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We present the first spatially resolved mid-infrared (37.1 $\mu$m) image ofthe Fomalhaut debris disk. We use PSF fitting and subtraction to distinctlymeasure the flux from the unresolved component and the debris disk. We measurean infrared excess in the point source of $0.9 \pm 0.2$ Jy, consistent withemission from warm dust in an inner disk structure (Su et al. 2016), andinconsistent with a stellar wind origin. We cannot confirm or rule out thepresence 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 planetesimalcollisions. Under the assumptions that the dust grains are icy aggregates andthe debris disk is in steady state, this result is consistent with the dustproduction rates predicted by Kenyon & Bromley (2008) from theoretical modelsof icy planet formation. We find a dust luminosity of $(7.9 \pm 0.8) \times10^{-4}$ L$_\odot$ and a dust mass of 8 -- 16 lunar masses, depending on grainporosity, with $\sim 1$ lunar mass in grains with radius 1 $\mu$m -- 1 mm. Ifthe grains are icy and highly porous, meter-sized objects must be invoked toexplain the far-IR, submm, and mm emission. If the grains are composed ofastronomical silicates, there is a dearth of blowout grains (Pawellek et al.2014) and the mass loss rate is well below the predicted dust productionvalues.

Dust Production Rates in the Fomalhaut Debris Disk from SOFIA/FORCAST Mid-infrared Imaging