SFR density profiles based on the curve-of-growth analyses (Fig. 2), which were deconvolved according to the PSF. Sources that are identified to host an AGN are marked with an asterisk after the ID. For the IR-based profiles, we assume that they follow the morphology of the observed 870 μm emissions, meaning the IR-based SFRs in each radial bin is the fraction of the total 870 μm flux times the total SFRs. The Hα-based profiles were derived by differentiating the curve-of-growth results, converting the Hα luminosity to SFRs according to Kennicutt & Evans (2012), and adopting an attenuation correction of Calzetti et al. (2000), except for ALESS66.1 for which the OIR photometry is contaminated by a foreground quasar (Fig. 1). For ALESS66.1, we plotted the profile without correcting for attenuation. For clarity, we only plotted the bins that have ≥1σ measurements.