used as a telluric calibrator. The exposures all had similar image quality, with the PSF FWHM varying by $<$30% between the exposures. We note that H-band spectral observations of the NGC 4244 NSC were obtained as well, but due to a number of observational problems and a significantly lower resolution, these data are not discussed here.

The data were reduced using the Gemini v. 1.9 IRAF package, utilizing pipelines based on the NIFSEXAMPLES scripts. To obtain a clean telluric absorption spectra from the HIP50459 observations, the spectra were processed as described for the science images below, after which 1-D spectra were extracted and the Br$\gamma$ absorption line was fit and removed.

For the science exposures, an off-source exposure was subtracted from each on-source exposure; for the February 9 data only one off-source exposure was available and was thus subtracted from both images. The images were then sliced up and rectified based on Ronchi mask and arc lamp images using NFTRANSFORM and spatially rebinned into image cubes using NIFCUBE. In this process, the original 0.043$\times$0.1$\arcsec$ pixels get rebinned into 0.05$\arcsec$ pixels which are block replicated in the long (slice) direction. Each data cube was then corrected for telluric absorption using the 