On the radiation driven alignment of dust grains: Detection of the polarization hole in a starless core (Corrigendum)

F. O. Alves; P. Frau; J. M. Girart; G. A. P. Franco; F. P. Santos; H. Wiesemeyer

doi:10.1051/0004-6361/201424678e

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Volume 574 (February 2015)

A&A, 574 (2015) C4

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201424678]

Issue		A&A Volume 574, February 2015


Article Number		C4
Number of page(s)		1
Section		Letters
DOI		https://doi.org/10.1051/0004-6361/201424678e
Published online		03 February 2015

A&A 574, C4 (2015)

On the radiation driven alignment of dust grains: Detection of the polarization hole in a starless core (Corrigendum)

F. O. Alves¹, P. Frau²^,3, J. M. Girart⁴, G. A. P. Franco⁵, F. P. Santos⁶ and H. Wiesemeyer⁷

¹ Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany
e-mail: falves@mpe.mpg.de
² Instituto de Ciencia de Materiales de Madrid (CSIC), Sor Juana Inés de la Cruz 3, 28049 Madrid, Spain
³ Observatorio Astronómico Nacional, Alfonso XII 3, 28014 Madrid, Spain
⁴ Institut de Ciències de l’Espai (CSIC-IEEC), Campus UAB, Facultat de Ciències, C5 par 2 a, 08193 Bellaterra, Catalunya, Spain
⁵ Departamento de Física – ICEx – UFMG, Caixa Postal 702, 30. 123-970 Belo Horizonte, Brazil
⁶ Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA
⁷ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

Key words: stars: formation / ISM: magnetic fields / techniques: polarimetric / ISM: individual objects: Core 109 / errata, addenda

Erratum for: A&A 569, L1 (2014), DOI: 10.1051/0004-6361/201424678

Figure 2 in the original manuscript displays the polarization efficiency for the optical, near infrared and sub-millimeter (submm) polarimetric data as P/A_V, where P is the polarization degree and A_V is the visual extinction traced by the data. However, the polarization efficiency for the submm data should be simply P. By dividing P by A_V, we obtain a steeper and wrong slope for the decrease in polarization efficiency. The suitable form for Fig. 2 of the original document is exhibited in Fig. 1 of the present corrigendum. The submm polarization efficiency decreases as ~−1.0 with respect to A_V, instead of the originally published ~−2.0.

Although the decrease in polarization efficiency at the submm regime is shallower than originally proposed, our modelling of the polarization degree with respect to the relative intensity, I/I_max, still predicts the detection of a polarization hole (Sect. 3 of the published manuscript). Therefore, the main conclusions are unchanged.

Fig. 1

Polarization efficiency of the optical and near-IR data (P/A_V) and the submm data (P_SM).

© ESO, 2015

All Figures

	Fig. 1 Polarization efficiency of the optical and near-IR data (P/A_V) and the submm data (P_SM).
In the text

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