EDP Sciences
Free Access
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., Hγ, He iλ4471, He ii 4541, He i 4686, and Hα.

thumbnail Fig. B.1

Observed spectra (black dots) and best-fitting synthetic models (red lines) of Hγ, He iλ4471, He iiλ4541, He iiλ4686 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.

Open with DEXTER

thumbnail Fig. B.2

Observed spectra (black dots) and best-fitting synthetic models (red lines) for the O V  subsample.

Open with DEXTER

thumbnail 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.

Open with DEXTER


© ESO, 2014

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