| Issue |
A&A
Volume 574, February 2015
|
|
|---|---|---|
| Article Number | C3 | |
| Number of page(s) | 2 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201424267e | |
| Published online | 27 January 2015 | |
Water in star-forming regions with Herschel (WISH)⋆ (Corrigendum)
V. The physical conditions in low-mass protostellar outflows revealed by multi-transition water observations
1
Leiden Observatory, Leiden University, PO Box 9513
2300 RA, Leiden, The Netherlands
e-mail: mottram@strw.leidenuniv.nl
2
Harvard-Smithsonian Center for Astrophysics, 60 Garden
Street, Cambridge,
MA
02138,
USA
3
Max Planck Institut für Extraterrestrische Physik,
Giessenbachstrasse 1,
85748
Garching,
Germany
4
Department of Astronomy, University of Michigan,
500 Church Street, Ann Arbor, MI
48109-1042,
USA
5
Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125
Florence,
Italy
6
Osservatorio Astronomico di Roma, via di Frascati 33, 00040
Monteporzio Catone,
Italy
7
Institute for Astronomy, ETH Zurich, 8093
Zurich,
Switzerland
8
School of Physics and Astronomy, University of
Leeds, Leeds
LS2 9JT,
UK
9
Université de Bordeaux, Observatoire Aquitain des Sciences de
l’Univers, 2 rue de
l’Observatoire, BP
89, 33270
Floirac Cedex,
France
10
CNRS, LAB, UMR 5804, Laboratoire d’Astrophysique de
Bordeaux, 2 rue de
l’Observatoire, BP
89, 33270
Floirac Cedex,
France
11
Joint Astronomy Centre, 660 North Aohoku Place, University
Park, Hilo,
HI
96720,
USA
12
Department of Physics and Astronomy, University of
Victoria, PO Box
3055
STN CSC, Victoria, BC
V8W 3P6,
Canada
13
NRC-Herzberg Institute of Astrophysics,
5071 West Saanich Road,
Victoria, BC
V9E 2E7,
Canada
14
Department of Earth and Space Sciences, Chalmers University of
Technology, Onsala Space Observatory, 439 92
Onsala,
Sweden
15
Observatorio Astronómico Nacional (IGN),
Alfonso XII 3, 28014
Madrid,
Spain
16
SRON Netherlands Institute for Space Research,
PO Box 800, 9700 AV
Groningen, The
Netherlands
17
Kapteyn Astronomical Institute, University of
Groningen, PO Box
800, 9700 AV
Groningen, The
Netherlands
18
Max-Planck-Institut für Radioastronomie,
Auf dem Hügel 69, 53121
Bonn,
Germany
Key words: stars: formation / ISM: jets and outflows / ISM: molecules / stars: protostars / errata, addenda
Detection statistics and average fraction of the total integrated intensity that each component contributes for each transition.
The original calculation of the fraction of the total integrated intensity in each component type presented in Table 4 of Mottram et al. (2014) did not correctly take into account the different distance corrections for the cavity shock compared to the spot shock and envelope components. For the cavity shock components a correction of (d/200 pc) was used, assuming that the emission is extended along the outflow axis but point-like perpendicular to it, while for the other components (d/200 pc)2 was used, assuming that both are point-like. The table given below provides the corrected values.
This primarily affects the contribution of the envelope, which is decreased in the corrected version, leading to a slight increase in the relative contribution of the cavity shock component. The correction does not change the discussion of the results or the conclusions drawn from them.
References
- Mottram, J. C., Kristensen, L. E., van Dishoeck, E. F., et al. 2014, A&A, 572, A21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© ESO, 2015
All Tables
Detection statistics and average fraction of the total integrated intensity that each component contributes for each transition.
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