Active galactic nuclei (AGNs) are a key component of galaxy evolution due tofeedback on the host from its supermassive black hole. The morphology of warm,in- and outflowing dusty material can reveal the nature of the onset offeedback, AGN feeding, and the unified model of AGN. Here we use the LargeBinocular Telescope Interferometer (LBTI) to image the dense, obscuring diskand extended dusty outflow region of NGC 1068. In Fizeau imaging mode the LBTIsynthesizes the equivalent resolution of a 22.8 m telescope. The 8.7 $\mu$mFizeau images of NGC 1068 {have an effective resolution of $47\times90$ mas($3.3\times6.2$ pc)} in a 5" field of view after performing PSF deconvolutiontechniques described here. This is the only extragalactic source to be Fizeauimaged using the LBTI, and the images bridge the scales measured with the VeryLarge Telescope Interferometer (VLTI; 0.5-5 pc) and those of single telescopessuch as JWST and Keck ($>15$ pc). The images detect and spatially resolve thelow surface brightness mid-infrared (MIR) features in the AGN disk/wind regionthat are over-resolved by the VLTI. The images show strong correlation betweenMIR dust emission and near-infrared (NIR) emission of highly excited atomiclines observed by SINFONI. Such LBTI imaging is a precursor to infrared imagingusing the upcoming generation of extremely large telescopes, with angularresolutions up to 6x better than JWST, the largest space telescope in orbit.

The study of scaling relations of disc galaxies and their evolution acrosscosmic time requires accurate estimates of galaxy stellar masses $M_\star$ overbroad redshift ranges. While photometric $M_\star$ estimates ($M_{\rm phot}$)based on spectral energy distribution (SED) modelling methods are employedroutinely at high-$z$, it is unclear to what extent these are compatible withdynamical $M_\star$ estimates ($M_{\rm dyn}$), available for nearby galaxies.Here we compare newly determined, SED-model based $M_{\rm phot}$ withpreviously obtained $M_{\rm dyn}$ inferred via rotation curve decompositiontechniques in a sample of $\sim100$ nearby galaxies from the SPARC database. Wefind that the two mass estimates show a systematic agreement at the $\sim12\%$($0.05$ dex) level and a $\sim55\%$ ($0.22$ dex) scatter across almost $5$ dexin $M_\star$. Our $M_{\rm phot}$ estimates correspond to mass-to-light ratiosin the $3.6\mu$m band that increase gradually with $3.6\mu$m luminosity, as aconsequence of the earlier (later) assembly history of high-mass (low-mass)disc galaxies. The choice of using either $M_{\rm dyn}$ or $M_{\rm phot}$ hasonly a marginal impact on the slope and zero-point of the Tully-Fisher and Fallrelations: the observed orthogonal scatter in both relations is virtually thesame for the two methods, and indistinguishable from that derived using aconstant mass-to-light ratio in the $3.6\mu$m band. $M_\star$ estimates basedon the assumption that discs are marginally stable lead to the largest scatterin the scaling relations.