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

Issue
A&A
Volume 540, April 2012
Article Number C1
Number of page(s) 1
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/200810284e
Published online 14 March 2012

Table 9

Comparison with theoretical evolutionary models: difference between the evolutionary and observed masses.

Minus signs had been accidentally dropped in Table 9, which compares the dynamical mass with the theoretical mass obtained from interpolation of evolutionary tracks in the HR diagram. Furthermore, the error bars had been omitted. We provide here the corrected Table 9. The errors on Δℳ are computed according to the formula where ℳ is the dynamical mass and ℳint is the mass interpolated in the HR diagram from the theoretical evolutionary tracks. One has with Teff,max,min = Teff ± σ(Teff) and Lmax,min = L ± σ(L).

The interpolation procedure was tested by running it on a grid of only 5 evolutionary tracks (3, 5, 9, 15, 25 M) instead of 9 (2.5, 3, 4, 5, 7, 9, 12, 15, 20 M); it recovered the values interpolated in the full grid to better than 0.01 M in most cases, an to within a few times 0.01 M in some unfavourable cases.

Figure 9, which corresponds to Table 9, was correct.

These corrections do not affect the conclusion that many components of detached systems appear slightly overluminous for their dynamical mass, or that their evolutionary mass tend to be larger than their dynamical mass, a trend also pointed out recently by Massey et al. (2012).

References

  • Massey, P., Morrell, N. I., Neugent, K. F., et al. 2012, ApJ, in press [arXiv:astro-ph/1201.3280] [Google Scholar]

© ESO, 2012

All Tables

Table 9

Comparison with theoretical evolutionary models: difference between the evolutionary and observed masses.

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