Small glitches and other rotational irregularities of the Vela pulsar (Corrigendum)

C. M. Espinoza; D. Antonopoulou; R. Dodson; M. Stepanova; A. Scherer

doi:10.1051/0004-6361/202039044e

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/202039044]

Issue		A&A Volume 649, May 2021


Article Number		C2
Number of page(s)		2
Section		Stellar structure and evolution
DOI		https://doi.org/10.1051/0004-6361/202039044e
Published online		04 May 2021

A&A 649, C2 (2021)

Small glitches and other rotational irregularities of the Vela pulsar (Corrigendum)

C. M. Espinoza¹, D. Antonopoulou²^,3, R. Dodson⁴, M. Stepanova¹ and A. Scherer⁵

¹ Departamento de Física, Universidad de Santiago de Chile (USACH), Estación Central, Santiago 9170124, Chile
e-mail: cristobal.espinoza.r@usach.cl
² Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
³ Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK
⁴ International Centre for Radio Astronomy Research, University of Western Australia, Crawley, WA 6009, Australia
⁵ Instituto de Astrofísica, Pontificia Universidad Católica de Chile, 782-0436 Macul, Santiago, Chile

Key words: stars: neutron / pulsars: general / pulsars: individual: PSR B0833–45 / stars: rotation / errata, addenda

Erratum for: A&A 647, A25 (2021), https://doi.org/10.1051/0004-6361/202039044

There was an error with the plotted lines that indicate detection capabilities in quadrants I and III of Fig. 9 (for events with Δν and $Δ \dot{ν}$ $\Delta\dot{\nu}$ of equal signs). The correct figure and updated caption is below.

Section 6: To accommodate the correction to Fig. 9, the last sentence of the second paragraph must read “For the other events (quadrants I and III) we used the condition $ϕ_{g} (t = 10 d) > σ_{ϕ}^{\max}$ $\phi_{\rm g}(t=10\,{\rm d})>\sigma_\phi^{\rm max}$ as an indication for event sizes that would be under typical noise levels”.

Fig. 1.

Sizes of all the irregularities selected for all possible combinations of signs for Δν and $Δ \dot{ν}$ $\Delta\dot{\nu}$ , including cases in which one of the parameters was not detected (Δν = 0 or $Δ \dot{ν} = 0$ $\Delta\dot{\nu}=0$ , which are plotted as a letter x and crosses, respectively). These results are for N_d = 10 d, and the known Vela glitches in the dataset were measured as for Fig. 2. The straight lines represent detection limits (events in the shaded areas are unlikely to be detected) when considering average noise levels. The curved dotted lines give an indication of the event sizes below which deviations to the timing model will remain under typical noise levels for 10 d since the event epoch (see Sect. 6).

© ESO 2021

All Figures

Fig. 1.

Sizes of all the irregularities selected for all possible combinations of signs for Δν and $Δ \dot{ν}$ $\Delta\dot{\nu}$ , including cases in which one of the parameters was not detected (Δν = 0 or $Δ \dot{ν} = 0$ $\Delta\dot{\nu}=0$ , which are plotted as a letter x and crosses, respectively). These results are for N_d = 10 d, and the known Vela glitches in the dataset were measured as for Fig. 2. The straight lines represent detection limits (events in the shaded areas are unlikely to be detected) when considering average noise levels. The curved dotted lines give an indication of the event sizes below which deviations to the timing model will remain under typical noise levels for 10 d since the event epoch (see Sect. 6).

In the text

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