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.
Stellar and wind parameters obtained from quantitative analysis of our sample of O Vz stars.
Stellar and wind parameters obtained from quantitative analysis of our sample of O V stars.
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 i λ4471, He ii 4541, He i 4686, and Hα.
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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. |
Open with DEXTER |
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Fig. B.1
continued. |
Open with DEXTER |
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Fig. B.2
Observed spectra (black dots) and best-fitting synthetic models (red lines) for the O V subsample. |
Open with DEXTER |
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Fig. B.2
continued. |
Open with DEXTER |
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Fig. B.2
continued. |
Open with DEXTER |
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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. |
Open with DEXTER |
© ESO, 2014
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