Table 4:

Priors used for HD 49933 data analysis. $\nu _{\rm s}$ is the rotational splitting, i the star inclination angle, $\delta \nu _{02}$ the small frequency separation, $\Delta \nu $ the large separation. The value of $\epsilon $ and D0 depend on the model and set the position of the first prior frequency (see Eq. (2)).
Parameter Prior nature Values
$\nu _{\rm s}$ Gaussian $3.4\pm0.34$ $\mu {\rm Hz}$
i Uniform $[0^\circ{-}90^\circ]$
$\delta \nu _{02}$ Gaussian $6 \pm 3$  $\mu {\rm Hz}$
$\Delta \nu $ Gaussian $85.6 \pm 0.8$  $\mu {\rm Hz}$
$\epsilon $ Fixed 1.55 ($M_{\rm A}$) / 1.05 ($M_{\rm B}$)
D0 Fixed 1 $\mu {\rm Hz}$
Parameter Prior nature $x_{\rm min}$ $x_{\rm max}$

h (ppm2/$ \mu Hz)$
Jeffrey 1 10
Vl=1 Jeffrey 1.5 5
Vl=2 Jeffrey 0.5 5
$\Gamma$ $(\mu {\rm {Hz}})$ Jeffrey 5 25
$\nu _{\rm s}$ is the rotational splitting, i the star inclination angle, $\delta \nu _{02}$ the small frequency separation, $\Delta \nu $ the large separation. The value of $\epsilon $ and D0 depend on the model and set the position of the first prior frequency (see Eq. (2)).

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