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Making use of both MUSE observations of 85 galaxies from the survey GASP (GAsStripping Phenomena in galaxies with MUSE) and a large sample from MaNGA(Mapping Nearby Galaxies at Apache Point Observatory survey) we investigate thedistribution of gas metallicity gradients as a function of stellar mass, forlocal cluster and field galaxies. Overall, metallicity profiles steepen withincreasing stellar mass up to $10^{10.3}\,{\rm M_\odot}$ and flatten out athigher masses. Combining the results from the metallicity profiles and thestellar mass surface density gradients, we propose that the observed steepeningis a consequence of local metal enrichment due to in-situ star formation duringthe inside-out formation of disk galaxies. The metallicity gradient-stellarmass relation is characterized by a rather large scatter, especially for$10^{9.8}<{\rm M_\star/M_\odot}<10^{10.5}$, and we demonstrate that metallicitygradients anti-correlate with the galaxy gas fraction. Focusing on the galaxyenvironment, at any given stellar mass, cluster galaxies have systematicallyflatter metallicity profiles than their field counterparts. Manysub-populations coexist in clusters: galaxies with shallower metallicityprofiles appear to have fallen into their present host halo sooner and haveexperienced the environmental effects for a longer time than cluster galaxieswith steeper metallicity profiles. Recent galaxy infallers, like galaxiescurrently undergoing ram-pressure stripping, show metallicity gradients moresimilar to those of field galaxies, suggesting they have not felt the effect ofthe cluster yet.

GASP and MaNGA surveys shed light on the enigma of the gas metallicity gradients in disk galaxies