tokens: Sérsic fit, finding good agreement within 2%–3%. Therefore, we did not adjust our stellar mass for missing light. 3. Analysis 3.1. Velocity Dispersion We measure the observed stellar line-of-sight velocity dispersions (LOSVD) of our galaxy sample using pPXF (Cappellari 2017 ), which utilizes a maximum penalized likelihood approach to fitting spectra to a library of stellar or stellar population templates and determines galaxy kinematics. For our analysis, we use the Indo–US stellar library templates (Valdes et al. 2004 ) with R ∼4200, which are smoothed to the binned resolution of the reduced spectra of R ∼3000. We mask out portions of the spectra where telluric atmospheric absorption bands are significant and also where the spectra are potentially impacted by [O ii ] or [O iii ] emission lines. Good fits to the continuum are obtained for all galaxies, as shown in Figure 1 . We do not introduce additional freedom (e.g., additive/multiplicative polynomial) to attempt better match to the continuum. The results are not sensitive to this choice. As our 1D spectra are optimally extracted with a Gaussian kernel based on the PSF, i.e., seeing-limited, we correct our velocity dispersions within the aperture to velocity dispersions within r e as per van de Sande et al. ( 2013 ), resulting in a mean correction of 0.02 dex. The measured velocity dispersions including aperture corrections are shown in Table 2 . We find large velocity dispersions for all galaxies ranging from 200 − 300 km s −1 . We derive LOSVD uncertainties using Monte Carlo simulations. We take the best-fit spectrum to the observed data from pPXF and perturb its flux 1000 times by a random value drawn from a Gaussian with a standard deviation consistent with the uncertainties of the observed spectrum (determined as outlined in Section 2.2 ). The LOSVD for each iteration is determined and the standard deviation of all 1000 Monte Carlo simulations is used as the error for the LOSVD. These errors are larger than the formal pPXF uncertainties by a factor of 1.1–2.2. To test potential systematic errors of our measurements, we ran pPXF for multiple scenarios. We exclude the H β line and find consistent results, suggesting that emission line-infilling is not significant for these galaxies. To explore dependence on stellar library, we use the MILES stellar library (Sanchez-Blazquez et al. 2006 ; Falcón-Barroso et al. 2011 ) and find that the results agree within the uncertainties. To investigate stability and consistency, we take the best-fit spectrum for each galaxy and smooth it to simulate different velocity dispersions, perturbing the flux by observational errors as per the Monte Carlo simulation above. We are able to recover velocity dispersions for the range 150–500 km s −1 within the pPXF uncertainties, which shows that we should be able to recover dispersions and uncertainties from data of this quality. The median residuals for the recovered velocity dispersions are small (≲17 km s −1
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