| Issue |
A&A
Volume 706, February 2026
|
|
|---|---|---|
| Article Number | C4 | |
| Number of page(s) | 1 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/202659182e | |
| Published online | 20 February 2026 | |
The extremely sharp transition between molecular and ionized gas in the Horsehead nebula (Corrigendum)
1
Instituto de Astrofísica, Pontificia Universidad Católica de Chile,
Av. Vicuña Mackenna 4860,
7820436
Macul, Santiago,
Chile
2
Núcleo Milenio de Formación Planetaria (NPF), Universidad de Valparaíso,
Av. Gran Bretaña 1111,
Valparaíso,
Chile
3
Instituto de Física Fundamental (CSIC),
Calle Serrano 121,
28006,
Madrid,
Spain
4
LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université,
92190
Meudon,
France
5
IRAM,
300 rue de la Piscine,
38406
Saint-Martin-d’Hères,
France
6
LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université,
75014
Paris,
France
7
Institut d’Astrophysique Spatiale, Université Paris-Saclay, CNRS,
Bâtiment 121,
91405
Orsay Cedex,
France
8
Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory,
439 92
Onsala,
Sweden
9
Joint ALMA Observatory,
Alonso de Cordova 3107 Vitacura,
Santiago,
Chile
10
Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire,
33615
Pessac,
France
11
Space Telescope Science Institute,
3700 San Martin Drive,
Baltimore,
MD
21218-2463,
USA
12
Steward Observatory, University of Arizona,
Tucson,
AZ,
85721,
USA
★ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.
Key words: astrochemistry / ISM: clouds / molecules / ISM: photon-dominated region (PDR) / errata, addenda
In the original publication, the thermal pressure estimated in Sect. 4.4, defined as Pth = nHTkin, was underestimated by a factor of two due to the conversion to the total hydrogen nuclei density, nH = n(H) + 2n(H2) ≃ 2nH2. As a result, the updated values correspond to Pth = (4.6–8.0) × 106 K cm−3, which are more consistent with the modeling results presented in Sect. 5. The discussion and conclusions of Hernández-Vera et al. (2023) remain unchanged, as the updated values are still of the same order of magnitude as those reported in the literature (Habart et al. 2005), and the relation Pth,PDR > Pth,H II still holds.
References
- Habart, E., Abergel, A., Walmsley, C. M., Teyssier, D., & Pety, J. 2005, A&A, 437, 177 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Hernández-Vera, C., Guzmán, V. V., Goicoechea, J. R., et al. 2023, A&A, 677, A152 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© The Authors 2026
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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