| Issue |
A&A
Volume 551, March 2013
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361/201118566e | |
| Published online | 11 February 2013 | |
Cluster-formation in the Rosette molecular cloud at the junctions of filaments (Corrigendum)
1
IRFU/SAp CEA/DSM, Laboratoire AIM CNRS – Université Paris
Diderot,
91191
Gif-sur-Yvette,
France
e-mail: nschneid@cea.fr
2
Max-Planck Institut für Radioastronomie,
Auf dem Hügel, Bonn, Germany
3
Monash Centre for Astrophysics (MoCA), School of Mathematical
Sciences, Monash University, 3800
Victoria,
Australia
4
Zentrum Astronomie, Universität Heidelberg, Inst. Theor. Astrophysik,
Albert-Ueberle Str.
2, 69120
Heidelberg,
Germany
5
OASU/LAB-UMR5804, CNRS, Université Bordeaux 1,
33270
Floirac,
France
6
National Research Council of Canada, Herzberg Institute of
Astrophysics, Victoria
BC, Canada
7
Laboratoire d’Astrophysique de Marseille, CNRS/INSU − Université
de Provence, 13388
Marseille Cedex 13,
France
8
Université de Toulouse, UPS, CESR, 9 Av. du colonel Roche,
31028
Toulouse,
France
9
IAPS-INAF, Fosso del Cavaliere 100, 00133
Roma,
Italy
10
Cardiff University School of Physics and Astronomy,
Cardiff,
UK
11
CITA & Dep. of Astronomy and Astrophysics, University of
Toronto, Toronto,
CA,
Canada
12
Department of Physics and Astronomy, University of
Victoria, PO Box 355, STN
CSC, Victoria BC,
Canada
13
Institut d’Astrophysique de Paris, UPMC, UMR 7095,
CNRS, 98 Bd Arago,
75014
Paris,
France
14
ESO, Karl Schwarzschild Str. 2, 85748
Garching,
Germany
15
Department of Physics & Astronomy, The Open
University, Milton
Keynes
MK7 6AA,
UK
16
The Rutherford Appleton Laboratory, Chilton, Didcot, OX11
0NL, UK
Key words: ISM: clouds / ISM: structure / evolution / HII regions / errata, addenda
The paper by Schneider et al. (2012) contains an error in Sect. 2.2 and in Fig. 6. The bottom y-axis label of Fig. 6 must read “PDF(η)” instead of “log 10PDF(η)”. The corrected version of the figure is shown in Fig. 1 here. In Sect. 2.2 of Schneider et al. (2012), the slope fitted to the high-density tail of the composite PDF, Fig. 6 (here Fig. 1), in Rosette was wrongly quoted to correspond to a radial volumetric density profile n ∝ r-0.65. The value of the slope −0.65 actually corresponds to the radial column density profile, N ∝ r-0.65. Since n ∝ N/r, this translates into the equivalent volumetric density profile, n ∝ r-1.65 (see the derivation of the relation between PDF slopes and (column) density profiles in Federrath & Klessen 2013). Hence the statement in Sect. 2.2 is incorrect, i.e., that the “exponent is smaller than what is typically found for dense cores (−1.5 to −2), suggesting that on large (cloud)-scales, turbulence is the dominating process compared to gravity”. The corrected value n ∝ r-1.65 is much closer to what is found in related studies (e.g., Arzoumanian et al. 2011) and suggests that gravitational collapse – at least locally – does play an important role in Rosette and likely is the reason for the high-density power-law tail in Fig. 1.
 |
Fig. 1 Corrected version of Fig. 6 in Schneider et al. (2012). |
References
- Arzoumanian, D., André, P., Didelon, P., et al. 2011, A&A, 529, L6 [Google Scholar]
- Federrath, C., & Klessen, R. S. 2013, ApJ, 763, 51 [NASA ADS] [CrossRef] [Google Scholar]
- Schneider, N., Csengeri, T., Hennemann, M., et al. 2012, A&A, 540, L11 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© ESO, 2013
All Figures
|
Fig. 1 Corrected version of Fig. 6 in Schneider et al. (2012). |
| In the text | |
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.