The Surface-Based Photogravitational Parameter Φ Reveals Mass Discrepancies in Wolf-Rayet Stars

This dataset provides a calibration and application of the photogravitational parameter Φ ≡ L/(M g) as a surface–based diagnostic for determining the masses of Wolf–Rayet stars. The method is first calibrated against 12 WR+O binaries with secure dynamical masses, yielding an RMS accuracy of ~9% across both WN and WC subtypes. With these calibrated constants in place, we then apply the method to 10 isolated WR stars, deriving masses that are systematically 35–54% lower than evolutionary model predictions, with a median discrepancy of ~40%. By anchoring the relation in binary systems with dynamical solutions, the Φ–based approach, calibrated on secure dynamical masses, provides a reproducible, observation–driven mass diagnostic. The dataset includes calibration values, the list of reference binaries, inputs for the isolated stars, and reproducible scripts for computing the calibrated masses M_Φ, the Eddington ratio Γ, and closure checks.