  We present the first spatially resolved mid-infrared (37.1 $\mu$m) image of
the Fomalhaut debris disk. We use PSF fitting and subtraction to distinctly
measure the flux from the unresolved component and the debris disk. We measure
an infrared excess in the point source of $0.9 \pm 0.2$ Jy, consistent with
emission from warm dust in an inner disk structure (Su et al. 2016), and
inconsistent with a stellar wind origin. We cannot confirm or rule out the
presence of a pileup ring (Su et al. 2016) near the star. In the cold region,
the 37 $\mu$m imaging is sensitive to emission from small, blowout grains,
which is an excellent probe of the dust production rate from planetesimal
collisions. Under the assumptions that the dust grains are icy aggregates and
the debris disk is in steady state, this result is consistent with the dust
production rates predicted by Kenyon & Bromley (2008) from theoretical models
of icy planet formation. We find a dust luminosity of $(7.9 \pm 0.8) \times
10^{-4}$ L$_\odot$ and a dust mass of 8 -- 16 lunar masses, depending on grain
porosity, with $\sim 1$ lunar mass in grains with radius 1 $\mu$m -- 1 mm. If
the grains are icy and highly porous, meter-sized objects must be invoked to
explain the far-IR, submm, and mm emission. If the grains are composed of
astronomical silicates, there is a dearth of blowout grains (Pawellek et al.
2014) and the mass loss rate is well below the predicted dust production
values.
