Phillips , T.G. and Bergin, E.A. and Lis, D.C. and Neufeld, D.A. and Bell, T.A. and Wang, S. and Crockett, N.R. and Emprechtinger, M. and Blake, G.A. and Caux, E. and Ceccarelli, C. and Cernicharo, J. and Comito, C. and Daniel, F. and Dubernet, M.-L. and Encrenaz, P. and Gerin, M. and Giesen, T.F. and Goicoechea, J.R. and Goldsmith, P.F. and Herbst, E. and Joblin, C. and Johnstone, D. and Langer, W.D. and Latter, W.D. and Lord, S.D. and Maret, S. and Martin, P.G. and Melnick, G.J. and Menten, K.M. and Morris, P. and Muller, H.S.P. and Murphy, J.A. and Ossenkopf, V. and Pearson, J.C. and Perault, M. and Plume, R. and Qin, S.-L. and Schilke, P. and Schlemmer, S. and Stutzki, J. and Trappe, N. and van der Tak, F.F.S. and Vastel, C. and Yorke, H.W. and Yu, S. and Zmuidzinas, J. and Boogert, A. and Gusten, R. and Hartogh, P. and Honingh, N. and Kooi, J. and Karpov, A. and Krieg, J.-M. and Schieder, R.
Herschel observations of EXtra-Ordinary Sources (HEXOS):
Detection of hydrogen fluoride in absorption towards Orion KL.
Astronomy & Astrophysics, 518 (L109).
We report a detection of the fundamental rotational transition of hydrogen fluoride in absorption towards Orion KL using Herschel/HIFI. After the
removal of contaminating features associated with common molecules (“weeds”), the HF spectrum shows a P-Cygni profile, with weak redshifted
emission and strong blue-shifted absorption, associated with the low-velocity molecular outflow. We derive an estimate of 2.9 × 1013 cm−2 for the
HF column density responsible for the broad absorption component. Using our best estimate of the H2 column density within the low-velocity
molecular outflow, we obtain a lower limit of ∼1.6 × 10−10 for the HF abundance relative to hydrogen nuclei, corresponding to ∼0.6% of the solar
abundance of fluorine. This value is close to that inferred from previous ISO observations of HF J = 2−1 absorption towards Sgr B2, but is in
sharp contrast to the lower limit of 6 × 10−9 derived by Neufeld et al. for cold, foreground clouds on the line of sight towards G10.6-0.4.
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