Chemical stratification in the Orion Bar: JCMT spectral legacy survey observations (Corrigendum)

M. H. D. van der Wiel^1,2, F. F. S. van der Tak^2,1, V. Ossenkopf^3,2, M. Spaans¹, H. Roberts⁴, G. A. Fuller⁵ and R. Plume⁶

¹ Kapteyn Astronomical Institute, PO Box 800, 9700 AV, Groningen, The Netherlands e-mail: wiel@astro.rug.nl
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

Abstract

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.