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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

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 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 as an indication for event sizes that would be under typical noise levels”.

thumbnail Fig. 1.

Sizes of all the irregularities selected for all possible combinations of signs for Δν and , including cases in which one of the parameters was not detected (Δν = 0 or , which are plotted as a letter x and crosses, respectively). These results are for Nd = 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

thumbnail Fig. 1.

Sizes of all the irregularities selected for all possible combinations of signs for Δν and , including cases in which one of the parameters was not detected (Δν = 0 or , which are plotted as a letter x and crosses, respectively). These results are for Nd = 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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