Probing massive star formation with intrinsic multiplicity constraints from TESS eclipsing binaries

Massive stars play a central role in stellar and galactic evolution as progenitors of supernovae, neutron stars, black holes, and gravitational wave sources. Despite their importance, the dominant formation mechanisms of massive binaries remain poorly constrained observationally. Our aim was to use a large homogeneous sample of eclipsing binaries to observationally constrain binary formation across a wide range of primary masses and to test predictions from various formation scenarios. We combined photometric time series data from TESS with distance measurements from DR3 and near-infrared photometry from 2MASS to analyze an all-sky sample of eclipsing binaries. By accounting for observational and geometric selection effects, we derived bias-corrected estimates of the binary fractions and orbital parameter distributions across different mass bins. Gaia We derived bias-corrected binary fractions and bias-corrected distributions of the orbital period and the radius-to-separation ratio for systems spanning primary masses from 1.1 M_⊙ to 47 M_⊙. For primary masses up to ∼5 M_⊙, the observed distributions show close agreement with theoretical predictions for systems formed via disk fragmentation followed by migration. At higher masses, we observed an apparent deficit of very short period systems relative to theoretical expectations, although this regime is also expected to be affected by incompleteness. Overall, the observed properties exhibit a gradual transition across the full range of primary masses. Within the orbital period range accessible to our sample, the results do not require a sharp transition in binary properties between F- and O-type stars. The observed continuity is consistent with disk fragmentation followed by migration acting across a broad range of stellar masses, although the present data do not uniquely require this formation pathway, and alternative channels may also contribute.