| Issue |
A&A
Volume 674, June 2023
|
|
|---|---|---|
| Article Number | C2 | |
| Number of page(s) | 1 | |
| Section | Galactic structure, stellar clusters and populations | |
| DOI | https://doi.org/10.1051/0004-6361/202244199e | |
| Published online | 26 June 2023 | |
A detection of the layered structure of nearby open clusters (Corrigendum)
1
Xinjiang Astronomical Observatory, Chinese Academy of Sciences, No. 150, Science 1 Street, Urumqi, Xinjiang 830011, PR China
e-mail: zhy@xao.ac.cn
2
University of Chinese Academy of Sciences, 19 Yuquan Road, Shijingshan District, Beijing 100049, PR China
Key words: methods: statistical / open clusters and associations: general / galaxies: stellar content / errata, addenda
1. Correction
The following sentences in the first paragraph on page 3, “by Bailer-Jones (2015) and solved the inversion problem within a Bayesian framework. Our approach closely followed the distance correction procedure described in Carrera et al. (2019); see their appendix.” should read “by Bailer-Jones (2015) and later adopted by Pang et al. (2021). The distance correction procedure we closely followed is from Carrera et al. (2019, see their appendix). The distance correction problem is solved within a Bayesian framework.”
The sentences in the second paragraph on page 3, “The prior is composed of two components, one representing the star cluster density, and the other considering the field. The former follows a normal distribution and the latter an exponentially decreasing density as in Bailer-Jones (2015). We combined these two components with weights proportional to the membership probability.” should read “Each star’s prior function includes two components, the members’ density of clusters, which shows a normal distribution and the distribution of field stars, which is an exponentially decreasing distribution of density (Bailer-Jones 2015). These two components are combined by the membership probability as a weighting factor.”. The text “......, which is used for the cluster term, and 1–α for the field star term. ...... . The likelihood function can be calculated from the observed parallax and its nominal error. The mean of the posterior was considered as the corrected distance of each star. More details about this parallax inversion method can be found in Carrera et al. (2019).” should read “......, which denotes the cluster member term. And 1–α is used to represent the field star. ...... . We calculated the likelihood function with the observed parallax and its error. The posterior mean is the corrected distance of each member. The detailed distance correction procedure is described in Carrera et al. (2019) and Pang et al. (2021).”.
2. Apology statement
The revised sentences had been copied from Pang et al. (2021). All authors of this paper apologize for this mistake.
References
- Bailer-Jones, C. A. L. 2015, PASP, 127, 994, DOI: 10.1086/683116 [NASA ADS] [CrossRef] [Google Scholar]
- Carrera, R., Pasquato, M., Vallenari, A., et al. 2019, A&A, 627, A119, DOI: 10.1051/0004-6361/201935599 [CrossRef] [EDP Sciences] [Google Scholar]
- Pang, X., Li, Y., Yu, Z., et al. 2021, ApJ, 912, 162, DOI: 10.3847/1538-4357/abeaac [NASA ADS] [CrossRef] [Google Scholar]
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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