  In situ measurements of the fast solar wind reveal non-thermal distributions
of electrons, protons and, minor ions extending from $0.3$ AU to the
heliopause. The physical mechanisms responsible for these non-thermal
properties and the location where these properties originate remain open
questions. Here we present spectroscopic evidence, from extreme ultraviolet
spectroscopy, that the velocity distribution functions (VDFs) of minor ions are
already non-Gaussian at the base of the fast solar wind in a coronal hole, at
altitudes of $< 1.1 R_{\odot}$. Analysis of Fe, Si, and Mg spectral lines
reveal a peaked line-shape core and broad wings that can be characteristed by a
kappa VDF. A kappa distribution fit gives very small kappa indices off-limb of
$\kappa\approx1.9-2.5$, indicating either (a) ion populations far from thermal
equilibrium, (b) fluid motions such as non-Gaussian turbulent fluctuations or
non-uniform wave motions, or (c) some combination of both. These observations
provide important empirical constraints for the source region of the fast solar
wind and for the theoretical models of the different acceleration, heating, and
energy deposition processes therein. To the best of our knowledge, this is the
first time that the ion VDF in the fast solar wind has been probed so close to
its source region. The findings are also a timely precursor to the upcoming
2018 launch of the Parker Solar Probe, which will provide the closest in situ
measurements of the solar wind at approximately $0.04$ AU ($8.5$ solar radii).
