  B[e] Supergiants are a phase in the evolution of some massive stars for which
we have observational evidence but no predictions by any stellar evolution
model. The mass-loss during this phase creates a complex circumstellar
environment with atomic, molecular, and dust regions usually found in rings or
disk-like structures. However, the detailed structure and the formation of the
circumstellar environment are not well-understood, requiring further
investigation. To address that we initiated an observing campaign to obtain a
homogeneous set of high-resolution spectra in both the optical and NIR (using
MPG-ESO/FEROS, GEMINI/Phoenix and VLT/CRIRES, respectively). We monitor a
number of Galactic B[e] Supergiants, for which we examined the [OI] and [CaII]
emission lines and the bandheads of the CO and SiO molecules to probe the
structure and the kinematics of their formation regions. We find that the
emission from each tracer forms either in a single or in multiple equatorial
rings.
