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

Issue
A&A
Volume 512, March-April 2010
Article Number C1
Number of page(s) 1
Section Letters
DOI https://doi.org/10.1051/0004-6361/200912505e
Published online 31 March 2010
A&A 512, C1 (2010)

The secondary eclipse of the transiting exoplanet CoRoT-2b[*] (Corrigendum)

R. Alonso1 - T. Guillot2 - T. Mazeh3,4 - S. Aigrain5 - A. Alapini5 - P. Barge6 - A. Hatzes7 - F. Pont5

1 - Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
2 - Observatoire de la Côte d'Azur, Laboratoire Cassiopée, CNRS UMR 6202, BP 4229, 06304 Nice Cedex 4, France
3 - Radcliffe Institute for Advanced Studies at Harvard, 8 Garden St., Cambridge, MA 02138, USA
4 - School of Physics and Astronomy, R. and B. Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel
5 - School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK
6 - Laboratoire d'Astrophysique de Marseille, UMR 6110, Technopole de Marseille-Etoile, 13388 Marseille Cedex 13, France
7 - Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany



Key words: planetary systems - techniques: photometric - errata, addenda

As noticed by Snellen et al. (2009), there was an error in the calculation of the brightness temperature from the observed eclipse depths. We have corrected this mistake. The relevant parts of the paper that are affected should read as follows:

  • Section 4, 4th sentence: we used a value of $T_{\rm eff}$ = 5625 $\pm$ 120 K for the star (Alonso et al. 2008a), and the model spectrum of a G5V star from Pickles (1998), obtaining $T_{\rm p,CoRoT}$ = 2120 +95-110 K.

  • Section 4, 12th sentence: if we further assume that $F_{\rm p,internal}=0$ and that the planet is in thermal equilibrium[*], this temperature favors unrealistic high values of the re-distribution factor f>0.70.

  • Section 4, 2nd paragraph: assuming blackbody radiation and negligible $F_{\rm p,internal}$, Fig. 6 shows that likely values of the albedo (corresponding to f between 0.25 and 0.5) are $A_{\rm g}=0.085$ $\pm$ 0.045.
The rest of the discussion remains unaffected.

\begin{figure}
\par\includegraphics[width=8.5cm,clip]{12505efg1.ps}
\end{figure} Figure 6:

The equilibrium temperature of CoRoT-2b as a function of the albedo matching the observed secondary eclipse depth. The zero-albedo equilibrium temperature is about 2120 K. In dotted lines, we plot the re-distribution factors f. Realistic re-distribution factors require the contribution of some reflected light (non zero albedo) or the presence of an additional source of energy in the planet (assumed zero in this plot).

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References

Footnotes

... CoRoT-2b[*]
Based on observations obtained with CoRoT, a space project operated by the French Space Agency, CNES, with participation of the Science Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany and Spain.
... equilibrium[*]
$T_{\rm eq}=T_\star(R_\star/a)^{1/2}[f(1-A)]^{1/4}$.

All Figures

  \begin{figure}
\par\includegraphics[width=8.5cm,clip]{12505efg1.ps}
\end{figure} Figure 6:

The equilibrium temperature of CoRoT-2b as a function of the albedo matching the observed secondary eclipse depth. The zero-albedo equilibrium temperature is about 2120 K. In dotted lines, we plot the re-distribution factors f. Realistic re-distribution factors require the contribution of some reflected light (non zero albedo) or the presence of an additional source of energy in the planet (assumed zero in this plot).

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In the text

Copyright ESO 2010

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