Constraining the nature and Galactic origin of the Be binary MWC 656

Abstract

The binary star MWC 656 was initially proposed as the first confirmed system composed of a Be star and a black hole (BH). However, recent studies have challenged this interpretation, suggesting that the compact companion is unlikely to be a BH. In this study, we revisited the nature of MWC 656 by analyzing archival data across multiple wavelengths, including radio observations from the Karl G. Jansky Very Large Array (VLA), optical astrometry from the Gaia satellite, and high-energy γ-ray data from the Fermi-LAT. Using all available VLA observations at the X band (8.0-12.0 GHz), we produced the deepest radio map toward this system to date, with a noise level of 780 nJy beam⁻¹. The source MWC 656 was detected with Sᵥ = 4.6 ± 0.8μJy and a spectral index of α = 1.2 ± 1.8, derived by sub-band imaging. The radio-X-ray-luminosity ratio of MWC 656 is consistent with both the fundamental plane of accreting BHs and with the Güdel-Benz relation for magnetically active stars, leaving the emission mechanism ambiguous. The optical astrometric results of MWC 656 indicate a peculiar velocity of 11.2 ± 2.3 km s⁻¹, discarding it as a runaway star. Its current location, 442 pc below the Galactic plane, implies a vertical travel time incompatible with the lifetime of a B1.5-type star. Moreover, the agreement between observed and expected motion in all three velocity components argues against a deceleration scenario, suggesting that MWC 656 likely formed in situ at high Galactic latitudes. We carried out a maximum-likelihood analysis of Fermi-LAT data, but we cannot report a significant detection of γ-ray emission from this source. These results reinforce recent evidence that challenge the BH companion interpretation, and favor a non-BH compact object such as a white dwarf or neutron star.