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Fig. 6


Bayesian analysis results. Each panel shows host mass M versus lens-source relative parallax πrel, with 1, 2, 3, and 4σ contours under two different conditions. The solid black contours are derived from the light curve alone, without any priors. The colored symbols show contour levels after applying various priors, respectively Galactic proper motion only, Kepler only, full Galactic and Kepler priors, and full Galactic and Kepler priors, plus VLT imaging constraints. The proper-motion and Kepler priors are fully consistent with the light curve, but there is strong tension between between the distance-related priors and the lightcurve, with the former favoring high masses and small lens-source separations. The highest part of this disputed mass range, M > 0.7   M, is essentially ruled out by the VLT imaging constraint (lower right).

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