| Issue |
A&A
Volume 579, July 2015
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201424568e | |
| Published online | 02 July 2015 | |
The chemistry and spatial distribution of small hydrocarbons in UV-irradiated molecular clouds: the Orion Bar PDR (Corrigendum)⋆
1 Grupo de Astrofísica Molecular. Instituto de Ciencia de Materiales de Madrid (ICMM, CSIC), Sor Juana Ines de la Cruz 3, 28049 Cantoblanco Madrid Spain
e-mail: s.cuadrado@icmm.csic.es
2 Centro de Astrobiología (CSIC-INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850 Madrid, Spain
3 Université de Toulouse, UPS-OMP, IRAP, 31062 Toulouse, France
4 CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
5 Observatorio Astronómico Nacional, Apdo. 112, 28803 Alcalá de Henares, Madrid, Spain
Key words: astrochemistry / photon-dominated region (PDR) / ISM: molecules / ISM: abundances / surveys / errata, addenda
In Sect. 3.2.1 (p. 5) of our original publication (Cuadrado et al. 2015), we stated that the centrifugal distortion constant, D, of l-C3H+ is higher than that of C3. However, the sentence should read “higher than that of linear C3H”. The D value of l-C3H+ is 7.6605 kHz (Cuadrado et al. 2015), while that of l-C3H is 5.1365 kHz (Yamamoto et al. 1990). For clarity, we note that the D constant of C3 is 44.099 kHz (Krieg et al. 2013). Botschwina et al. (2014) found a high degree of floppiness for l-C3H+ but not as high as that of C3. In addition, Stein et al. (2015) have recently computed that the lowest energy bending mode of l-C3H+ lies at 125.7 cm-1, which is about twice that of C3 (~63.4 cm-1, Schmuttenmaer et al. 1990).
Furthermore, p. 12 contained a typographical error on the total column density of hydrogen nuclei towards the dissociation front position. The correct NH = N(H)+2N(H2) value is NH = 6.3 × 1022 cm-2, with N(H) ≃ 3 × 1021 cm-2 and N(H2) ≃ 3 × 1022 cm-2. The molecular abundances, N(X)/NH,
derived from the column densities inferred from observations (Tables 4–6) were all computed using the correct NH value. Therefore, the numbers in the tables and the results of the paper remain unchanged.
Acknowledgments
The authors thank Christopher Stein and Evelyne Roueff for noting these errors in our original publication.
References
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