VLA RECOMBINATION LINE OBSERVATIONS OF THE COMETARY H-II-REGION G34.3- DYNAMICS AND PHYSICAL-PROPERTIES(0.2 )

We have observed the H93 alpha radio recombination line emission towar d the cometary H II region G34.3+0.2 component C. A velocity gradient with a total extent of approximate to 35 km s(-1) is found in the H93 alpha line emission perpendicular to the symmetry axis of the cometary H II region. A smaller velocity gradient is found parallel to the sym metry axis. The moving star bow shock model and the champagne outflow model have been suggested to explain observations of G34.3+0.2C. Neith er model adequately matches the available velocity data. G34.3+0.2 com ponents A and B are found near G34.3+0.2C. The continuum spectral indi ces of components A and B are consistent with that expected for an ion ized wind outflow. We suggest a qualitative model for the region where the ionizing star of the cometary H II region G34.3+0.2C photoevapora tes material from a hot ultracompact molecular core found just to the east of the continuum emission. Interaction between the ionized gas of the cometary H II region and winds from components A and B may explai n many of the current observations. We have also mapped the 6(16) --> 5(23) transition of H2O toward G34.3+0.2. We find strong H2O maser emi ssion within a approximate to 50'' x 30'' region. Some of the H2O mase rs are projected onto sources of radio continuum emission, but others are found well separated from radio continuum emission.