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# Erratum: The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas

Illya Plotnikov, Lorenzo Sironi

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Illya Plotnikov, Lorenzo Sironi. Erratum: The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas. Monthly Notices of the Royal Astronomical Society, 2019, 490 (1), pp.156-156. 10.1093/mnras/stz2653. hal-04982444

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# Erratum: The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas

by Illya Plotnikov<sup>1,2*</sup> and Lorenzo Sironi<sup>3</sup>

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**Key words:** errata, addenda – magnetic fields – masers – radiation mechanisms: non-thermal – shock waves – stars: neutron.

The authors regret to report that the last part of Appendix B of the recent paper 'The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas' (Plotnikov & Sironi 2019) contains an error that we correct here. This error does not affect any of the results reported in the main body of the paper or in Appendix A.

The electromagnetic field components $B_x$, $B_y$, $E_x$, and $E_z$ were not normalized correctly in 2D and 3D post-simulation diagnostics, leading to under-estimation of the O-mode contribution in 2D and 3D simulations. We emphasize that field components relevant for X-mode emission $B_x$ and $E_y$ were normalized correctly in all cases.

Let us list the two corrections to the estimates in the last three paragraphs of Appendix B:

(i) In the results of 3D simulations, the ratio of O-mode to X-mode contributions is $\langle\delta B_y^2\rangle / \langle\delta B_z^2\rangle \sim 0.2 - 0.5$, instead of $10^{-3}$, as originally reported. This can affect the linear polarization of the precursor waves more significantly than originally expected

but does not impact significantly the wave total energy and so, the efficiency of the maser emission (so, Fig. B1 and B2 are basically unchanged; more precisely, the figures correctly capture the comparison of X-mode efficiency as a function of dimensionality, basically neglecting the O-mode).

(ii) Still in 3D simulations, the ratio of Poynting flux in the transverse y-direction to Poynting flux is the longitudinal x-direction is also increased by about two orders of magnitude, $|\Pi_y|/|\Pi_x| \sim 5 \times 10^{-2}$, instead of $5 \times 10^{-4}$ as given initially. The emitted precursor wave is still strongly beamed along the shock-normal direction.

All the results discussed in the main text of the original article (pertaining to 1D simulations) are not affected by this error.

## REFERENCE

Plotnikov I., Sironi L., 2019, MNRAS, 485, 3816

This paper has been typeset from a TeX/LATeX file prepared by the author.

<footnote n="1"><sup>1</sup>Department of Astrophysical Sciences, Princeton University, 4 Ivy Ln., Princeton, NJ 08544, USA</footnote>

<footnote n="2"><sup>2</sup>Université de Toulouse, UPS-OMP, IRAP, 9 av. Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France</footnote>

<footnote n="3"><sup>3</sup>Department of Astronomy, Columbia University, 550 W 120th St., New York, NY 10027, USA</footnote>

<footnote>* E-mail: illyap@astro.princeton.edu</footnote>