High spectral resolution observations toward Orion BN at 6 $\mu$m: no
  evidence for hot water
  Orion BN has a large proper motion and radial velocity with respect to the
gas and other stars in the region where it is presumed to have formed. Multiple
dynamical interaction scenarios have been proposed to explain this motion. In
one case BN is thought to have interacted with stars in the Trapezium cluster,
while in another it is thought to have interacted with source I while deeply
embedded in molecular gas. If there is dense gas that has been retained in
close proximity to BN, it may be evidence that the latter scenario is favored.
We observed BN at high spectral resolution in three windows near 6 $\mu$m using
SOFIA/EXES targeting the $\nu_2$ vibrational band of H$_2$O. Absorption from
only three transitions of H$_2$O is detected, and through kinematic analysis is
associated with cool, dense foreground gas, not BN itself. We find no evidence
for H$_2$O absorption or emission at the systemic velocity of BN.
