Statistical simulations of the dust foreground to cosmic microwave background polarization (Corrigendum)

F. Vansyngel; F. Boulanger; T. Ghosh; B. Wandelt; J. Aumont; A. Bracco; F. Levrier; P. G. Martin; L. Montier

doi:10.1051/0004-6361/201629992e

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Volume 618 (October 2018)

A&A, 618 (2018) C4

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201629992]

Issue		A&A Volume 618, October 2018


Article Number		C4
Number of page(s)		1
Section		Cosmology (including clusters of galaxies)
DOI		https://doi.org/10.1051/0004-6361/201629992e
Published online		11 October 2018

A&A 618, C4 (2018)

Corrigendum

Statistical simulations of the dust foreground to cosmic microwave background polarization (Corrigendum)

F. Vansyngel¹, F. Boulanger¹, T. Ghosh¹^,2, B. Wandelt³^,4, J. Aumont¹, A. Bracco¹^,5, F. Levrier⁶, P. G. Martin⁷ and L. Montier⁸

¹ Institut d'Astrophysique Spatiale, CNRS, Université Paris-Sud, Université Paris-Saclay, Bât. 121, 91405 Orsay Cedex, France
² California Institute of Technology, Pasadena, CA 91125, USA
³ Sorbonne Universités, UPMC Université Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, France
⁴ Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, 75014 Paris, France
⁵ Laboratoire AIM, IRFU/Service d'Astrophysique, CEA/DSM, CNRS, Université Paris Diderot, Bât. 709, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France
⁶ LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Université Paris 06, Ecole normale supérieure, 75005, Paris, France
⁷ CITA, University of Toronto, 60 St. George St., Toronto, ON M5S 3H8, Canada
⁸ CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France

Key words: polarization / ISM: general / comic background radiation / submillimeter: ISM / errata, addenda

Erratum for: A&A, 603, A62 (2017), https://doi.org/10.1051/0004-6361/201629992

The caption of Fig. 8 had a confusing description of the material shown in the plots. The correct caption together with the figure is given below.

© ESO 2018

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	Fig. 8 High-resolution power spectra on the LR63 region; simulation vs. data. From top to bottom: TE, EE; and BB power spectra of the Planck 353 GHz, CMB-corrected maps (red crosses), and one high-resolution (N_side = 2048, FWHM = 10') realization of the model (blue squares).
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