Free Access
Erratum
This article is an erratum for:
[https://doi.org/10.1051/0004-6361/200913125]


Issue
A&A
Volume 533, September 2011
Article Number C3
Number of page(s) 1
Section Galactic structure, stellar clusters and populations
DOI https://doi.org/10.1051/0004-6361/200913125e
Published online 16 September 2011

thumbnail Fig. 6

Radial velocity distribution for our sample of stars with M < 0.25   M. For the most probable binaries we plot the mean values of the two components (Table 2). The Gaussian fit of the distribution yields a mean Vrad of 24.87 km s-1 (with a of 2.74 km s-1), which is fully consistent with the membership in the ONC (e.g., Stassun et al. 1999).

Open with DEXTER

thumbnail Fig. 8

vsini distribution for our low-mass stars. Our vsini limit of 9 km s-1 is shown with a dotted line.

Open with DEXTER

References

  1. Stassun, K. G., Mathieu, R. D., Mazeh, T., & Vrba, F. J. 1999, AJ, 117, 2941 [NASA ADS] [CrossRef] [Google Scholar]

© ESO, 2011

All Figures

thumbnail Fig. 6

Radial velocity distribution for our sample of stars with M < 0.25   M. For the most probable binaries we plot the mean values of the two components (Table 2). The Gaussian fit of the distribution yields a mean Vrad of 24.87 km s-1 (with a of 2.74 km s-1), which is fully consistent with the membership in the ONC (e.g., Stassun et al. 1999).

Open with DEXTER
In the text
thumbnail Fig. 8

vsini distribution for our low-mass stars. Our vsini limit of 9 km s-1 is shown with a dotted line.

Open with DEXTER
In the text

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