8.7$\times$10$^3$ & 10.9 & 0.81 & 1.68\

Kinematic Results
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We first describe the two ingredients used to derive the kinematics of the NGC 4244 nuclear star cluster: (1) spectral templates, and (2) a method to determine the line-of-sight velocity distribution (LOSVD) from the binned spectra based on the templates.

Spectral templates were obtained from two sources. Three template stars were observed with NIFS by @davidge08 in a configuration identical to ours. Spectra for these stars were kindly provided by the author. Their spectral types: K1III, K5III, and M0III are representative of the spectral types of the red giant branch (RGB) and asymptotic giant branch (AGB) stars most likely to dominate our spectrum. We also use a larger library of spectral templates that has been observed by C. Winge using the somewhat higher resolution (3.35 Å FWHM) GNIRS spectrograph on Gemini South[^1]. This library contains stars from spectral type F7-M3 and includes dwarf, giant and some supergiant stars.

To determine the LOSVD of each spectrum we used the penalized pixel fitting (PPXF) method of @cappellari04. The program finds the best matching set of templates and convolves them to find the best fitting LOSVD, which is parametrized using a Gauss-Hermite series. 