The VLT-FLAMES Tarantula Survey - XIII: On the nature of O Vz stars in 30 Doradus

C. Sabín-Sanjulián; S. Simón-Díaz; A. Herrero; N. R. Walborn; J. Puls; J. Maíz Apellániz; C. J. Evans; I. Brott; A. de Koter; M. Garcia; N. Markova; F. Najarro; O. H. Ramírez-Agudelo; H. Sana; W. D. Taylor; J. S. Vink

doi:10.1051/0004-6361/201322798

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Volume 564 (April 2014)

A&A, 564 (2014) A39

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Issue		A&A Volume 564, April 2014


Article Number		A39
Number of page(s)		24
Section		Stellar structure and evolution
DOI		https://doi.org/10.1051/0004-6361/201322798
Published online		02 April 2014

Online material

Appendix A: Tables

Tables A.1 and A.2 present the stellar parameters from our HHe analysis of the O Vz and O V samples. Table A.3 presents first estimates for the stars where it was also necessary to use nitrogen lines in the analysis due to weak He i lines and/or strong nebular contamination.

Table A.1

Stellar and wind parameters obtained from quantitative analysis of our sample of O Vz stars.

Table A.2

Stellar and wind parameters obtained from quantitative analysis of our sample of O V stars.

Table A.3

First estimates of stellar and wind parameters from HHeN analysis of the subsample of stars for which He i-ii analysis alone was considered unreliable (see notes in Sect. 4).

Appendix B: Figures

Figures B.1 to B.3 show the best-fitting models to the observed VFTS spectra for the most important diagnostic lines in this study, i.e., H_γ, He i λ4471, He ii 4541, He i 4686, and H_α.

	Fig. B.1 Observed spectra (black dots) and best-fitting synthetic models (red lines) of Hγ, He i λ4471, He ii λ4541, He ii λ4686 and Hα for the O Vz subsample. Each spectrum is labeled with its VFTS number and spectral classification. The cores of strong nebular lines have been removed.
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	Fig. B.1 continued.
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	Fig. B.2 Observed spectra (black dots) and best-fitting synthetic models (red lines) for the O V subsample.
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	Fig. B.2 continued.
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	Fig. B.2 continued.
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	Fig. B.3 Observed spectra (black dots) and best-fitting synthetic models (pink lines) for the O Vz and O V stars analyzed using H, He and N as the diagnostic lines.
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© ESO, 2014

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