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We analyze the observed spatial, chemical and dynamical distributions oflocal metal-poor stars, based on photometrically derived metallicity anddistance estimates along with proper motions from the Gaia mission. Along theGalactic prime meridian, we identify stellar populations with distinctproperties in the metallicity versus rotational velocity space, including GaiaSausage/Enceladus (GSE), the metal-weak thick disk (MWTD), and the Splash(sometimes referred to as the "in situ" halo). We model the observedphase-space distributions using Gaussian mixtures and refine their positionsand fractional contributions as a function of distances from the Galactic plane($|Z|$) and the Galactic center ($R_{\rm GC}$), providing a global perspectiveof the major stellar populations in the local halo. Within the sample volume($|Z|<6$ kpc), stars associated with GSE exhibit a larger proportion ofmetal-poor stars at greater $R_{\rm GC}$ ($\Delta \langle{\rm[Fe/H]}\rangle/\Delta R_{\rm GC} =-0.05\pm0.02$ dex kpc$^{-1}$). This observed trend, alongwith a mild anticorrelation of the mean rotational velocity with metallicity($\Delta \langle v_\phi \rangle / \Delta \langle{\rm[Fe/H]} \rangle \sim -10$km s$^{-1}$ dex$^{-1}$), implies that more metal-rich stars in the inner regionof the GSE progenitor were gradually stripped away, while the prograde orbit ofthe merger at infall became radialized by dynamical friction. The metal-richGSE stars are causally disconnected from the Splash structure, whose stars aremostly found on prograde orbits ($>94\%$) and exhibit a more centrallyconcentrated distribution than GSE. The MWTD exhibits a similar spatialdistribution to the Splash, suggesting earlier dynamical heating of stars inthe primordial disk of the Milky Way, possibly before the GSE merger.

A Blueprint for the Milky Way's Stellar Populations. III. Spatial Distributions and Population Fractions of Local Halo Stars