An 8.5 GHz Arecibo survey of Carbon Recombination Lines toward Ultra-compact \HII regions: Physical properties of dense molecular material

Details An 8.5 GHz Arecibo survey of Carbon Recombination Lines toward Ultra-compact \HII regions: Physical properties of dense molecular material An 8.5 GHz Arecibo survey of Carbon Recombination Lines toward Ultra-compact \HII regions: Physical properties of dense molecular material

2005-01-29

arxiv.org/abs/astro-ph/0501650v1

Astrophys.J. 625 (2005) 181-193

Astronomy and Astrophysics

Astrophysics

28 pages, 7 figures, 5 tables (accepted for publication in ApJ)

Scientific paper

10.1086/429313

We report here on a survey of carbon recombination lines (RLs) near 8.5 GHz toward 17 ultra-compact \HII regions (\UCHII s). Carbon RLs are detected in 11 directions, indicating the presence of dense photodissociation regions (PDRs) associated with the \UCHII s. In this paper, we show that the carbon RLs provide important, complementary information on the kinematics and physical properties of the ambient medium near \UCHII s. Non-LTE models for the carbon line forming region are developed, assuming that the PDRs surround the \UCHII s, and we constrained the model parameters by multi-frequency RL data. Modeling shows that carbon RL emission near 8.5 GHz is dominated by stimulated emission and hence we preferentially observe the PDR material that is in front of the \UCHII continuum. We find that the relative motion between ionized gas and the associated PDR is about half that estimated earlier, and has an RMS velocity difference of 3.3 \kms. Our models also give estimates for the PDR density and pressure. We found that the neutral density of PDRs is typically $>$ 5 $\times$ 10$^5$ \cmthree and \UCHII s can be embedded in regions with high ambient pressure. Our results are consistent with a pressure confined \HII region model where the stars are moving relative to the cloud core. Other models cannot be ruled out, however. Interestingly, in most cases, the PDR pressure is an order of magnitude larger than the pressure of the ionized gas. Further investigation is needed to understand this large pressure difference.

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