  We study spatially resolved scaling relations among stars, dust, and gas in
ten nearby spiral galaxies. In a preceding paper Abdurro'uf et al. (2022), we
have derived spatially resolved properties of the stellar population and dust
by panchromatic spectral energy distribution (SED) fitting using piXedfit. Now,
we investigate resolved star formation ($\Sigma_{\rm H_{2}}$--$\Sigma_{\rm
SFR}$--$\Sigma_{*}$) and dust scaling relations. While the relations with all
sub-galactic regions of the galaxies are reasonably tight ($\sigma \lesssim
0.3$ dex), we find that most of the scaling relations exhibit galaxy-to-galaxy
variations in normalization and shape. Only two relations of $\Sigma_{\rm
dust}$--$\Sigma_{\rm gas}$ and $\Sigma_{\rm dust}$--$\Sigma_{\rm H_{2}}$ do not
show noticeable galaxy-to-galaxy variations among our sample galaxies. We
further investigate correlations among the scaling relations. We find
significant correlations among the normalization of the $\Sigma_{\rm
H_{2}}$--$\Sigma_{\rm SFR}$--$\Sigma_{*}$ relations, which suggest that
galaxies with higher levels of resolved $\text{H}_{2}$ fraction ($f_{\rm
H_{2}}$) tend to have higher levels of resolved star formation efficiency (SFE)
and specific star formation rate (sSFR). We also observe that galaxies with
higher levels of resolved dust-to-stellar mass ratios tend to have higher
levels of resolved sSFR, SFE, and $f_{\rm H_{2}}$. Moreover, we find that
galaxies with higher global sSFR and less compact morphology tend to have
higher levels of the resolved sSFR, SFE, and $f_{\rm H_{2}}$, which can explain
the variations in the normalization of the $\Sigma_{\rm H_{2}}$--$\Sigma_{\rm
SFR}$--$\Sigma_{*}$ relationships. Overall, we observe indications of the
contributions of both global and local factors in governing the star formation
process in galaxies.
