Validation of up to seven TESS planet candidates through multi-colour transit photometry using MuSCAT2 data

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Volume 690 (October 2024)

A&A, 690 (2024) A62

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Table 3

Prior probability distributions of the fitted parameters.

Description	Parameter	Value
Global parameters

Orbital period	P (days)	$N$ $\[\mathcal{N}\]$ ⁽^a⁾
Stellar density	ρ_* (g/cm³)	$U$ $\[\mathcal{U}\]$ (1, 35)
Impact parameter	b	$U$ $\[\mathcal{U}\]$ (0, 1)
Zero epoch	T₀	$N$ $\[\mathcal{N}\]$ ^(a)
Robust area ratio	$k_{true}^{2}$ $\[k_{\text {true }}^2\]$	$U$ $\[\mathcal{U}\]$ (1, 0)
Host temperature	T_h (K)	$N$ $\[\mathcal{N}\]$ ^(a)
Cont. temperature	T_c (K)	$U$ $\[\mathcal{U}\]$ (1200, 7000)
Passband-dependent parameters

Limb darkening	q	$N$ $\[\mathcal{N}\]$ ^(b)
Light-curve-dependent parameters

Log₁₀ white noise	log₁₀ σ	$U$ $\[\mathcal{U}\]$ (−4, 0)^(c)

Notes. Transit light curve model parameters and priors. Individual target posteriors are shown in Tables A.1 and A.2. The global parameters are independent of the passband or light curve. The passband-dependent parameters are specified for each passband, and the light-curve-dependent parameters are repeated for each individual light curve. $N$ $\[\mathcal{N}\]$ stands for a normal prior, and $U$ $\[\mathcal{U}\]$ (a, b) stands for a uniform distribution from a to 4b4. ^(a)Centered on the ExoFOP values. Prior σ equals three times the nominal error bars. For the uniform distributions, the whole interval equals six times the nominal error bars. ^(b)Limb darkening coefficients correspond to the transformed power-2 limb darkening law coefficients (Hestroffer 1997; Morello et al. 2017; Short et al. 2019) and have normal priors calculated using LDTK. ^(c)Average log₁₀ white noise parameters for each light curve have uninformative uniform priors.

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