Fits to stellar kinematic observables and the photometric light profile. The profiles are a function of projected radius at the assumed distance of 5.2 kpc. The green lines and bands correspond to the maximum posterior values, and the 68 and 95% CL centered at the median (respectively). For comparison, the gray (gray-dashed) line indicates the velocity dispersion obtained when a fraction of the dark component in the maximum posterior result is concentrated in the form of a 40 000 (10 000) M_⊙ IMBH. Such IMBH models are strongly disfavored in our analysis. The stellar stellar kinematics datasets are described in Sect. 3. All data, including the photometric profile, have been self-consistently binned with the center from Anderson & Van der Marel (2010). Upper left: tangential proper motion velocity dispersion. Upper middle: radial proper motion velocity dispersion. Upper right: LOS velocity dispersion. Lower left: surface brightness profile used to determine the photometric component of the distribution. The red line shows the best-fit profile that was used throughout the analysis (see Sect. 2 for details). For presentation purposes, this profile has been normalized to match the central luminosity density of Trager et al. (1995) after correcting for extinction using the same approach as in Zocchi et al. (2017) with the reddening reported in Harris (1996) (2010 edition) catalog. Lower middle: posterior distribution for the virial shape parameter 1 as a result of the fits, with the red data point indicating the value with 1σ errors computed by binulator (see Sect. 3). Lower right: the same as the lower left figure, but for the virial shape parameter 2.