Evidence of early disk-locking among low-mass members of the Orion Nebula Cluster (Corrigendum)

K. Biazzo; C. H. F. Melo; L. Pasquini; S. Randich; J. Bouvier; X. Delfosse

doi:10.1051/0004-6361/200913125e

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A&A, 533 (2011) C3

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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

A&A 533, C3 (2011)

Evidence of early disk-locking among low-mass members of the Orion Nebula Cluster (Corrigendum)

K. Biazzo¹^,2^,3, C. H. F. Melo², L. Pasquini², S. Randich¹, J. Bouvier⁴ and X. Delfosse⁴

¹ INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
e-mail: kbiazzo@arcetri.astro.it
² ESO – European Southern Observatory, Karl-Schwarzschild-Str. 3, 85748 Garching bei München, Germany
³ INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy
⁴ Laboratoire d’Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France

Key words: open clusters and associations: individual: Orion Nebula Cluster / stars: low-mass / stars: pre-main sequence / stars: late-type / accretion, accretion disks / errata, addenda

Erratum for: A&A 508, 13011312 (2009), DOI: 10.1051/0004-6361/200913125

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 V_rad of 24.87 km s^-1 (with a $σ_{V} rad$ $\hbox{$\sigma_V{}_{\rm rad}$}$ of 2.74 km s^-1), which is fully consistent with the membership in the ONC (e.g., Stassun et al. 1999).

Fig. 8

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

References

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

© ESO, 2011

All Figures

	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 V_rad of 24.87 km s^-1 (with a $σ_{V} rad$ $\hbox{$\sigma_V{}_{\rm rad}$}$ of 2.74 km s^-1), which is fully consistent with the membership in the ONC (e.g., Stassun et al. 1999).
In the text

	Fig. 8 vsini distribution for our low-mass stars. Our vsini limit of 9 km s^-1 is shown with a dotted line.
In the text

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