| Issue |
A&A
Volume 702, October 2025
|
|
|---|---|---|
| Article Number | C6 | |
| Number of page(s) | 2 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/202556847e | |
| Published online | 27 October 2025 | |
ALMA-IMF
XVIII. The assembly of a star cluster: Dense N2H+ (1−0) kinematics in the massive G351.77 protocluster (Corrigendum)
1
Departamento de Astronomía, Universidad de Concepción,
Casilla 160-C,
Concepción,
Chile
2
Franco-Chilean Laboratory for Astronomy, IRL 3386, CNRS and Universidad de Chile,
Santiago,
Chile
3
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México,
Morelia, Michoacán
58089,
Mexico
4
Univ. Grenoble Alpes, CNRS, IPAG,
38000
Grenoble,
France
5
Department of Astronomy, University of Florida,
PO Box 112055,
Gainesville,
FL
32611,
USA
6
SKA Observatory, Jodrell Bank,
Lower Withington,
Macclesfield
SK11 9FT,
UK
7
Max-Planck-Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg,
Germany
8
European Southern Observatory,
Karl-Schwarzschild-Strasse 2,
85748
Garching,
Germany
9
Max-Planck-Institut für Extraterrestrische Physik,
Giessenbachstrasse 1,
85748
Garching,
Germany
10
Departments of Astronomy and Chemistry, University of Virginia,
Charlottesville,
VA
22904,
USA
11
Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N,
allée Geoffroy Saint-Hilaire,
33615
Pessac,
France
12
Astronomy Department, Universidad de Chile,
Casilla 36-D,
Santiago,
Chile
13
Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB),
Martí i Franquès 1,
08028
Barcelona, Catalonia,
Spain
14
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona,
Martí i Franquès 1,
08028
Barcelona, Catalonia,
Spain
15
Institut d’Estudis Espacials (IEEC),
Esteve Terradas 1, Edifici RDIT, Ofic. 212 Parc Mediterrani de la Tecnologia (PMT) Campus del Baix Llobregat – UPC
08860
Castelldefels (Barcelona),
Catalonia,
Spain
16
Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, UMR 5804,
33615
Pessac,
France
17
NRC Herzberg Astronomy and Astrophysics Research Centre,
5071 West Saanich Road,
Victoria,
BC
V9E 2E7,
Canada
18
Instituto Argentino de Radioastronomía (CCT-La Plata, CONICET; UNLP; CICPBA),
C.C. No. 5, 1894,
Villa Elisa,
Buenos Aires,
Argentina
19
Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS,
Beijing
100101,
China
20
Instituto de Astronomía, Universidad Católica del Norte,
Av. Angamos
0610,
Antofagasta,
Chile
21
Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité,
75005
Paris,
France
22
Observatoire de Paris, PSL University, Sorbonne Université, LERMA,
75014
Paris,
France
23
School of Physics and Astronomy, Yunnan University,
Kunming
650091,
PR China
24
Department of Earth and Planetary Sciences, Institute of Science Tokyo,
Meguro, Tokyo
152-8551,
Japan
25
National Astronomical Observatory of Japan, National Institutes of Natural Sciences,
2-21-1 Osawa,
Mitaka, Tokyo
181-8588,
Japan
★ Corresponding author: nsandovalgarrido@gmail.com
Key words: stars: formation / ISM: clouds / ISM: kinematics and dynamics / ISM: molecules / errata, addenda
In the original version of this paper, at the end of Sect. 3.4 we described Eq. (1).
(1)
as follows: "where < VLSR,1 > and < VLSR,2 > are the averaged centroid velocities of the first and second velocity component, respectively,
and
are the standard deviations of the centroid velocities in the first and second velocity component, respectively, and X represents the cut-off value used as the middle point, normalized by the standard deviations of the centroid velocity distributions. Applying Eq. (1) we obtain a X=0.025. This value allows us to separate the centroid velocity distribution of the one-velocity-component fit into two parts and combine the measurements with the first and the second velocity component.”
The corrected text should read:
where < VLSR,1 > and < VLSR,2 > are the averaged centroid velocities of the first and second velocity component, respectively, and
and
are the standard deviations of the centroid velocities in the first and second velocity component, respectively. Here, X represents the parameter used to derive the velocity corresponding to the middle point. Applying Eq. (1), we obtain X ≈ 0.86, which yields a middle point of 0.025 km s−1. This value allows us to separate the centroid velocity distribution of the one-velocity-component fit into two parts and combine the measurements with the first and the second velocity component.
In addition, the caption of Fig. 3 should be corrected as follows:
Centroid velocity distributions of the one- and two-velocity-components fits. The black histogram represents the centroid velocity distribution of the spectra fit by the one-velocity-component model. The blue and red histograms show the centroid velocity distributions of the spectra fit with the two-velocity-components model, where blue corresponds to the first velocity component and red to the second. The solid black line represents the middle point located at 0.025 km s−1, measured via Eq. (1) (see text). This divides the black histogram into two velocities, as explained in Sect. 3.4.
© The Authors 2025
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