMC) obtained with the $\mathit{\text{Far}}\mathit{\text{Ultraviolet}}\mathit{\text{Spectroscopic}}\mathit{\text{Explorer}}\mathit{\text{(FUSE)}}$. The integrated MW O~{\small VI} column densities log N(O~{\small VI}) are in the range from 13.68 to 14.73 with a mean of {14.26${}_{-0.09}^{+0.07}$} atoms cm${}^{-2}$. The O~{\small VI} exponential scale height is found to be {2.28$\pm$1.06} kpc. The O~{\small VI} column density correlates with the Doppler parameter $b$. The O~{\small VI} velocity dispersion ranges from {14.0 to 91.6 with an average value of 62.7 km s${}^{-1}$}. These high values of velocity dispersion reveal the effect of turbulence, multiple velocity components and collision on broad O~{\small VI} profiles. There is a significant variation of O~{\small VI} column density on all scales studied {(0.0025$\text{degr}$ - 6.35$\text{degr}$)}. The smallest scale for which O~{\small VI} column density variations has been found is {$△\theta$ $\sim$~9$\text{arcsec}$}. Comparison of the O~{\small VI} velocity profiles with Fe~{\small II} indicates the presence of intermediate velocity cloud (IVC) and/or high velocity cloud (HVC) components in the O~{\small VI} absorption.