fitting model (described below) to the magnitude of the source in the 2MASS Point Source Catalog [$K_s$=13.55; @2mass_psc]. Based on the variation between models and the uncertainty in the sky-level on our image, this zeropoint should be good to $\sim$10%. The image and calibrated contours are shown in the bottom panel of Fig. \[firstfig\].

Results
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In this section, we present results from our Gemini/NIFS K-band observations. We first discuss morphological fits to our high resolution K-band image (§3.1). We then present the kinematics of the cluster in §3.2 and its stellar populations in §3.3. The most significant finding is that the NGC 4244 NSC is strongly rotating. Comparison of the kinematics to the stellar populations and morphological fits shows that this rotation is occuring even off the major-axis of the cluster where older stellar populations appear to dominate.

Morphological Results
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We briefly describe our analysis of the morphology of the NGC 4244 NSC using the high resolution K-band image of the cluster created from our Gemini/NIFS data. This information is used in §3.3 to argue that the entire cluster is rotating, and will be used as input for dynamical modeling [@delorenzi08] using NMAGIC code [@delorenzi07].

As we found 