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Erratum
This article is an erratum for: [this article]

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

An error occurred during the production process. Figure 1 was published twice. The corrected Figs. 1 and 2 are published below.

thumbnail 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

thumbnail 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

thumbnail 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
thumbnail 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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