  The data from the Gaia satellite led us to revise our conception of the
Galaxy structure and history. Hitherto unknown components have been discovered
and a deep re-thinking of what the Galactic halo is is in progress. We selected
from the Gaia catalogue stars with extreme transverse velocities with respect
to the Sun ($|V_T| > 500 $ and observed them with FORS2 at the ESO VLT, to
classify them using both their chemical and dynamical properties. Two
apparently young stars, identified in paper\,I, were observed with UVES. We
derived abundances for Na, Mg, Ca, Ti, Mn, and Fe, analysing the spectra with
while for Ba we used line profile fitting. We computed actions from parallaxes
and kinematical data. The stars span the metallicity range $ Fe/H -0.5$ with $
Fe/H = -1.6$. Star GHS143 has a total speed of about 1440 which is almost three
times faster than the local escape velocity of 522 strongly implying this star
is unbound to the Galaxy. Remarkably, this star is not escaping from the
Galaxy, but it is falling into it. Ten stars are apparently young with masses
in excess of 1.3M. Their interpretation as evolved blue stragglers is doubtful.
The existence of a young metal-poor population is possible. The two stars
observed with UVES show no lithium, suggesting they are blue stragglers. We
detected a metal-poor population, confined to the bulge, that we call SpiteF,
and argue that it is the result of a recent accretion event. We detect 102
candidates of the Aurora population that should have formed prior to the
formation of the disc. Our sample is non-homogeneous and mainly retrograde. The
stars are metal poor, and 23<!PCT!> have Fe/H -2.0$. Our selection is efficient
at finding very metal-poor stars, but it selects peculiar populations.
