& K band Magnitude & Integration Time (s) & S/N & Aperture Size ($\prime\prime$)\
\[0.5ex\] 2MASS 0345$+$25 & 12.7 & 480 & 80$-$116 & 0.5\
BRI 0021$-$0214 & 10.6 & 480 & 158$-$184 & 0.6\
$\sigma$ Orionis 51 & 16.1 & 3600 & 29$-$59 & 0.23$^{1}$\
$\sigma$ Orionis 71 & 16.1 & 3600 & 34$-$73 & 0.26$^{1}$\
$\sigma$ Orionis J053$-$024 & 16.2 & 3600 & 22$-$44 & 0.26$^{1}$\
KPNO-Tau 1 & 13.7 & 1000 & 96$-$123 & 0.5\
KPNO-Tau 4 & 13.3 & 1000 & 102$-$133 & 0.5\
KPNO-Tau 12 & 14.9 & 1800 & 52$-$119 & 0.5\
2MASS 0535$-$0546 & 13.8 & 500 & 84$-$131 & 0.45\
0457$+$3015 & 14.5 & 1800 & 63$-$129 & 0.44\
\[1ex\]

152$-$717 & 17.6 & 6300 & 4$-$8 & 0.2$^{1}$\
\[1ex\] $^{1}$Observed using Adaptive Optics

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Raw data were reduced using the GEMINI NIFS package within IRAF. The reduction was made in three steps: a baseline calibration to produce a shift reference file, a flat field file, a flat bad pixel mask file, a wavelength referenced arc file, and a spatially referenced ronchi file; a telluric calibration reduction to produce a 1D spectrum of the standard star to be used for telluric calibration 