Properties of galactic B[e] supergiants^*

III. MWC 300

¹ Ritter Observatory, Dept. of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390, USA
² Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 196140 Saint-Petersburg, Russia
³ Complejo Astronómico El Leoncito (CASLEO), Casilla de Correo 467, 5400 San Juan, Argentina
⁴ CFHT Corporation, 65–1238 Mamalahoa Hwy, Kamuela, HI 96743, Hawaii, USA
⁵ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany
⁶ Institute for Computational Astrophysics, Saint Mary's University, Halifax, NS  B3H 3C3, Canada
⁷ The Aerospace Corp. M2/266, PO Box 92957, Los Angeles, CA 90009, USA
⁸ Center for Astrophysics and Space Science, University of California, San Diego, 0111, La Jolla, CA 92093, USA
⁹ Earth and Space Science Support Office, M/S 160, NASA Langley Research Center, Hampton, VA 23681, USA

Corresponding author: A. S. Miroshnichenko, anatoly@physics.utoledo.edu

Received: 12 August 2003
Accepted: 21 December 2003

Abstract

We present the results of optical and near-IR spectroscopic and mid-IR imaging observations of the emission-line star MWC 300. Its properties and evolutionary state are still under debate (a B[e] supergiant or a Herbig Be star). For the first time we detected radial velocity variations of the photospheric lines and found a correlation between them and those of the He i λ5876 Å line. Most of the pure emission lines had stable positions for nearly 20 years. New estimates of the object's luminosity (/), distance ( kpc), and systemic velocity ( km s^-1) were derived. We found that both the circumstellar extinction in the disk-like dusty envelope and the interstellar extinction play a significant role in the attenuation of the stellar brightness. Our 2D modeling of the observed spectral energy distribution in the wavelength range from 0.3 μm to 1.3 mm suggests that the star is viewed through a gaseous-and-dusty flared disk with an opening angle of 30°, an inclination angle of 10°, an equatorial optical depth , and a total mass of 0.08 . We argue that MWC 300 is most likely a binary system, because of the similarities of its observed parameters with those of recognized B[e] binaries.