This article has an erratum: [https://doi.org/10.1051/0004-6361/200811391e]
Volume 498, Number 1, April IV 2009
|Page(s)||161 - 165|
|Section||Interstellar and circumstellar matter|
|Published online||18 February 2009|
Chemical stratification in the Orion Bar: JCMT Spectral Legacy Survey observations
Kapteyn Astronomical Institute, PO Box 800, 9700 AV, Groningen, The Netherlands e-mail: firstname.lastname@example.org
2 SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV, Groningen, The Netherlands
3 I. Physikalisches Institut der Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany
4 Astrophysics Research Centre, School of Mathematics and Physics, Queen's University of Belfast, Belfast, BT7 1NN, UK
5 Jodrell Bank Centre for Astrophysics, Alan Turing Building, University of Manchester, Manchester, M13 9PL, UK
6 Department of Physics and Astronomy, University of Calgary, Calgary, T2N 1N4, AB, Canada
Accepted: 6 February 2009
Context. Photon-dominated regions (PDRs) are expected to show a layered structure in molecular abundances and emerging line emission, which is sensitive to the physical structure of the region as well as the UV radiation illuminating it.
Aims. We aim to study this layering in the Orion Bar, a prototypical nearby PDR with a favorable edge-on geometry.
Methods. We present new maps of fields at 14´´–23´´ resolution toward the Orion Bar in the SO 88–99, H2CO 515–414, 13CO 3–2, C2H 49/2–37/2 and 47/2–35/2, C18O 2–1 and HCN 3–2 transitions.
Results. The data reveal a clear chemical stratification pattern. The C2H emission peaks close to the ionization front, followed by H2CO and SO, while C18O, HCN and 13CO peak deeper into the cloud. A simple PDR model reproduces the observed stratification, although the SO emission is predicted to peak much deeper into the cloud than observed while the H2CO peak is predicted to peak closer to the ionization front than observed. In addition, the predicted SO abundance is higher than observed while the H2CO abundance is lower than observed.
Conclusions. The discrepancies between the models and observations indicate that more sophisticated models, including production of H2CO through grain surface chemistry, are needed to quantitatively match the observations of this region.
Key words: ISM: molecules / ISM: structure / ISM: individual objects: Orion Bar / stars: formation
© ESO, 2009
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