| Issue |
A&A
Volume 622, February 2019
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Catalogs and data | |
| DOI | https://doi.org/10.1051/0004-6361/201833500e | |
| Published online | 15 February 2019 | |
Exploring the stellar properties of M dwarfs with high-resolution spectroscopy from the optical to the near-infrared (Corrigendum)
1
Astronomy & Astrophysics Division, Physical Research Laboratory, Ahmedabad 380009, India
e-mail: arvindr@prl.res.in
2
Univ. Lyon, ENS de Lyon, Univ. Lyon1, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69007 Lyon, France
3
Institut für Theoretische Physik, Universität Göttingen, 37077 Göttingen, Germany
4
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
5
Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua Campo Alegre, 4169-007 Porto, Portugal
6
Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
7
Dipartimento di Fisica e Astronomia, Via Gobetti 93/2, 40131 Bologna, Italy
Key words: stars: fundamental parameters / stars: low-mass / stars: atmospheres / errata, addenda
References to the figures in the text are not correct. The corrected figure references along with the respective texts of the original paper are as follows:
– Caption of Fig. 5: References to right and left panels are inverted. The corrected figure caption is:
Left panel: comparison of Teff versus spectral type relation as a function of metallicity from this study with Passegger et al. (2018; open triangle) and with Rajpurohit et al. (2013; open circle). Right panel: comparison of Teff determined from this study with Passegger et al. (2018; open triangle) and with Gaidos & Mann (2014; filled square) as function of metallicity.
– Corrected text (page 5, right column): In order to explore the effect of stellar properties of M dwarfs, we have compared our results with the behavior of Teff, as a function of spectral type with Rajpurohit et al. (2013) as shown in Fig. 5 (left panel).
– Corrected text (page 5, right column): In order to explore further, we compared T eff determination with Gaidos & Mann (2014; hereafter G14) along with Passegger et al. (2018), for the common stars in our sample as shown in Fig 5 (right panel).
– Corrected text (page 6, left column): Passegger et al. (2018) compare the observed spectra with the synthetic spectra computed using the PHOENIX-ACES models, which are based on the PHOENIX version by Husser et al. (2013), and the equation of state by Barman et al. (2001), as shown in Fig 5 (right panel).
– Corrected text (page 6, right column): Figure 6 (left panel) shows the comparison of log g with Passegger et al. (2018) indicating difference of around 0.2 to 0.6 dex with our values.
– Corrected text (page 7, left column): Figure 6 (right panel) shows the comparison of the [M/H] derived in this study with Passegger et al. (2018) and G14, indicating difference of around 0.2 to 0.4 dex with our values.
References
- Barman, T. S., Hauschildt, P. H., & Allard, F. 2001, ApJ, 556, 885 [NASA ADS] [CrossRef] [Google Scholar]
- Gaidos, E., & Mann, A. W. 2014, ApJ, 791, 54 [NASA ADS] [CrossRef] [Google Scholar]
- Husser, T.-O., Wende-von Berg, S., Dreizler, S., et al. 2013, A&A, 553, A6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Passegger, V. M., Reiners, A., Jeffers, S. V., et al. 2018, A&A, 615, A6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Rajpurohit, A. S., Reylé, C., Allard, F., et al. 2013, A&A, 556, A15 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
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