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tokens: cube is the removal of the continuum and determination of the stellar kinematics. Because both the MUSE and SINFONI spectral resolutions are only moderate, we only fit for the stellar velocity and velocity dispersion. We also included an additive fourth degree polynomial in the fit to model any emission from the central AGN. To create the continuum-subtracted MUSE cube, we renormalized the best-fitting binned spectra to the median continuum level of each individual spectrum before subtraction. Fig. 4 shows the results of our ppxf fits for the MUSE cube. Figure 4. Results from fitting the MUSE cube with ppxf . The top row plots the stellar velocity ( left ) and dispersion ( right ). The bottom row plots the mean light-weighted stellar population age ( left ) and mean light-weighted metallicity ( right ). In all frames, North is up and East is to the left. 2.6.2 Emission line fitting To measure the bulk distribution and kinematics of the molecular and ionized gas in NGC 5728, we fit single Gaussians to the relevant emission line tracers of the gas. In particular, we fit the CO (2–1) line (ν rest = 230.538 GHz) in the ALMA cube; the H β, [O iii ] doublet, [O i ], [N ii ] doublet, H α, and [S ii ] doublet lines in the MUSE cube; and the [Fe ii ]λ1.64 m, [Si vi ], H 2 (1–0) S(1), and Brγ lines in the SINFONI cube. This set of lines represent the strongest emission lines observed in nearby galaxies and AGNs and provide diagnostic power into the state of gas in a range of phases from cold molecular gas [CO (2–1)] to warm molecular gas [H 2 (1–0) S(1)] to hydrogen recombination lines (H β, H α, Br γ) and forbidden lines ([O iii ], [O i ], [N ii ], [S ii ], [Fe ii ], [Si vi ]) from ionized gas in a range of ionization levels. For each line, we cut out the relevant sections of the continuum-subtracted spectra that contain the single line or multiple lines in the case of the [O iii ] doublet, H α and [N ii ] blended region, and [S ii ] doublet. We fixed the velocity and velocity dispersion to be the same for all doublets and fixed the intensity ratio to the expected theoretical value of 3 for the [O iii ] and [N ii ] doublets. For the fit of the [Si vi ] line, we also included Gaussian components for the nearby H 2 (1–0) S(3) and Br δ lines. As an estimate of the local noise around each line, we measured the root mean square (RMS) of the line-free regions. Using the RMS, we produced 100 simulated spectra for every emission line by randomly perturbing the original spectra assuming a Gaussian distribution with a standard deviation equal to the RMS. Each of the simulated spectra were fit in the same way as the original spectra and uncertainties on the integrated flux, velocity, and velocity dispersion were calculated from the standard deviation of the best-fitting values from the simulated spectra. Finally, all velocity dispersions derived from MUSE and SINFONI data were corrected for instrumental broadening. For lines from MUSE, we assumed an