  We analyze the global structure of the Milky Way (MW)'s stellar halo
including its dominant subcomponent, Gaia-Sausage-Enceladus (GSE). The method
to reconstruct the global distribution of this old stellar component is to
employ the superposition of the orbits covering over the large MW's space,
where each of the orbit-weighting factor is assigned following the probability
that the star is located at its currently observed position. The selected
local, metal-poor sample with ${\rm [Fe/H]}<-1$ using {\it Gaia} EDR3 and SDSS
DR16 shows that the global shape of the halo is systematically rounder at all
radii in more metal-poor ranges, such that an axial ratio, $q$, is nearly 1 for
${\rm [Fe/H]}<-2.2$ and $\sim 0.7$ for $-1.4<{\rm [Fe/H]}<-1.0$. It is also
found that a halo in relatively metal-rich range of ${\rm [Fe/H]}>-1.8$
actually shows a boxy/peanut-like shape, suggesting a major merger event. The
distribution of azimuthal velocities shows a disk-like flattened structure at
$-1.4<{\rm [Fe/H]}<-1.0$, which is thought to be the metal-weak thick disk. For
the subsample of stars showing GSE-like kinematics and at ${\rm [Fe/H]}>-1.8$,
its global density distribution is more spherical with $q \sim 0.9$ than the
general halo sample, having an outer ridge at $r\sim20$~kpc. This spherical
shape is consistent with the feature of accreted halo components and the ridge
suggests that the orbit of GSE's progenitor has an apocenter of $\sim 20$~kpc.
Implications for the formation of the stellar halo are also presented.
