Resolving the kinematics of the disks around Galactic B[e] supergiants

Abstract

B[e] Supergiants are luminous evolved massive stars. The mass-loss during this phase creates a complex circumstellar environment with atomic, molecular, and dusty regions usually found in rings or disk-like structures. For a better comprehension of the mechanisms behind the formation of these rings, detailed knowledge about their structure and dynamics is essential. To address that, we obtained high-resolution optical and near-infrared spectra for 8 selected Galactic B[e] Supergiants, for which CO emission has been detected. Assuming Keplerian rotation for the disk, we combine the kinematics obtained from the CO bands in the near-IR with those obtained by fitting the forbidden emission [OI] $\lambda$5577, [OI] $\lambda \lambda$6300,6363, and [CaII] $\lambda \lambda$7291,7323 lines in the optical to probe the disk structure. We find that the emission originates from multiple ring structures around all B[e] Supergiants, with each one of them displaying a unique combination of rings regardless of whether the object is part of a binary system. The confirmed binaries display spectroscopic variations of their line intensities and profiles as well as photometric variability, whereas the ring structures around the single stars are stable.

arXiv comment27 pages, 13 figures, 4 tables. Published in MNRAS. Minor corrections in this version: (a) adding references in the text to Fig. 6, tables A6 and A8, and footnote 5, (b) adding/modifying the acknowledgments section

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