EXPANDED VERY LARGE ARRAY OBSERVATIONS OF THE H66α AND He66α RECOMBINATION LINES TOWARD MWC 349A

We have used the greatly enhanced spectral capabilities of the Expanded Very Large Array to observe both the 22.3 GHz continuum emission and the H66 alpha recombination line toward the well-studied Galactic emission-line star MWC 349A. The continuum flux density is found to be 411 +/- 41 mJy in good agreement with previous determinations. The H66 alpha line peak intensity is about 25 mJy, and the average line-to-continuum flux ratio is about 5%, as expected for local thermodynamic equilibrium conditions. This shows that the H66 alpha recombination line is not strongly masing as had previously been suggested, although a moderate maser contribution could be present. The H66 alpha recombination line is also detected in our observations; the relative strengths of the two recombination lines yield an ionized helium to ionized hydrogen abundance ratio y(+) = 0.12 +/- 0.02. The ionized helium appears to share the kinematics of the thermally excited ionized hydrogen gas, so the two species are likely to be well mixed. The electron temperature of the ionized gas in MWC 349A deduced from our observations is 6300 +/- 600 K.