We present the results of optical and near-IR spectroscopic and broadband multicolour photometric observations of the emission-line star AS 381. Its properties were found to be similar to those of Be stars with warm dust, a group of galactic objects recently defined by Sheikina et al. (2000). The spectrum of AS 381 indicates the presence of both a hot (early B-type) and a cool (K-type) star in the system. A high interstellar reddening (AV ∼ 7 mag) suggests that it is located at a distance of ≥ 3 kpc, and the companions have luminosity types II or higher. The emission-line profiles indicate that the system is surrounded by a flattened circumstellar envelope, which is viewed close to pole-on. The hot companion is found to be ∼2 mag brighter in the V-band and more massive (∼20 M⊙) than the cool one (∼7 M⊙). The strong line emission and position of the companions in the Hertzsprung-Russell diagram indicate that the system is experiencing mass exchange. We suggest that AS 381 is the first B[e] supergiant binary discovered in the Milky Way.
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Miroshnichenko, A. S., Bjorkman, K. S., Chentsov, E. L., Klochkova, V. G., Ezhkova, O. V., Gray, R. O., … Puetter, R. (2002). The luminous B[e] binary AS 381. Astronomy and Astrophysics, 383(1), 171–181. https://doi.org/10.1051/0004-6361:20011711