  We present Far-Infrared polarimetry observations of M82 at 53 and $154~\mu
\rm{m}$ and NGC 253 at $89~\mu \rm{m}$, which were taken with HAWC+ in
polarimetry mode on the Stratospheric Observatory for Infrared Astronomy
(SOFIA). The polarization of M82 at $53~\mu \rm{m}$ clearly shows a magnetic
field geometry perpendicular to the disk in the hot dust emission. For M82 the
polarization at $154~\mu \rm{m}$ shows a combination of field geometry
perpendicular to the disk in the nuclear region, but closer to parallel to the
disk away from the nucleus. The fractional polarization at $53~\mu \rm{m}$
$(154~\mu \rm{m})$ ranges from 7% (3%) off nucleus to 0.5% (0.3%) near the
nucleus. A simple interpretation of the observations of M82 invokes a massive
polar outflow, dragging the field along, from a region $\sim 700$~pc in
diameter that has entrained some of the gas and dust, creating a vertical field
geometry seen mostly in the hotter $(53~\mu \rm{m})$ dust emission. This
outflow sits within a larger disk with a more typical planar geometry that more
strongly contributes to the cooler $(154~\mu \rm{m})$ dust emission. For NGC
253, the polarization at $89~\mu \rm{m}$ is dominated by a planar geometry in
the tilted disk, with weak indication of a vertical geometry above and below
the plane from the nucleus. The polarization observations of NGC 253 at $53~\mu
\rm{m}$ were of insufficient S/N for detailed analysis.
