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We develop a method to estimate photometric metallicities by simultaneouslyfitting the dereddened colors u-g, g-r, r-i and i-z from the SDSS with thosepredicted by the metallicity-dependent stellar loci. The method is tested witha spectroscopic sample of main-sequence stars in Stripe 82 selected from theSDSS DR9 and three open clusters. With 1 per cent photometry, the method iscapable of delivering photometric metallicities precise to about 0.05, 0.12,and 0.18 dex at metallicities of 0.0, -1.0, and -2.0, respectively, comparableto the precision achievable with low-resolution spectroscopy at asignal-to-noise ratio of 10. We apply this method to the re-calibrated Stripe82 catalog and derive metallicities for about 0.5 million stars of colors 0.3 <g-i < 1.6 mag and distances between 0.3 -- 18 kpc. Potential systematics in themetallicities thus derived, due to the contamination of giants and binaries,are investigated. Photometric distances are also calculated. About 91, 72, and53 per cent of the sample stars are brighter than r = 20.5, 19.5, and 18.5 mag,respectively. The median metallicity errors are around 0.19, 0.16, 0.11, and0.085 dex for the whole sample, and for stars brighter than r = 20.5, 19.5, and18.5 mag, respectively. The median distance errors are 8.8, 8.4, 7.7, and 7.3per cent for the aforementioned four groups of stars, respectively. The dataare publicly available. Potential applications of the data in studies of thedistribution, (sub)structure, and chemistry of the Galactic stellarpopulations, are briefly discussed. The results will be presented in futurepapers.

Stellar loci III: Photometric metallicities for half million FGK stars of Stripe 82