flux of the nuclear component by the flux expected from the point spread function as measured from the AGN continuum. Through this scaling, the size of the seeing disk as measured during the observation itself is automatically taken into account. For a more detailed description and the performance of these fits see @colletthesis and Nesvadba et al. (2017, in prep.).

Map construction {#ssec:mapconstruction}
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We constructed emission-line maps of these galaxies in very similar ways to the SINFONI samples previously analyzed by @nesvadba06a [@nesvadba08; @nesvadba11a], @collet14a [@collet14b], and Nesvadba et al. (2016, in prep.). Namely, we obtained integrated spectra from box apertures in each galaxy, covering 3$\times$3 pixels (0.4$\times$0.4). This is less than the size of the seeing disk, and corresponds to the spatial resolution that can be obtained with adaptive-optics assisted observations and a pixel scale of 125 mas$\times$250 mas (§\[ssec:obsdatred\]). This therefore minimizes pixel-to-pixel noise without introducing artificial beam-smearing effects. For galaxies where \[OIII\]$\lambda\lambda$4959,5007 is observed, we fitted the \[OIII\]$\lambda\lambda$4959,5007 lines first, which probe the same gas, and have a fixed flux ratio $R_{\rm 4959,5007}=1/3$. For most galaxies we use the \[OIII\]$\lambda$5007 maps to measure the morphology and kinematics of the warm ionized gas. In §\[ssec:oiiihacomparison\] we will 