How do wavelength correlations affect transmission spectra? Application of a new fast and flexible 2D Gaussian process framework to transiting exoplanet spectroscopy

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Volume 686 (June 2024)

A&A, 686 (2024) A89

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Table C.2

Priors used for fitting the 600B and 600RI VLT/FORS2 datasets.

Parameter	Prior Distribution	Prior Range
T₀: Central transit time (days – predicted time)	Uniform	(−0.01, 0.01)
P: Period (days)	Fixed	3.4059095
a/R_*: System scale	Gaussian	(μ = 8.19, σ = 0.1)
ρ²: Transit depth	Uniform	(0, 1)
${\bar{ρ}}_{600 B} :$ $\[\bar{\rho}_{600 \mathrm{B}}\text:\]$ Mean radius ratio (600B)	Gaussian	(μ = 0.12546, σ = 0.00026)
${\bar{ρ}}_{600 R I} :$ $\[\bar{\rho}_{600 \mathrm{RI}} \text:\]$ Mean radius ratio (600RI)	Gaussian	(μ = 0.125054, σ = 0.00035)
b: Impact parameter	Gaussian	(μ = 0.761, σ = 0.018)
F_oot: Baseline flux	Uniform	(0.99, 1.01)
T_grad: Linear Trend in Baseline flux	Uniform	(−0.1, 0.1)
h_CM: Common-mode systematics height scale	Log-uniform	(0.000001, 0.01)
h_HFS: High-frequency systematics height scale	Log-uniform	(0.000001, 0.01)
h_WSS: Wavelength-specific systematics height scale	Log-uniform	(0.000001, 0.01)
l_t: Time length scale (days)	Log-uniform	(1x observation cadence, 2x total time range)
$l_{λ_{C M}} :$ $\[\l_{\lambda_{\mathrm{CM}}}\text:\]$ Wavelength length scale	Log-uniform	(1 bin width, 50x total wavelength range)
$l_{λ_{H F S}} :$ $\[l_{\lambda_{\mathrm{HFS}}} \text:\]$ Wavelength length scale	Log-uniform	(1 bin width, 50x total wavelength range)
σ: White noise amplitude	Log-uniform	(0.00001, 0.01)

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