Polarization angle swings in blazars: The case of 3C 279 (Corrigendum)

S. Kiehlmann; T. Savolainen; S. G. Jorstad; K. V. Sokolovsky; F. K. Schinzel; A. P. Marscher; V. M. Larionov; I. Agudo; H. Akitaya; E. Benítez; A. Berdyugin; D. A. Blinov; N. G. Bochkarev; G. A. Borman; A. N. Burenkov; C. Casadio; V. T. Doroshenko; N. V. Efimova; Y. Fukazawa; J. L. Gómez; T. S. Grishina; V. A. Hagen-Thorn; J. Heidt; D. Hiriart; R. Itoh; M. Joshi; K. S. Kawabata; G. N. Kimeridze; E. N. Kopatskaya; I. V. Korobtsev; T. Krajci; O. M. Kurtanidze; S. O. Kurtanidze; E. G. Larionova; L. V. Larionova; E. Lindfors; J. M. López; I. M. McHardy; S. N. Molina; Y. Moritani; D. A. Morozova; S. V. Nazarov; M. G. Nikolashvili; K. Nilsson; N. G. Pulatova; R. Reinthal; A. Sadun; M. Sasada; S. S. Savchenko; S. G. Sergeev; L. A. Sigua; P. S. Smith; M. Sorcia; O. I. Spiridonova; K. Takaki; L. O. Takalo; B. Taylor; I. S. Troitsky; M. Uemura; L. S. Ugolkova; T. Ui; M. Yoshida; J. A. Zensus; V. E. Zhdanova

doi:10.1051/0004-6361/201527725e

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Erratum

This article is an erratum for: [this article]

Issue		A&A Volume 592, August 2016


Article Number		C1
Number of page(s)		2
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/201527725e
Published online		28 July 2016

A&A 592, C1 (2016)

Polarization angle swings in blazars: The case of 3C 279 (Corrigendum)

S. Kiehlmann¹^,2^,3, T. Savolainen¹^,2^,3, S. G. Jorstad⁴^,5, K. V. Sokolovsky⁶^,7^,8, F. K. Schinzel⁹, A. P. Marscher⁴, V. M. Larionov⁵^,10, I. Agudo¹¹, H. Akitaya¹², E. Benítez¹³, A. Berdyugin¹⁴, D. A. Blinov¹⁵^,16^,5, N. G. Bochkarev⁷, G. A. Borman¹⁷, A. N. Burenkov¹⁸, C. Casadio¹¹, V. T. Doroshenko¹⁹, N. V. Efimova¹⁰, Y. Fukazawa²⁰, J. L. Gómez¹¹, T. S. Grishina⁵, V. A. Hagen-Thorn⁵, J. Heidt²¹, D. Hiriart²², R. Itoh²⁰, M. Joshi⁴, K. S. Kawabata¹², G. N. Kimeridze²³, E. N. Kopatskaya⁵, I. V. Korobtsev²⁴, T. Krajci²⁵, O. M. Kurtanidze²³^,21^{, 26}, S. O. Kurtanidze²³, E. G. Larionova⁵, L. V. Larionova⁵, E. Lindfors¹⁴, J. M. López²², I. M. McHardy²⁷, S. N. Molina⁹, Y. Moritani²⁸, D. A. Morozova⁵, S. V. Nazarov¹⁸, M. G. Nikolashvili²³, K. Nilsson²⁹, N. G. Pulatova¹⁷, R. Reinthal¹⁴, A. Sadun³⁰, M. Sasada⁴, S. S. Savchenko⁵, S. G. Sergeev¹⁷, L. A. Sigua²³, P. S. Smith³¹, M. Sorcia¹³, O. I. Spiridonova¹⁸, K. Takaki²⁰, L. O. Takalo¹⁴, B. Taylor⁴^,32, I. S. Troitsky⁵, M. Uemura¹², L. S. Ugolkova⁷, T. Ui²⁰, M. Yoshida¹², J. A. Zensus³ and V. E. Zhdanova¹⁸

