SPECTROSCOPY OF H-II REGIONS AT 2 MU-M - ULTRACOMPACT SOURCES

We have measured the line fluxes of Her 2.058 mu m and Br gamma 2.165 mu m from ultracompact (UC) H II regions excited by stars of spectral types 04 to B1. The ratio of these two lines is compared with theoreti cal predictions of the dependence of this ratio on the effective tempe rature of the exciting star(s) for electron densities of n(e) = 10(2), 10(4) and 10(6) cm(-3). From our observations, the He I 2.058 mu m/Br gamma ratio is approximately constant over this range of spectral typ es. Our observations are in good agreement with the theoretical model of Doyon, Puxley & Joseph for an electron temperature and density of T -e = 5 x 10(3) K, n(e) = 10(4) cm(-3) and a Galactic helium abundance of 0.1. Alternatively, for an electron temperature and density of T-e = 10(4) K and n(e) = 10(4) cm(-3) the He I linewidth must be increased from its Doppler value of 6 km s(-1) to about 17 km s(-1), e.g. by tu rbulent motions of the ionized gas, to be consistent with our observat ions. We also consider the role of telluric CO2 absorption on the He I recombination line at 2.058 mu m. Because of the intrinsic narrowness of the He I line (20-40 km s(-1)) the percentage of He I line flux re moved varies as the Earth revolves. For the observations presented her e, up to 36 per cent of the He I line is absorbed before it reaches th e telescope.