Recent large optical and near-infrared spectroscopic surveys have revolutionized our views on stellar populations in the Galaxy with accurate measurements of photospheric abundances and radial velocities for a large number of stars. On the other hand, at least two orders of magnitude larger number of stars in the Milky Way have been observed in the imaging surveys such as in SDSS, SCUSS, and Pan-STARRS. I will introduce a method of computing a metallicity of individual stars based on ugriz photometry, and present new metallicity maps of the Milky Way based on these industrial-sized data sets. I will also discuss chemo-dynamical properties of stars in the disk and the halo and their origins by combining photometric metallicity estimates with Gaia’s proper motion measurements.