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We present a simple but effective technique for measuring angular variationin $R_V$ across the sky. We divide stars from the Pan-STARRS1 catalog intoHealpix pixels and determine the posterior distribution of reddening and $R_V$for each pixel using two independent Monte Carlo methods. We find the twomethods to be self-consistent in the limits where they are expected to performsimilarly. We also find some agreement with high-precision photometric studiesof $R_V$ in Perseus and Ophiuchus, as well as with a map of reddening near theGalactic plane based on stellar spectra from APOGEE. While current studies of$R_V$ are mostly limited to isolated clouds, we have developed a systematicmethod for comparing $R_V$ values for the majority of observable dust. This isa proof of concept for a more rigorous Galactic reddening map.x

A Color-locus Method for Mapping $R_V$ Using Ensembles of Stars