Issue |
A&A
Volume 635, March 2020
|
|
---|---|---|
Article Number | C2 | |
Number of page(s) | 1 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/201834461e | |
Published online | 03 March 2020 |
Stellar ages, masses, and radii from asteroseismic modeling are robust to systematic errors in spectroscopy (Corrigendum)
1
Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark
e-mail: bellinger@phys.au.dk
2
Stellar Ages & Galactic Evolution (SAGE) Group, Max Planck Institute for Solar System Research, Göttingen, Germany
3
Max Planck Institute for Astrophysics, Garching, Germany
4
Department of Astronomy, Yale University, New Haven, CT, USA
Key words: asteroseismology / stars: abundances / stars: low-mass / stars: evolution / stars: oscillations / errata, addenda
The original article presented the density scaling relation (Eq. (2)) incorrectly. The correct relation is:
This error affects the rightmost panel of Fig. 10, the bottom left panel of Fig. 13, and the bottom left panel of Fig. 14. The corrected panels are presented in Figs. 1 and 2.
![]() |
Fig. 1.
Corrected rightmost panel of Fig. 10. The biases in the residuals are consistent with zero (−0.004 ± 0.017 ρ ⊙). |
![]() |
Fig. 2.
Corrected bottom left panels of Figs. 13 and 14. The dashed lines corresponding to the scaling relations have been removed. |
The sentence “We note that the large number of outliers in mean density estimates in Fig. 10 arise mainly from their very small uncertainties”. is no longer relevant, as the majority of these are no longer outliers with the correct relation.
© ESO 2020
All Figures
![]() |
Fig. 1.
Corrected rightmost panel of Fig. 10. The biases in the residuals are consistent with zero (−0.004 ± 0.017 ρ ⊙). |
In the text |
![]() |
Fig. 2.
Corrected bottom left panels of Figs. 13 and 14. The dashed lines corresponding to the scaling relations have been removed. |
In the text |
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