2025ApJ...992..107O

The ∼2100 daylong secondary period of Betelgeuse's optical lightcurve and radial velocity motivated the prediction of a low-mass stellar companion, expected to be at maximal apparent separation from Betelgeuse around 2024 December. We carried out Director's Discretionary Time observations with the Chandra X-ray Observatory to identify any X-ray emission from the companion and constrain its nature as either a compact object or young stellar object (YSO). Past X-ray observations occurred at the wrong phase of the companion's orbit for optimal detection prospects and/or lacked the deep exposure required to constrain the typical X-ray luminosities of YSOs. In our 41.85 ks exposure with Chandra, we do not detect an X-ray source at the position of Betelgeuse. For an estimated hydrogen column density N_H = 6 × 10²² cm^–2, we place a limit on the X-ray luminosity L_X ≲ 2 × 10³⁰ erg s^–1 (≲4.7 × 10^–4L_⊙) in 0.5-8 keV for a 10 MK plasma temperature spectral model, or L_X ≲ 5 × 10²⁹ erg s^–1 (≲1.2 × 10^–4L_⊙) for an absorbed power law with photon index Γ = 2. These limits robustly exclude an accreting compact object (white dwarf or neutron star) as the companion. Solar-mass YSOs with an age similar to Betelgeuse (∼10 Myr) display a range of X-ray luminosities (10^28–32 erg s^–1), and we can place upper bounds within this range for most absorbing columns. Based on these considerations, we conclude that the companion to Betelgeuse is likely a low-mass YSO.