We wish to determine the Neon/Helium abundance ratio in
 Wolf-Rayet winds by measuring in SWS AOT Band-3A (12.0 - 16.5
 micron) with AOT SWS06 the flux of the [NeII] 12.184 micron and
 [NeIII] 15.55 micron and the neighbouring HeII emission lines in
 WR stars with galactocentric distances ranging from 6 kpc to 10
 kpc from the Sun.  We wish simulataneous spectrophotometric
 observations in SWS AOT Band-1A (2.38 - 2.60) where emission
 lines of CIV, HeII and He I occur.  The width of those spectral
 lines will be a measure of the WR steller wind velocities, since
 the [NeIII] lines are formed where the winds have reached their
 terminal velocities.  The abundance and velocities together will
 allow the determination of mass loss rates.
 The Neon abundance determinations are a crucial check of
 stellar evolution models for massive stars, which predict a much
 larger than solar Neon abundance.