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Studying the internal processes of individual galaxies at kilo-parsec scalesis crucial in enhancing our understanding of galaxy formation and evolutionprocesses. In this work, we investigate the distribution of star formation rate(SFR), specific SFR (sSFR), and dust attenuation across individual galaxies fora 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 ofthe MUSE integral-field spectrograph and measure reliable spatially resolvedH$\alpha$ and H$\beta$ emission line maps for individual galaxies. We alsoderive resolved stellar mass, SFR and dust maps using pixel-by-pixel SEDfitting on high resolution multi-band HST/ACS and HST/WFC3 data from theCANDELS survey. By combining these, we analyze the radial profile of variousphysical parameters across these galaxies. We observe a radial dependence inboth stellar and nebular color excess profiles peaking at the inner regions ofgalaxies. We also find the color excess profiles to most strongly correlatewith 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 thecentral regions outward. This increase compared to the almost flat medianradial profile of sSFR$_{\mathrm{SED}}$, which traces longer timescales of starformation, is in favor of the inside-out quenching of star formation. We bringfurther evidence for this quenching scenario from the locus of differentsubregions of galaxies on the SFR-M$_{*}$ and sSFR-M$_{*}$ relations.

Spatially resolved properties of galaxies from CANDELS+MUSE: Radial extinction profile and insights on quenching