The solar-like oscillations of HD 49933: a Bayesian approach

Free access article

Issue		A&A Volume 506, Number 1, October IV 2009 The CoRoT space mission: early results


Page(s)		15 - 32
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361/200911657
Published online		03 September 2009

Online Material

Table 10: HD 49933 frequencies and height-to-noise posterior estimates for l=0 and l=1 modes for the $M^2_{\rm A}$ model. n is given supposing $\epsilon \in [1,2]$ . H/N represents the height-to-noise ratio in the power spectrum.

Table 11: Height and width posterior estimates for HD 49933 for the model $M^2_{\rm A}$ . n is given for the l=0 modes.

Table 12: Energy posterior estimates for HD 49933, model $M^2_{\rm A}$ . n is given for the l=0 modes.

Table 13: HD 49933 frequencies and height-to-noise posterior estimates for the l=0 and l=1 modes for the $M^2_{\rm B}$ model. n is given supposing $\epsilon \in [1,2]$ . H/N represents the height-to-noise ratio in the power spectrum.

Table 14: Height and width posterior estimates for HD 49933 for the model $M^2_{\rm B}$ . n is given for the l=0 modes.

Table 15: Energy posterior estimates for HD 49933, model $M^2_{\rm B}$ . n is given for the l=0 modes.

$\begin{figure} \par\subfigure{\epsfig{figure=11657_ZD.ps,width=6.cm,height=18cm,angle=90} } \par \end{figure}$	Figure 11: HD 49933 power spectrum and echelle diagram for $M^2_{\rm A}$ model (identification A with l=2 modes). The superimposed dashed line is the best fit according to the median value of the parameters.
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$\begin{figure} \par\subfigure{\epsfig{figure=11657_ZE.ps,width=6.cm,height=18cm,angle=90} } \par \end{figure}$	Figure 12: HD 49933 power spectrum and echelle diagram for $M^1_{\rm B}$ model (identification B without l=2 modes). The superimposed dashed line is the best fit according to the median value of the parameters.
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