We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with $P_{ \rm obs}=2.77$ days containing a possible massive white dwarf or a neutron star using the LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we derived a circular Keplerian orbit with an inclination of $i=$81.31$^{ \circ}$$^{ +6.26^{ \circ}}_{ -7.85^{ \circ}}$, which is consistent with that derived from $v{ \rm sin}I$. Together with the mass of the visible star, we derived the mass of the invisible object to be 1.34$^{ +0.35}_{ -0.40} M_{ \odot}$. Spectral disentangling with the LAMOST medium-resolution spectra shows no absorption feature from an additional component, suggesting the presence of a compact object. No X-ray or radio pulsed signal is detected from ROSAT and FAST archive observations. J0606+2132 could evolve into either a Type Ia supernova or a neutron star through accretion-induced collapse if it is a white dwarf, or into an intermediate-mass X-ray binary if it is a neutron star.
Categories: astro-ph.SR astro-ph.HE