  MWC 297 is a young, early-type star driving an ionized outflow and surrounded
by warm, entrained dust. Previous analyses of near- and mid-IR interferometric
images suggest that the emission at these wavelengths arises from a compact
accretion disk with a moderate ($i < 40$ degrees) inclination. We have obtained
5-40 micron images of MWC 297 with FORCAST on SOFIA, as well as near-infrared
spectra acquired with SpeX on the IRTF and radio data obtained with the VLA and
BIMA, and supplemented these with archival data from Herschel/PACS and SPIRE.
The FORCAST images, combined with the VLA data, indicate that the outflow lobes
are aligned nearly north-south and are well separated. Simple geometrical
modeling of the FORCAST images suggests that the disk driving the outflow has
an inclination of $55\pm 5$ degrees, in disagreement with the results of the
interferometric analyses. Analysis of the SpeX data, with a wind model,
suggests the the mass loss rate is on the order of $6.0 \pm ^{3.7}_{1.7} \times
10^{-7} M_\odot ~\mathrm{yr}^{-1}$ and the extinction to the source is $A_V
\sim 8.1 \pm^{2.5}_{1.5}$ mag. We have combined our data with values from the
literature to generate the spectral energy distribution of the source from
$0.35~ \mu$m to $6$ cm and estimate the total luminosity. We find the total
luminosity to be about $7900 ~ L_\odot$, if we include emission from an
extended region around the star, only slightly below that expected for a B1.5V
star. The reddening must be produced by dust along the line of sight, but
distant from the star.
