Continuum images. Top left: 321 GHz image of NGC 5793, with ﹩3\sigma ﹩, ﹩5\sigma ﹩, ﹩7\sigma ﹩, and ﹩10\sigma ﹩ contours in black (﹩1\sigma =0.39﹩ mJy beam⁻¹). Top right: 325 GHz image of NGC 5793, with ﹩3\sigma ﹩, ﹩6\sigma ﹩, ﹩10\sigma ﹩, ﹩15\sigma ﹩, and ﹩20\sigma ﹩ contours in black (﹩1\sigma =0.29﹩ mJy beam⁻¹). Center left: 321 GHz image of Circinus, with ﹩5\sigma ﹩, ﹩10\sigma ﹩, ﹩25\sigma ﹩, ﹩50\sigma ﹩, and ﹩75\sigma ﹩ contours in black (﹩1\sigma =0.48﹩ mJy beam⁻¹). Center right: 321 GHz image of NGC 4945, with ﹩4\sigma ﹩, ﹩8\sigma ﹩, ﹩15\sigma ﹩, ﹩25\sigma ﹩, and ﹩35\sigma ﹩ contours in black (﹩1\sigma =3.0﹩ mJy beam⁻¹). Bottom left: 321 GHz image of NGC 1068, with ﹩5\sigma ﹩, ﹩8\sigma ﹩, ﹩15\sigma ﹩, ﹩25\sigma ﹩, and ﹩45\sigma ﹩ contours in black (﹩1\sigma =0.42﹩ mJy beam⁻¹). Bottom right: 321 GHz image of NGC 1386, with ﹩4\sigma ﹩, ﹩6\sigma ﹩, ﹩8\sigma ﹩, ﹩10\sigma ﹩, and ﹩12\sigma ﹩ contours in black (﹩1\sigma =0.36﹩ mJy beam⁻¹). Half-power restoring beam shapes are shown at the bottom left of each image, and scale bars are shown at the bottom right. For NGC 5793, we adopt a Hubble law distance of 50 Mpc using ﹩{H}_{0}=70﹩ km s⁻¹ Mpc⁻¹. We use distances of 10.1 Mpc for NGC 1068 and 15.9 Mpc for NGC 1386; these were measured by Nasonova et al. (2011) and Tully et al. (2013), respectively, using the Tully–Fisher relation.