IONIZED CARBON IN NGC-6334

We have observed the 158 mu m P-2(3/2)-P-2(1/2) fine-structure transition of C+ along the ridge of star formation in NGC 6334 with a velocity resolution comparable to that of millimeter-wave molecular and recombination lines. The C II radiation is bright and widespread, with integrated intensities I-int > 10(-4) ergs cm(-2) s(-1) sr(-1) along a line extending over 16'. There is a general correlation between regions of intense C II emission and warm dust and CO radiation, such as would be expected for phenomena which are all associated with star formation, but no small-scale correspondence is found. The C II excitation temperature is higher than that of the dust or CO. The line profiles are complex, with evidence for self-absorption as well as emission from H II regions. No single physical component of the gas appears responsible for the observed C II line profiles, as is usually the case for CO or recombination lines. Rather, the PDR, ionized gas, and colder or more tenuous material all contribute, with relative importance determined by the geometry and energetics of the region.