  In this work we combine spectroscopic information from the \textit{SkyMapper
survey for Extremely Metal-Poor stars} and astrometry from Gaia DR2 to
investigate the kinematics of a sample of 475 stars with a metallicity range of
$ -6.5 \leq \rm [Fe/H] \leq -2.05$ dex. Exploiting the action map, we identify
16 and 40 stars dynamically consistent with the \textit{Gaia Sausage} and
\textit{Gaia Sequoia} accretion events, respectively. The most metal-poor of
these candidates have metallicities of $\rm [Fe/H]=-3.31$ and $\rm
[Fe/H]=-3.74$, respectively, helping to define the low-metallicity tail of the
progenitors involved in the accretion events. We also find, consistent with
other studies, that $\sim$21\% of the sample have orbits that remain confined
to within 3~kpc of the Galactic plane, i.e., |Z$_{max}$| $\leq$ 3~kpc. Of
particular interest is a sub-sample ($\sim$11\% of the total) of low
|Z$_{max}$| stars with low eccentricities and prograde motions. The lowest
metallicity of these stars has [Fe/H] = --4.30 and the sub-sample is best
interpreted as the very low-metallicity tail of the metal-weak thick disk
population. The low |Z$_{max}$|, low eccentricity stars with retrograde orbits
are likely accreted, while the low |Z$_{max}$|, high eccentricity pro- and
retrograde stars are plausibly associated with the \textit{Gaia Sausage}
system. We find that a small fraction of our sample ($\sim$4\% of the total) is
likely escaping from the Galaxy, and postulate that these stars have gained
energy from gravitational interactions that occur when infalling dwarf galaxies
are tidally disrupted.

Astrophysics of Galaxies;Solar and Stellar Astrophysics