NFTELLURIC program, which allows for interactive correction of the small differences in the wavelength calibration and airmass between the observations of the calibrator and each exposure. The final data cubes from each individual on-source exposure were combined using GEMCOMBINE correcting for spatial and spectral offsets. The resulting data cube has a $\sim$3$\arcsec$$\times$3$\arcsec$ field of view with 0.05$\arcsec$ spatial pixels and 2.132 Å spectral pixels from 2.00-2.44 $\mu$m. Based on measurements of the sky lines, the spectral resolution is $\sim$4.1Å (53 kms$^{-1}$) FWHM. The spatial resolution in the combined image was measured using four compact sources after subtracting the NSC model (§3.1) and found to be 0.23$\arcsec$ FWHM. These four compact sources are shown as crosses in Fig. \[firstfig\]; three of the four are also detected as point-like sources in the higher resolution (0.08$\arcsec$ FWHM) HST images. The spatial resolution of our data cube is roughly $\sim$2$\times$ lower than that achieved when using a brighter tip/tilt star (e.g. for our telluric calibrators).

A spectrum from the inner 0.1$\arcsec$ of the cluster is shown in Fig. \[firstfig\]. The plotted spectrum is the normalized flux ratio of the galaxy spectrum to the Br$\gamma$-corrected A0V telluric calibrator spectrum. All the spectral analysis presented below 