| Issue |
A&A
Volume 685, May 2024
|
|
|---|---|---|
| Article Number | C3 | |
| Number of page(s) | 1 | |
| Section | Letters to the Editor | |
| DOI | https://doi.org/10.1051/0004-6361/202450416e | |
| Published online | 14 May 2024 | |
Letter to the Editor
The orbital parameters of the δ Cep inner binary system determined using 2019 HARPS-N spectroscopic data (Corrigendum)
1
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France
e-mail: nicolas.nardetto@oca.eu
2
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warszawa, Poland
3
LESIA (UMR 8109), Observatoire de Paris, PSL, CNRS, UPMC, Univ. Paris-Diderot, 5 place Jules Janssen, Meudon, France
4
Instituto de Astrofísica, Departamento de Ciencias Físicas, Facultad de Ciencias Exactas, Universidad Andrés Bello, Fernández Concha 700, Las Condes, Santiago, Chile
5
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile
6
Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
7
European Southern Observatory, Alonso de Córdova 3107, Casilla, 19001 Santiago 19, Chile
8
INAF – Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate (LC), Italy
9
Leibniz Institute for Astrophysics, An der Sternwarte 16, 14482 Potsdam, Germany
Key words: binaries: close / binaries: spectroscopic / stars: oscillations / stars: individual: δ Cep / stars: variables: Cepheids / errata / addenda
Figure 2 was accidentally replaced with Figure 1 during the production process of the published version. The corrected 3 panels are shown here.
 |
Fig. 2. Same as Fig. 1 but after correction for the orbital velocity of the Cepheid component as described by the parameters listed in Table 2. The residuals in the middle and right panels are plotted as a function of the pulsation phase and BJD, respectively. The derived pulsation velocity curves shown in the left panel, including that from this work (blue open diamonds), have a dispersion much lower than in the left panel of Fig. 1. The rms residuals in the middle and right panels are about 0.4 km s−1. The RVcc-g curve corrected for the binarity and corresponding to this work is also shown in Fig. 5. |
© The Authors 2024
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. 2. Same as Fig. 1 but after correction for the orbital velocity of the Cepheid component as described by the parameters listed in Table 2. The residuals in the middle and right panels are plotted as a function of the pulsation phase and BJD, respectively. The derived pulsation velocity curves shown in the left panel, including that from this work (blue open diamonds), have a dispersion much lower than in the left panel of Fig. 1. The rms residuals in the middle and right panels are about 0.4 km s−1. The RVcc-g curve corrected for the binarity and corresponding to this work is also shown in Fig. 5. |
| In the text | |
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