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We observed the compact HII region, RCW 122C, at both 50 and 100 $\mu m$ with the University of Texas 20-channel $^{3}He$ cooled silicon bolometer array on the Kuiper Airborne Observatory (KAO) during March 7 through 16, 1993, flying from Christchurch, New Zealand. The FWHM of the beam is $18 \arcsec \times 25 \arcsec$ at $50 \mu m$ and $25 \arcsec \times 35 \arcsec$ at $100 \mu m$. While this source was detected as a single source by the IRAS and balloon-borne telescope (Ghosh et al. 1989, ApJS, 89, 233), our KAO data clearly show that RCW 122C actually consists of two sources. The two sources are separated by about $80 \arcsec$. The preliminary analysis has shown that the spectral types of the two exciting stars must not be earlier than O6 type. This work was supported by NASA grant NAG 2-67.
