  Observational studies have identified several sub-structures in different
regions of the Magellanic Clouds, the nearest pair of interacting dwarf
satellites of the Milky Way. By studying the metallicity of the sources in
these sub-structures, we aim to shed light on the possible origin of these
sub-structures. Spectroscopic metallicities exist only for a few thousand
sources, mostly giant stars located in specific regions of the galaxies. These
metallicities come from different instruments at various spectral resolutions,
and systematic uncertainties hamper comparisons and draw firm conclusions about
their origin. The third data release of \textit{Gaia} has provided us with
$\sim$ 0.17 million XP spectra of the different stellar populations in the SMC
alone as faint as $\sim$ 18 mags in the G band, which are spread across $\sim$
10$^\circ$ from the SMC centre. We aim to determine the metallicities of these
sources based on synthetic Str\"{o}mgren photometry derived from XP spectra and
produce a high-resolution metallicity map of the SMC. Our metallicity gradient
estimate of the SMC turns out to be --0.062 $\pm$ 0.009 dex/deg. This is
comparable with the previous estimates, which also validate our method of
metallicity estimation. We aim to apply this method to other stellar
populations and to the LMC to create a high-resolution metallicity map of the
Magellanic Clouds.
