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 \textit{Far Ultraviolet Spectroscopic Explorer (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 $\it b$. 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$\degr$ - 6.35$\degr$)}. The smallest scale for which O~{\small VI}
column density variations has been found is {$\bigtriangleup \theta$
$\sim$~9$\arcsec$}. 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.
