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We present the metallicity distribution of a sample of 471 RR Lyrae (RRL)stars in the Sculptor dSph, obtained from the $I$-band Period-Luminosityrelation. It is the first time that the early chemical evolution of a dwarfgalaxy is characterized in such a detailed and quantitative way, usingphotometric data alone. We find a broad metallicity distribution (FWHM=0.8 dex)that is peaked at [Fe/H]$\simeq$-1.90 dex, in excellent agreement withliterature values obtained from spectroscopic data. Moreover, we are able todirectly trace the metallicity gradient out to a radius of $\sim$55 arcmin. Wefind that in the outer regions (r$>\sim$32 arcmin) the slope of the metallicitygradient from the RRLs (-0.025 dex arcmin$^{-1}$) is comparable to theliterature values based on red giant (RG) stars. However, in the central partof Sculptor we do not observe the latter gradients. This suggests that there isa more metal-rich and/or younger population in Sculptor that does not produceRRLs. This scenario is strengthened by the observation of a metal-rich peak inthe metallicity distribution of RG stars by other authors, which is not presentin the metallicity distribution of the RRLs within the same central area.

Probing the early chemical evolution of the Sculptor dSph with purely old stellar tracers