Public alert data for KMT-2025-BLG-2093 give a source radius crossing time of 4.12 hours for a fixed limb law

We test how a finite source fit changes when data from one telescope are removed. We use six public I-band alert light curves of the known event KMT-2025-BLG-2093. A fit to 1218 selected points gives a source radius crossing time of 4.117 hours for the fixed surface brightness law I(mu) = 1 - Gamma + 1.5 Gamma mu with Gamma = 0.4. The conditional profile has delta chi squared at most one from 3.991 to 4.253 hours. The finite source model lowers chi squared by 89.41 relative to a point source. Removing Chile data changes the best time to 4.705 hours, broadens the profile, and reduces this model improvement to 5.52. Removing Australia or South Africa gives 4.100 or 4.073 hours. Fixed Gamma values of 0, 0.4, and 0.7 give times from 4.027 to 4.216 hours while their best chi squared values span only 0.394. A separate disk integral and synthetic controls check the computation. The residual scatter exceeds the scaled errors, so the profile widths have no assigned probability coverage. These are alert pySIS data, not the improved TLC reduction used in the published planet-candidate study. The result is a reproducible timing and coverage benchmark. It does not measure lens mass or establish that the lens has no host star.

microlensing · KMT-2025-BLG-2093 · KMTNet · finite source · source crossing time · public photometry · reproducibility