2013ApJ...764..188I

We report the first detection of the v = 1-0, R(0) ro-vibrational transition of HF at 2.499385 µm arising from interstellar gas. The line is seen in absorption toward three background sources–HD 154368, Elias 29, and AFGL 2136 IRS 1–all of which have reported H₂ column densities determined from observations of H₂. This allows for the first direct determination of the HF/H₂ abundance ratio. We find values of N(HF)/N(H₂) = 1.15x10^–8 and 0.69x10^–8 for HD 154368 and Elias 29, respectively. The sight line toward AFGL 2136 IRS 1 also shows absorption from the v = 1-0, R(1) transition of HF, indicating warm, dense (n_H ≳ 10⁹/cm3) gas, likely very close to the central protostar. Ascribing portions of the HF absorption to warm and cold gas, we find N(HF)/N(H₂) = (1.7-2.9)x10^–8 and (0.33-0.58) x10^–8 for the two components, respectively. Except for the warm component toward AFGL 2136 IRS 1, all observed HF/H₂ ratios are well below N(HF)/N(H₂) = 3.6x10^–8, the value predicted if nearly all gas phase fluorine is in the form of HF. Models of fluorine chemistry that account for depletion onto grains are able to reproduce the results toward HD 154368, but not in the cold, dense gas toward AFGL 2136 IRS 1 and Elias 29. Most likely, some combinations of simplifying assumptions made in the chemical models are responsible for these discrepancies.