Volume 510, February 2010
|Number of page(s)||2|
|Section||Interstellar and circumstellar matter|
|Published online||18 February 2010|
Chemical stratification in the Orion Bar: JCMT spectral legacy survey observations (Corrigendum)
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
The integrated line intensities in Table 1 of Van der Wiel et al. (2009, A&A 498, 161) should be modified due to an error in the adopted channel widths: values are reduced by ~20% for C2H, H2CO and SO, reduced by a factor ~5 for C18O and HCN, and increased by ~40% for 13CO. Derived column densities for C2H, H2CO and SO are decreased by ~20%; for C18O it is increased by ~40%. Corrected abundance values of C2H, H2CO and SO are a factor <2 smaller than the originally published values. The values for HCN column densities and abundance are replaced by lower limits. Consequences for the discussion and conclusions are minor. In addition, the southwest arrow in Fig. 1 should be shifted to the southwest by ~10.
Key words: ISM: molecules / ISM: structure / ISM: individual: Orion Bar / stars: formation / errata, addenda
© ESO, 2010
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