The Hot-Neptune Initiative (HONEI) - I. Two hot sub-Neptunes on a close-in eccentric orbit (TOI-5800 b) and a farther-out circular orbit (TOI-5817 b)

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Volume 701 (September 2025)

A&A, 701 (2025) A79

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Table B.4

Priors utilised for the parameters of the preferred joint model fit of Sect. 3.4.

Parameter		Prior distribution TOI-5800	Prior distribution TOI-5817
Keplerian Parameters:
ρ_⋆	[g cm⁻³]	𝒩(2.41, 0.21)	𝒩(0.47, 0.05)
T_0,b	[BJD_TDB − 2459000]	𝒩(771.71, 0.01)	𝒩(799.30, 0.01)
P_b	[d]	𝒩(2.628, 0.001)	𝒩(15.61, 0.01)
$e_{b}^{}$ $\[e_{b}^{}\]$		0	0
$ω_{b}^{}$ $\[\omega_{b}^{}\]$		90	90
Transit Parameters:
R_p/R_⋆		𝒰(0.0, 1.0)	𝒰(0.0, 1.0)
D		1.0	1.0
q₁ (TESS)		𝒰(0, 1)	𝒰(0, 1)
q₂ (TESS)		𝒰(0, 1)	𝒰(0, 1)
Light curve GP Hyperparameters:
σ_TESS	[ppt]	ℒ(10⁻⁵, 1)	ℒ(10⁻⁵, 1)
ρ_TESS	[d]	ℒ(10⁻¹, 100)	ℒ(10⁻¹, 100)
RV parameters:
K_b	[m s⁻¹]	𝒰(0, 20)	𝒰(0, 10)
${\bar{μ}}_{HARPS}$ $\[\bar{\mu}_{\text {HARPS }}\]$	[m s⁻¹]	𝒰(−20, 20)	−
σ_HARPS	[m s⁻¹]	𝒰(0, 10)	−
${\bar{μ}}_{HARPS-N}$ $\[\bar{\mu}_{\text {HARPS-N}}\]$	[m s⁻¹]	−	𝒰(−20852, −20752)
σ_HARPS-N	[m s⁻¹]	−	𝒰(0, 10)

Notes. 𝒰(a, b) indicates a uniform distribution between a and b, ℒ(a, b) a log-normal distribution, and 𝒩(a, b) a normal distribution, where a and b are the mean and standard deviation. ^(*) In the case of non-null eccentricity, the priors are set as follows: ( $\sqrt{e} \sin ω, \sqrt{e} \cos ω$ $\[\sqrt{e} \sin~ \omega, \sqrt{e} \cos~ \omega\]$ ) in 𝒰(−1.0, 1.0).

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