We present a stellar population analysis of the nearby, face-on, SA(s)c galaxy, NGC628, which is part of the PPAK IFS Nearby Galaxies Survey (PINGS). The data cover a field of view of ~6 arcmin in diameter with a sampling of $sim$2.7 arcsec per spectrum and a wavelength range (3700-7000A). We apply spectral inversion methods to derive 2-dimensional maps of star formation histories and chemical enrichment. We present maps of the mean (luminosity- and mass-weighted) age and metallicity that reveal the presence of structures such as a nuclear ring, previously seen in molecular gas. The disk is dominated in mass by an old stellar component at all radii sampled by our data, while the percentage of young stars increase with radius. The mean stellar age and metallicity profiles have a two defined regions, an inner one with flatter gradients (even slightly positive) and an external ones with a negative, steeper one, separated at $sim$60 arcsec. This break in the profiles is more prominent in the old stellar component. The young component shows a metallicity gradient that is very similar to that of the gas, and that is flatter in the whole disc. The agreement between the metallicity gradient of the young stars and the gas, and the recovery of the measured colours from our derived star formation histories validate the techniques to recover the age-metallicity and the star formation histories in disc galaxies from integrated spectra. We speculate about the possible origin of the break and conclude that the most likely scenario is that we are seeing, in the center of NGC 628, a dissolving bar, as predicted in some numerical simulations.
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