  We analyse a set of very metal-poor stars for which accurate chemical
abundances have been obtained as part of the ESO Large Program "First stars" in
the light of the Gaia DR2 data. The kinematics and orbital properties of the
stars in the sample show they probably belong to the thick disc, partially
heated to halo kinematics, and to the accreted Nissen & Schuster-Gaia
Sausage-Enceladus satellite. The continuity of these properties with stars at
both higher ($\rm [Fe/H]>-2$) and lower metallicities ($\rm [Fe/H]<-4.$)
suggests that the Galaxy at $\rm [Fe/H] \lesssim -0.5$ and down to at least
$\rm [Fe/H]\sim-6$ is dominated by these two populations. In particular, we
show that the disc extends continuously from $\rm [Fe/H] \le -4$ (where stars
with disc-like kinematics have been recently discovered) up to $\rm [Fe/H] \ge
-2$, the metallicity regime of the Galactic thick disc. There exists indeed an
"ultra-metal poor thick disc", which constitutes the extremely metal-poor tail
of the canonical Galactic thick disc, and which extends this latter from $\rm
[Fe/H] \sim -0.5$ up to the most metal-poor stars discovered in the Galaxy up
to date. These results suggest that the disc may be the main, and possibly the
only stellar population that has formed in the Galaxy at these metallicities.
This requires that the dissipative collapse that led to the formation of the
old Galactic disc must have been extremely fast. We also discuss these results
in the light of recent simulation efforts made to reproduce the first stages of
Milky Way-type galaxies.
