HII region offset by 19 pc along the major axis of the cluster gives a lower-limit to the mass of $\sim$2.5$\times$10$^6$ M$_\odot$. This mass measurement is consistent with the masses derived from the stellar population fitting of the spectrum as well.

In §2 we describe the observations and data reduction. Our results on the kinematics, morphology and stellar populations of the cluster are presented in §3. We discuss the results in the context of other galaxies and formation models in §4.

Observations & Data Reduction
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K-band spectra of the NGC 4244 nuclear star cluster were obtained using the Near-Infrared Integral Field Spectrograph (NIFS) on Gemini North, an image-slicing integral field unit spectrograph. The spectrograph was used in conjunction with the ALTAIR Laser Guide Star system. The cluster itself was used as a tip/tilt star, but is too faint ($r$=16.18) to get the highest-Strehl performance. The cluster was observed in K-band on the nights of February 9 and April 29 2007. In total 5$\times$900 second exposures were obtained on-source and 4$\times$900 sec exposures off-source (sky). The airmass of the observations ranged between 1.11 and 1.42, and an A0 star, HIP50459 was observed on both nights at similar airmass to be 