Volume 599, March 2017
|Number of page(s)||11|
|Section||Interstellar and circumstellar matter|
|Published online||21 February 2017|
Spatial distribution of far-infrared rotationally excited CH+ and OH emission lines in the Orion Bar photodissociation region⋆
1 Institut d’Astrophysique Spatiale, Université Paris-Saclay, 91405 Orsay Cedex, France
2 I. Physikalisches Institut der Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany
3 Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
4 Instituto de Ciencia de Materiales de Madrid, CSIC, Sor Juana Inés de la Cruz 3, 28049 Madrid, Spain
5 Université de Toulouse, UPS-OMP, IRAP, 31400 Toulouse, France
6 CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
7 LERMA, Observatoire de Paris, PSL Research University, École Normale Supérieure, CNRS, 75014 Paris, France
8 Sorbonne Universités, UPMC Paris 06, CNRS, LERMA, 75005 Paris, France
Received: 1 August 2016
Accepted: 12 September 2016
Context. The methylidyne cation (CH+) and hydroxyl (OH) are key molecules in the warm interstellar chemistry, but their formation and excitation mechanisms are not well understood. Their abundance and excitation are predicted to be enhanced by the presence of vibrationally excited H2 or hot gas (~500−1000 K) in photodissociation regions (PDRs) with high incident far-ultraviolet (FUV) radiation field. The excitation may also originate in dense gas (>105 cm-3) followed by nonreactive collisions with H2, H, and electrons. Previous observations of the Orion Bar suggest that the rotationally excited CH+ and OH correlate with the excited CO, which is a tracer of dense and warm gas, and that formation pumping contributes to CH+ excitation.
Aims. Our goal is to examine the spatial distribution of the rotationally excited CH+ and OH emission lines in the Orion Bar to establish their physical origin and main formation and excitation mechanisms.
Methods. We present spatially sampled maps of the CH+J = 3–2 transition at 119.8 μm and the OH Λ doublet at 84 μm in the Orion Bar over an area of 110″× 110″ with Herschel/PACS. We compare the spatial distribution of these molecules with those of their chemical precursors, C+, O and H2, and tracers of warm and dense gas (high-J CO). We assess the spatial variation of the CH+J = 2–1 velocity-resolved line profile at 1669 GHz with Herschel/HIFI spectrometer observations.
Results. The OH and especially CH+ lines correlate well with the high-J CO emission and delineate the warm and dense molecular region at the edge of the Bar. While notably similar, the differences in the CH+ and OH morphologies indicate that CH+ formation and excitation are strongly related to the observed vibrationally excited H2. This, together with the observed broad CH+ line widths, indicates that formation pumping contributes to the excitation of this reactive molecular ion. Interestingly, the peak of the rotationally excited OH 84 μm emission coincides with a bright young object, proplyd 244–440, which shows that OH can be an excellent tracer of UV-irradiated dense gas.
Conclusions. The spatial distribution of CH+ and OH revealed in our maps is consistent with previous modeling studies. Both formation pumping and nonreactive collisions in a UV-irradiated dense gas are important CH+J = 3–2 excitation processes. The excitation of the OH Λ doublet at 84 μm is mainly sensitive to the temperature and density.
Key words: ISM: individual objects: Orion Bar / ISM: lines and bands / photon-dominated region (PDR)
© ESO, 2017
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