Cluster-formation in the Rosette molecular cloud at the junctions of filaments (Corrigendum)

N. Schneider; T. Csengeri; M. Hennemann; F. Motte; P. Didelon; C. Federrath; S. Bontemps; J. Di Francesco; D. Arzoumanian; V. Minier; Ph. André; T. Hill; A. Zavagno; Q. Nguyen-Luong; M. Attard; J.-Ph. Bernard; D. Elia; C. Fallscheer; M. Griffin; J. Kirk; R. Klessen; V. Könyves; P. Martin; A. Men’shchikov; P. Palmeirim; N. Peretto; M. Pestalozzi; D. Russeil; S. Sadavoy; T. Sousbie; L. Testi; P. Tremblin; D. Ward-Thompson; G. White

doi:10.1051/0004-6361/201118566e

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Erratum

This article is an erratum for: [this article]

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

A&A 551, C1 (2013)

Cluster-formation in the Rosette molecular cloud at the junctions of filaments (Corrigendum)

N. Schneider¹^,5, T. Csengeri², M. Hennemann¹, F. Motte¹, P. Didelon¹, C. Federrath³^,4, S. Bontemps⁵, J. Di Francesco⁶, D. Arzoumanian¹, V. Minier¹, Ph. André¹, T. Hill¹, A. Zavagno⁷, Q. Nguyen-Luong¹, M. Attard¹, J.-Ph. Bernard⁸, D. Elia⁹, C. Fallscheer⁶, M. Griffin¹⁰, J. Kirk¹⁰, R. Klessen⁴, V. Könyves¹, P. Martin¹¹, A. Men’shchikov¹, P. Palmeirim¹, N. Peretto¹, M. Pestalozzi⁹, D. Russeil⁷, S. Sadavoy¹², T. Sousbie¹³, L. Testi¹⁴, P. Tremblin¹, D. Ward-Thompson¹⁰ and G. White¹⁵^,16

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

Erratum to: A&A 540, L11 (2012), DOI: 10.1051/0004-6361/201118566

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).
Open with DEXTER

References

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

All Figures

	Fig. 1 Corrected version of Fig. 6 in Schneider et al. (2012).
Open with DEXTER
In the text

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