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We present Herschel/SPIRE images at 250, 350, and 500 {\mu}m of NGC 4244, atypical low-mass, disk-only and edge-on spiral galaxy. The dust disk is clumpyand shows signs of truncation at the break radius of the stellar disk. Thisdisk coincides with the densest part of the Hi disk. We compare the SpectralEnergy Distribution, including the new SPIRE fluxes, to 3D radiative transfermodels; a smooth model disk and a clumpy model with embedded heating. Eachmodel requires a very high value for the dust scale-length (h(dust) = 2 - 5h(stars)), higher dust masses than previous models of NGC 4244 (Md = 0.47 -1.39 \times 10e7 Msun) and a face-on optical depth of {\tau}(V) = 0.4 - 1.12,in agreement with previous disk opacity studies. The vertical scales of starsand dust are similar. The clumpy model much better mimics the generalmorphology in the submm images and the general SED. The inferred gas-to-dustmass ratio is compatible with those of similar low-mass disks. The relativelylarge radial scale-length of the dust disk points to radial mixing of the dustyISM within the stellar disk. The large vertical dust scale and the clumpy dustdistribution of our SED model are both consistent with a scenario in which thevertical structure of the ISM is dictated by the balance of turbulence andself-gravity.

Herschel/SPIRE Observations of the Dusty Disk of NGC 4244