  We present results from deep and very spatially extended CTIO/DECam $g$ and
$r$ photometry (reaching out to $\sim$ 2 mag below the oldest MSTO and covering
$\sim$ 20 deg$^2$) around the Sextans dSph. We use this data-set to study the
structural properties of Sextans overall stellar population and its different
stellar evolutionary phases, as well as to search for signs of tidal
disturbance from the MW, which would indicate departure from dynamical
equilibrium. We perform the most accurate structural analysis to-date of
Sextans' stellar components by applying Bayesian MCMC methods to the individual
stars' positions. Surface density maps are built by decontaminating the sample
through a matched filter analysis of the CMD, and then analysed for departures
from axisymmetry. Sextans is found to be considerably less spatially extended
than early studies suggested. No significant distortions or tidal disturbances
are found down to a surface brightness of $\sim$ 31.8 mag/arcsec$^{-2}$ in
V-band. We identify an overdensity in the central regions that may correspond
to previously reported kinematic substructure(s). In agreement with previous
findings, old $\&$ metal-poor stars such as BHB stars cover a much larger area
than stars in other evolutionary phases, and bright BSs are less spatially
extended than faint ones. However, the different spatial distribution of bright
and faint BSs appears consistent with the general age/metallicity gradients
found in Sextans' stellar component. This is compatible with BSs having formed
by evolution of binaries and not necessarily due to the presence of a central
disrupted globular cluster, as suggested in the literature. We provide
structural parameters for the various populations analyzed and make publicly
available the photometric catalogue of point-sources as well as a catalogue of
literature spectroscopic measurements with updated membership probabilities.
