  Studying the internal processes of individual galaxies at kilo-parsec scales
is crucial in enhancing our understanding of galaxy formation and evolution
processes. In this work, we investigate the distribution of star formation rate
(SFR), specific SFR (sSFR), and dust attenuation across individual galaxies for
a sample of 32 galaxies selected from the MUSE-Wide Survey at 0.1 $< \textit{z}
<$ 0.42 with a dynamic range in stellar masses between $10^{7.7}$ and
$10^{10.3}$ M$_{\odot}$. We take advantage of the high spatial resolution of
the MUSE integral-field spectrograph and measure reliable spatially resolved
H$\alpha$ and H$\beta$ emission line maps for individual galaxies. We also
derive resolved stellar mass, SFR and dust maps using pixel-by-pixel SED
fitting on high resolution multi-band HST/ACS and HST/WFC3 data from the
CANDELS survey. By combining these, we analyze the radial profile of various
physical parameters across these galaxies. We observe a radial dependence in
both stellar and nebular color excess profiles peaking at the inner regions of
galaxies. We also find the color excess profiles to most strongly correlate
with the integrated sSFRs of galaxies. The median sSFR$_{\mathrm{H}\alpha}$
radial profiles of galaxies in our sample show a 0.8 dex increase from the
central regions outward. This increase compared to the almost flat median
radial profile of sSFR$_{\mathrm{SED}}$, which traces longer timescales of star
formation, is in favor of the inside-out quenching of star formation. We bring
further evidence for this quenching scenario from the locus of different
subregions of galaxies on the SFR-M$_{*}$ and sSFR-M$_{*}$ relations.
