| Issue |
A&A
Volume 530, June 2011
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/201016073 | |
| Published online | 10 May 2011 | |
The VLT-FLAMES survey of massive stars: atmospheric parameters and rotational velocity distributions for B-type stars in the Magellanic Clouds⋆ (Corrigendum)
1
Astrophysics Research Centre, School of Mathematics & Physics,
The Queen’s University of Belfast, Belfast, BT7 1NN, Northern
Ireland, UK
e-mail: I.Hunter@qub.ac.uk
2
The Isaac Newton Group of Telescopes, Apartado de Correos 321, 38700, Santa Cruz de La Palma, Canary
Islands, Spain
3
Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
4
LUTH, Observatoire de Meudon, 5 place Jules Janssen, 92195
Meudon Cedex,
France
5
UK Astronomy Technology Centre, Royal Observatory,
Blackford Hill, Edinburgh, EH9 3HJ, UK
Key words: stars: early-type / stars: atmospheres / stars: rotation / stars: evolution / galaxies: Magellanic Clouds / errata, addenda
An error occurred during the production process. Figure 1 was published twice. The corrected Figs. 1 and 2 are published below.
 |
Fig. 1
Comparison of the projected rotational velocity derived by the profile fitting method and the Fourier transform method for the non-supergiant objects in the sample. The dotted line indicates a one-to-one correlation. The dashed lines indicate a 10% or 10 km s-1 uncertainty, whichever is the larger. |
| Open with DEXTER | |
 |
Fig. 2
Comparison of the projected rotational velocity (vsini) derived by the profile fitting method and the Fourier transform method for the supergiant objects in the sample. The dotted line indicates a one-to-one correlation. The dashed lines indicate a 10 km s-1 uncertainty. Downward pointing arrows indicate those objects where it was only possible to derive upper limits to the vsini from the Fourier method. |
| Open with DEXTER | |
© ESO, 2011
All Figures
|
Fig. 1
Comparison of the projected rotational velocity derived by the profile fitting method and the Fourier transform method for the non-supergiant objects in the sample. The dotted line indicates a one-to-one correlation. The dashed lines indicate a 10% or 10 km s-1 uncertainty, whichever is the larger. |
| Open with DEXTER | |
| In the text | |
|
Fig. 2
Comparison of the projected rotational velocity (vsini) derived by the profile fitting method and the Fourier transform method for the supergiant objects in the sample. The dotted line indicates a one-to-one correlation. The dashed lines indicate a 10 km s-1 uncertainty. Downward pointing arrows indicate those objects where it was only possible to derive upper limits to the vsini from the Fourier method. |
| Open with DEXTER | |
| In the text | |
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