Toward Understanding the B[e] Phenomenon. VII. AS 386, a single-lined binary with a candidate black hole component

TL;DR

This study investigates the binary system AS 386, revealing it exhibits the B[e] phenomenon, contains a B-type star, and likely hosts a black hole companion, based on spectroscopic, photometric, and Doppler tomography analyses.

Contribution

First detailed spectroscopic and photometric analysis of AS 386 showing B[e] phenomenon and evidence for a black hole companion in a binary system.

Findings

AS 386 exhibits B[e] phenomenon and FS CMa characteristics.

Orbital period of 131.27 days with radial velocity variations.

Likely hosts a black hole companion due to absence of secondary star features.

Abstract

We report the results of spectroscopic and photometric observations of the emission-line object AS 386. For the first time, we found that it exhibits the B[e] phenomenon and fits the definition of an FS CMa type object. The optical spectrum shows the presence of a B-type star with the following properties: T_ eff = 11000+/-500 K, log L/L_sun = 3.7+/-0.3, a mass of 7+/-1 M_sun, and a distance D = 2.4+/-0.3 kpc from the Sun. We detected regular radial velocity variations of both absorption and emission lines with the following orbital parameters: P_orb = 131.27+/-0.09 days, semi-amplitude K_1 = 51.7+/-3.0 km/s, systemic radial velocity gamma = -31.8+/-2.6 km/s, and a mass function of f(m) = 1.9+/-0.3 M_sun. AS 386 exhibits irregular variations of the optical brightness (V=10.92+/-0.05 mag), while the near-IR brightness varies up to ~0.3 mag following the spectroscopic period. We explain this behavior by a variable illumination of the dusty disk inner rim by the B-type component. Doppler tomography based on the orbital variations of emission-line profiles shows that the material is distributed near the B-type component and in a circumbinary disk. We conclude that the system has undergone a strong mass transfer that created the circumstellar material and increased the B-type component mass. The absence of any traces of a secondary component, whose mass should be >= 7 M_sun, suggests that it is most likely a black hole.