Fig. A.1.
Additional cluster supergiants (black) of spectral type O7–8 by virtue of He II 2.189 μm absorption and/or C IV 2.079 μm emission. Spectra of cluster members of comparable spectral type overplotted in blue for comparison. The weakness of He II 2.189 μm in LHO118, −144 and −149 marks them as of the latest spectral type, with C IV 2.079 μm emission also apparently absent in LHO118. Note apparent infilling of Brγ in LHO31, −69, −73, −118 and −144. Emission in the Brγ profile of LHO16 is suspected to be part nebular in origin, while the depth of Brγ absorption in LHO149 is probably due to subtraction of the nebular-contaminated sky frame. HST/NICMOS F205W magnitudes are given in parentheses (Table A.1).
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