Program: GS-2010B-Q-31

B[e]sg are B-type supergiants, surrounded by non-spherically distributed material where strong line emission is created. The detection of strong infrared excess led to the assumption of these stars being surrounded by geometrically thick, high-density dusty disks. Because of the rapid rotation of these stars, the idea that their disks are revolving the star on (quasi-)Keplerian orbits became accepted. However, any attempt to theoretically generate a Keplerian disk around a rotating B[e]sg has failed. Instead, the new wind solutions by Cure and collaborators give a natural explanation for the observed density enhancements in the equatorial wind regions, and result in a radial wind velocity distribution that delivers line-of-sight velocities, different from those of a Keplerian rotating disk. A kinematical study of the equatorial disk/wind material gives direct proof of the slow-wind scenario. The most capable tracer of the kinematics within cool and dense regions is the CO molecule: its first-overtone bandhead structure (2.3 micron) is sensitive to the motion of the CO gas. Thus, we plan to observe the bandheads of B[e]sg in the LMC, known to show CO band emission. R=50000 provided by Phoenix, is enough for a detection of bandhead structures and an unambigous test of the slow-wind scenario.