¹ Aalto University Metsähovi Radio Observatory, Metsähovintie 114, 02540 Kylmälä, Finland
e-mail: sebastian.kiehlmann@aalto.fi
² Aalto University Department of Radio Science and Engineering, PL 13000, 00076 Aalto, Finland
³ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
⁴ Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA
⁵ Astronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, Russia
⁶ Astro Space Center of Lebedev Physical Institute, Profsoyuznaya 84/32, 117997 Moscow, Russia
⁷ Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Universiteskij prosp. 13, Moscow 119991, Russia
⁸ Institute of Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, Vas. Pavlou & I. Metaxa, 15 236 Penteli, Greece
⁹ Department of Physics and Astronomy, University of New Mexico, Albuquerque NM, 87131, USA
¹⁰ Main (Pulkovo) Astronomical Observatory of RAS, Pulkovskoye shosse, 60, 196140 St. Petersburg, Russia
¹¹ Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain
¹² Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, 739-8526 Hiroshima, Japan
¹³ Instituto de Astronomía, Universidad Nacional Autónoma de México, 04510 México DF, Mexico
¹⁴ Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
¹⁵ Foundation for Research and Technology – Hellas, IESL, Voutes, 71110 Heraklion, Greece
¹⁶ Department of Physics and Institute for Plasma Physics, University of Crete, 71003 Heraklion, Greece
¹⁷ Crimean Astrophysical Observatory, 98409 P/O Nauchny, Crimea
¹⁸ Special Astrophysical Observatory of the Russian AS, Nizhnij Arkhyz, 369167 Karachaevo-Cherkesia, Russia
¹⁹ Southern Station of the Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, P/O Nauchny 298409, Crimea
²⁰ Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan
²¹ ZAH, Landessternwarte Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany
²² Instituto de Astronomía, Universidad Nacional Autónoma de México, 22860 Ensenada BC, Mexico
²³ Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia
²⁴ Inst. of Solar-Terrestrial Physics, Lermontov st. 126a, p/o box 291, 664033 Irkutsk, Russia
²⁵ Center for Backyard Astrophysics – New Mexico, PO Box 1351, Cloudcroft, NM 88317, USA
²⁶ Engelhardt Astronomical Observatory, Kazan Federal University, Tatarstan, Russia
²⁷ Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK
²⁸ Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), The University of Tokyo, 5-1-5 Kashiwa-no-Ha, 277-8583 Kashiwa City Chiba, Japan
²⁹ Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
³⁰ Department of Physics, University of Colorado Denver, CO, USA
³¹ Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
³² Lowell Observatory, Flagstaff, AZ 86001, USA

Key words: polarization / galaxies: active / galaxies: jets / quasars: individual: 3C 279 / errata, addenda

Erratum to: A&A 590, A10 (2016), DOI: 10.1051/0004-6361/201527725

We mistakenly used a preliminary version of Fig. 8, based on just 20 000 simulations instead of 1 000 000 simulations as intended and stated in the manuscript. Here, we show the correct figure based on 1 000 000 simulations. Accordingly, the number of simulations, which fulfil the conditions on the mean and standard deviation of the polarization fraction, N, which is given in the legend of the figure for each model, is approximately 50 times higher than shown in the wrong figure. In comparison with Fig. 10, these numbers indicate that it is more likely that the three tested random walk processes produce the mean and standard deviation of the polarization fraction as observed during period IIa than observed during period IIIc. None of the results and conclusions presented in the original manuscript were affected by the inclusion of the wrong figure.

	Fig. 8 Distribution of the EVPA rotation amplitude (upper panel) and distribution of the EVPA variation estimator (lower panel) for all simulations with a mean polarization fraction consistent with the observed value during period IIa. The number of selected simulations is indicated in the legend. The corresponding observed values are indicated by black dotted lines.
Open with DEXTER

© ESO, 2016

All Figures

	Fig. 8 Distribution of the EVPA rotation amplitude (upper panel) and distribution of the EVPA variation estimator (lower panel) for all simulations with a mean polarization fraction consistent with the observed value during period IIa. The number of selected simulations is indicated in the legend. The corresponding observed values are indicated by black dotted lines.
Open with DEXTER
In the text

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