Volume 632, December 2019
|Number of page(s)||1|
|Published online||17 December 2019|
A cosmic collider: Was the IceCube neutrino generated in a precessing jet-jet interaction in TXS 0506+056? (Corrigendum)
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2 Max-Planck-Institut für Astronomie, Königstuhl, Heidelberg, Germany
3 Centre for Space Research, North-West University, Potchefstroom 2531, South Africa
4 I. Physikalisches Institut, Universität Köln, Zülpicher Str. 77, Köln, Germany
5 Center for Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02-668 Warsaw, Poland
6 Institute of Geodesy and Geoinformation, University of Bonn, Nußallee 17, 53115 Bonn, Germany
7 Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia
8 Astronomical Institute, Academy of Sciences, Boční II 1401, 14131 Prague, Czech Republic
9 ELI Beamlines, Institute of Physics, Czech Academy of Sciences, 25241 Dolní Břežany, Czech Republic
10 Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia
Key words: black hole physics / techniques: interferometric / BL Lacertae objects: individual: TXS 0506+056 / errata / addenda
Maria Petropoulou and Bing Theodore Zhang brought to our attention that in the original paper (Britzen et al. 2019), the right-hand side of Eq. (14) had not been divided numerically by c = 3 × 1010 cm s−1. This arithmetical error was carried through to the subsequent equations as well. Furthermore, the scaling factor, , from Eq. (13) was not carried through. Equation (14),
thus numerically evaluates to:
Interestingly, this further increases the number of relativistic protons needed to produce the IceCube neutrinos from TXS 0506+056 during the 2014−2015 neutrino flare to
The corresponding total kinetic power in relativistic protons, under the assumptions spelled out in the original manuscript, consequently increases to
which, for the standard parameter values adopted above, is far above the Eddington luminosity of the central supermassive black hole in TXS 0506+056. However, as the measured apparent speed of jet I appears to be significantly smaller than for jet II, an assumption of δI, 1 ≪ 1 and Γrel, 1 ≫ 1, and also possibly δII, 1 ≫ 1, may be realistic. In this case, more moderate jet power requirements result.
Based on this correction, we wish to reformulate our conclusion concerning the relation between the observed cosmic collision and the neutrino emission from TXS 0506+056 for the observed neutrino flare in 2014−2015 as follows. The quantitative analysis of the potential neutrino production in the jet of TXS 0506+056 suggests that the observed cosmic collision and interaction of jet components in the jet of this blazar may be related to the observed neutrino flare in 2014−2015. This would require a large velocity difference between the interacting jet components, assuming that the jet power is bounded by the Eddington limit of the central supermassive black hole in TXS 0506+056. Table 1 from our original paper, which remains unchanged, demonstrates that we find evidence for significantly different apparent jet speeds.
All of the results of the VLBA data analysis (kinematics, beaming, and the precession model), as presented in the original paper, are unaffected by this Corrigendum.
© S. Britzen et al. 2019
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Open Access funding provided by Max Planck Society.
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