Resolving the Wolf–Rayet Mass Discrepancy Through the Photogravitational Parameter Φ

This dataset introduces a fully observational method for determining the masses of Wolf–Rayet stars, based on the surface-calibrated photogravitational parameter: Φ ≡ L / (M g) This parameter serves as a direct diagnostic using only luminosity and surface gravity — without requiring interior models or opacity assumptions. We calibrate Φ using 12 WR+O binaries with secure dynamical masses, achieving an RMS accuracy of ∼9% across WN and WC subtypes. When applied to 10 isolated WR stars, the method reproduces the well-known 35–54% mass discrepancy relative to evolutionary predictions, with a median offset of ~40%. The Φ-based approach provides a consistent, reproducible, and fully empirical framework for massive-star mass determinations — enabling population-wide applications across the Galactic WR sample.