# Herschel CHESS discovery of the fossil cloud that gave birth to the Trapezium and Orion KL (Corrigendum)

A. López-Sepulcre, M. Kama, C. Ceccarelli, C. Dominik, E. Caux, A. Fuente, T. Alonso-Albi

► To cite this version:

A. López-Sepulcre, M. Kama, C. Ceccarelli, C. Dominik, E. Caux, et al., Herschel CHESS discovery of the fossil cloud that gave birth to the Trapezium and Orion KL (Corrigendum). Astronomy and Astrophysics - A&A, 2013, 553, 10.1051/0004-6361/201219416e. insu-03617078

HAL Id: insu-03617078

https://insu.hal.science/insu-03617078

Submitted on 23 Mar 2022

HAL is a multi-disciplinary open access
archive for the deposit and dissemination of sci-
entific research documents, whether they are pub-
lished or not. The documents may come from
teaching and research institutions in France or
abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est
destinée au dépôt et à la diffusion de documents
scientifiques de niveau recherche, publiés ou non,
émanant des établissements d'enseignement et de
recherche français ou étrangers, des laboratoires
publics ou privés.

<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
# Herschel CHESS discovery of the fossil cloud that gave birth to the Trapezium and Orion KL
(Corrigendum)

A. López-Sepulcre<fnref n="1" />, M. Kama<fnref n="2" />, C. Ceccarelli<fnref n="1" />, C. Dominik<fnref n="2" />,<fnref n="3" />, E. Caux<fnref n="4" />,<fnref n="5" />, A. Fuente<fnref n="6" />, and T. Alonso-Albi<fnref n="6" />

A&A 549, A114 (2013), DOI: 10.1051/0004-6361/201219416

**Key words.** astrochemistry – ISM: abundances – ISM: molecules – ISM: clouds – photon-dominated region (PDR) – errata, addenda

An error occurred during the production process. The right panel of Fig. 1 was the same as the left one. The correct Fig. 1 is shown here.

<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Spectral lines detected in absorption towards OMC-2 FIR 4. The green vertical lines mark $V_{LSR} = 9.3 \text{ km s}^{-1}$, i.e. the systemic velocity of the OH$^+$ lines.</figcaption></figure>

<footnote n="1">¹ UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France
e-mail: ana.sepulcre@obs.ujf-grenoble.fr</footnote>

<footnote n="2">² Astronomical Institute Anton Pannekoek, University of Amsterdam, Amsterdam, The Netherlands</footnote>

<footnote n="3">³ Department of Astrophysics/IMAPP, Radboud University Nijmegen, Nijmegen, The Netherlands</footnote>

<footnote n="4">⁴ Université de Toulouse, UPS-OMP, IRAP, Toulouse, France</footnote>

<footnote n="5">5 CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France</footnote>

<footnote n="6">⁶ Observatorio Astronómico Nacional, PO Box 112, 28803 Alcalá de Henares, Madrid, Spain</footnote>