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Orion BN has a large proper motion and radial velocity with respect to thegas and other stars in the region where it is presumed to have formed. Multipledynamical interaction scenarios have been proposed to explain this motion. Inone 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 deeplyembedded in molecular gas. If there is dense gas that has been retained inclose 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 usingSOFIA/EXES targeting the $\nu_2$ vibrational band of H$_2$O. Absorption fromonly three transitions of H$_2$O is detected, and through kinematic analysis isassociated with cool, dense foreground gas, not BN itself. We find no evidencefor H$_2$O absorption or emission at the systemic velocity of BN.

High spectral resolution observations toward Orion BN at 6 $\mu$m: no evidence for hot water