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Recent advances from astronomical surveys have revealed spatial, chemical,and kinematical inhomogeneities in the inner region of the stellar halo of theMilky Way Galaxy. In particular, large spectroscopic surveys, combined withGaia astrometric data, have provided powerful tools for analyzing the detailedabundances and accurate kinematics for individual stars. Despite thesenoteworthy efforts, however, spectroscopic samples are typically limited by thenumbers of stars considered; their analysis and interpretation are alsohampered by the complex selection functions that are often employed. Here wepresent a powerful alternative approach $-$ a synoptic view of the spatial,chemical, and kinematical distributions of stars in the Milky Way based onlarge photometric survey databases, enabled by a well-calibrated technique forobtaining individual stellar metal abundances from broad-band photometry. Wecombine metallicities with accurate proper motions from the Gaia mission alongthe Prime Meridian of the Galaxy, and find that various stellar components areclearly separated from each other in the metallicity versus rotation-velocityspace. The observed metallicity distribution of the inner-halo stars deviatesfrom the traditional single-peaked distribution, and exhibits complexsubstructures comprising varying contributions from individual stellarpopulations, sometimes with striking double peaks at low metallicities. Thesubstructures revealed from our less-biased, comprehensive maps demonstrate theclear advantages of this approach, which can be built upon by future mixed-bandand broad-band photometric surveys, and used as a blueprint for identifying thestars of greatest interest for upcoming spectroscopic studies.

A Blueprint for the Milky Way's Stellar Populations: The Power of Large Photometric and Astrometric Surveys