Volume 551, March 2013
|Number of page(s)||1|
|Published online||11 February 2013|
Cluster-formation in the Rosette molecular cloud at the junctions of filaments (Corrigendum)
IRFU/SAp CEA/DSM, Laboratoire AIM CNRS – Université Paris
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.
- Arzoumanian, D., André, P., Didelon, P., et al. 2011, A&A, 529, L6 [NASA ADS] [CrossRef] [EDP Sciences] [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
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