The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud

T. Shenar; D. P. Sablowski; R. Hainich; H. Todt; A. F. J. Moffat; L. M. Oskinova; V. Ramachandran; H. Sana; A. A. C. Sander; O. Schnurr; N. St-Louis; D. Vanbeveren; Y. Götberg; W.-R. Hamann

doi:10.1051/0004-6361/201935684e

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201935684]

Issue		A&A Volume 641, September 2020


Article Number		C2
Number of page(s)		2
Section		Stellar structure and evolution
DOI		https://doi.org/10.1051/0004-6361/201935684e
Published online		03 September 2020

A&A 641, C2 (2020)

Spectroscopy, orbital analysis, formation, and evolution (Corrigendum)

T. Shenar¹, D. P. Sablowski², R. Hainich³, H. Todt³, A. F. J. Moffat⁴, L. M. Oskinova³, V. Ramachandran³, H. Sana¹, A. A. C. Sander⁵, O. Schnurr⁶, N. St-Louis⁴, D. Vanbeveren⁷, Y. Götberg⁸ and W.-R. Hamann³

¹ Institute of Astrophysics, KU Leuven, Celestijnlaan 200D, 3001 Leuven, Belgium
e-mail: tomer.shenar@kuleuven.be
² Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
³ Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, 14476 Potsdam, Germany
⁴ Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, 6128, Succ. Centre-Ville, Montréal, Québec H3C 3J7, Canada
⁵ Armagh Observatory, College Hill, BT61 9DG Armagh, UK
⁶ Cherenkov Telescope Array Observatory gGmbH, Via Piero Gobetti 93/3, 40126 Bologna, Italy
⁷ Astronomy and Astrophysics Research Group, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium
⁸ The observatories of the Carnegie institution for science, 813 Santa Barbara St., Pasadena, CA 91101, USA

Key words: stars: massive / stars: Wolf-Rayet / Magellanic Clouds / binaries: close / binaries: spectroscopic / errata, addenda

Erratum for: A&A 627, A151 (2019), https://doi.org/10.1051/0004-6361/201935684

The mass-loss rates Ṁ provided for the Wolf-Rayet (WR) stars in Table 2 in the original paper were derived from the transformed radii R_t. While R_t is correctly defined in the paper (Eq. (2)), an incorrect exponent was implemented in the script used to calculate them (3/2 instead of 2/3). As a consequence, the Ṁ values, Fig. 22, and the coefficients given in Table 5 in the original paper for the Ṁ relations (Eq. (6)) are impacted. Tables 1 and 2 in this corrigendum list the revised values, and Fig. 1 shows the revised version of Fig. 22 in the original paper. Moreover, a typo pertaining to the R_t value of BAT99 119 is corrected.

Fig. 1.

Revised version of Fig. 22 from the original paper with updated mass-loss rates.

Table 1.

Revised mass-loss rates for LMC WR binaries.

Table 2.

Coefficients for the log Ṁ prescription (cf. Table 5 and Eq. (6) in the original paper).

Since the WR population studied here comprises a small fraction of the sample used to derive to mass-luminosity relation, the impact on the derived coefficients is limited, with changes smaller than the respective 1σ errors (cf. Table 5 in the original paper and Table 2 in this corrigendum). Moreover, these measurements have no impact on our main conclusions.

© ESO 2020

All Tables

Table 1.

Revised mass-loss rates for LMC WR binaries.

In the text

Table 2.

Coefficients for the log Ṁ prescription (cf. Table 5 and Eq. (6) in the original paper).

In the text

All Figures

	Fig. 1. Revised version of Fig. 22 from the original paper with updated mass-loss rates.
In the text

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