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As part of a study of high mass star formation in the near (1-5 $\mu$m) infrared (NIR), we have imaged the bipolar nebula NS 14 at J (1.23 $\mu$m), H (1.65 $\mu$m), and K (2.23 $\mu$m) broadband NIR wavelengths. We have also obtained 3.29 $\mu$m dust feature emission and Br$\gamma$ (n = 7$\rightarrow$4, 2.166 $\mu$m) hydrogen recombination line emission images of this region. The broadband reflection nebulosity, surrounding a central `trapezium' of stars, forms a bipolar structure that is also seen in the 3.29 $\mu$m dust feature emission. The 3.29 $\mu$m emission is limb brightened, indicating that small dust grains in the central regions of the bipolar structure have been evacuated. The unresolved Br$\gamma$ emission in the vicinity of the hottest star (star A) in the trapezium is too high for what is expected from case B recombination based on radio measurements and previous estimates of extinction to the region. We have modeled this region with two components, an ionizing wind source and traditional nebular case B recombination in order to match the observations. A study of the stellar population of the cluster centered on the nebular emission has also been made.
