Montage of WC stars with weaker emission features due to dilution by emission from hot dust. LHO76 and −79 are shown again for ease of comparison. Note that sharp emission features between e.g. 2.1 μm and 2.11 μm and visible in LHO19, −42, −75, −84, and −102 are residual sky lines; we find no evidence for the putative secondaries in any spectra. HST/NICMOS F205W magnitudes are given in parentheses (Table A.1), although we note that dusty WCL are known to be photometrically variable. Finally for ease of comparison the five Quintuplet proper members are LHO19, −42, −75, −84, and −102 (=MGM 5–3, −2, −1, −4, and −9 respectively).