Abstract
The strength of the He I 2.06 μm emission line relative to hydrogen recombination features has been previously proposed as a diagnostic of effective temperature T eff for stars powering H II regions. Such an indicator would be of particular interest for constraining the high-end initial mass function in starbursts. I reexamine the sensitivity of the 2.06 μm feature to nebular conditions, and find that constraints on the ionizing continuum shape are difficult to determine in the absence of additional constraints on nebular properties
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