  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.
