| Issue |
A&A
Volume 666, October 2022
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Galactic structure, stellar clusters and populations | |
| DOI | https://doi.org/10.1051/0004-6361/202140816e | |
| Published online | 29 September 2022 | |
TOPoS
VI. The metal-weak tail of the metallicity distribution functions of the Milky Way and the Gaia-Sausage-Enceladus structure⋆ (Corrigendum)
1
GEPI, Observatoire de Paris, Université PSL, CNRS, Place Jules Janssen, 92195 Meudon, France
e-mail: Piercarlo.Bonifacio@obspm.fr
2
Departamento de Ciencias Fisicas, Universidad Andres Bello, Fernandez Concha 700, Las Condes, Santiago, Chile
3
Dipartimento di Fisica e Astronomia, Universitá degli Studi di Firenze, Via G. Sansone 1, 50019 Sesto Fiorentino, Italy
4
INAF/Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
5
European Southern Observatory, Casilla, 19001 Santiago, Chile
6
Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
7
UPJV, Université de Picardie Jules Verne, 33 rue St Leu, 80080 Amiens, France
8
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12, 69120 Heidelberg, Germany
9
INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova I-35122, Italy
Key words: stars: Population II / stars: abundances / Galaxy: abundances / Galaxy: halo / errata, addenda
Spectroscopic and photometric metallicities derived and discussed in this paper as well as orbital actions computed and discussed this paper are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/C1
We realised that there was a mistake in the code that computed parameters for the photometric data sample. The effective temperature was not computed according to the formula in footnote 3. As a consequence the surface gravity and metallicity were also computed incorrectly. We also realised that almost 50% of the lines in the table were duplicated. Furthermore, for 301 763 stars, the interpolation arrived at the edge in metallicity of the synthetic grid (+0.5) and the program was not extrapolating. We removed these stars from the final catalogue. A new catalogue, containing 12 894 443 unique stars, has been produced correcting these two mistakes and deposited at CDS. In the paper this impacts only Fig. 8, which is corrected in this corrigendum, and the number of stars in this catalogue cited in Sect. 5.2; it should read: “The final sample, which we refer to in the following as ‘photometric’, consists of 12 894 443 unique stars”. None of the conclusions of the paper are altered by this change.
 |
Fig. 8. Distribution of photometric metallicities for the photometric and spectroscopic samples. Each sample has been normalised so that the area under the histogram is equal to one. |
© P. Bonifacio et al. 2022
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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All Figures
|
Fig. 8. Distribution of photometric metallicities for the photometric and spectroscopic samples. Each sample has been normalised so that the area under the histogram is equal to one. |
| In the text | |
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