Precise characterisation of HD 15337 with CHEOPS: A laboratory for planet formation and evolution

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Volume 686 (June 2024)

A&A, 686 (2024) A282

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Table A.2

Priors used for the internal structure modelling and corresponding posteriors from the best-fit model with error bars corresponding to the 5% and 95% percentiles.

Parameters	Prior	Best-fit
HD 15337 b
fm_core,b	𝒰(0.0, 1.0)^a	${0.14}_{- 0.12}^{+ 0.13}$ $0.14_{ - 0.12}^{ + 0.13}$
fm_mantle,b	𝒰(0.0, 1.0)^a	${0.75}_{- 0.14}^{+ 0.15}$ $0.75_{ - 0.14}^{ + 0.15}$
fm_water,b	𝒰(0.0, 0.5)^a	${0.10}_{- 0.08}^{+ 0.10}$ $0.10_{ - 0.08}^{ + 0.10}$
log m_gas,b (M_⊕)	𝒰(−12, log (0.5 M_b))	$- {9.02}_{- 2.68}^{+ 3.02}$ $- 9.02_{ - 2.68}^{ + 3.02}$
Si_mantle,b^b		${0.40}_{- 0.06}^{+ 0.08}$ $0.40_{ - 0.06}^{ + 0.08}$
Mg_mantle,b^b		${0.44}_{- 0.10}^{+ 0.11}$ $0.44_{ - 0.10}^{ + 0.11}$
Fe_core,b	𝒰(0.81, 1.00)	${0.90}_{- 0.08}^{+ 0.09}$ $0.90_{ - 0.08}^{ + 0.09}$

HD 15337 c
fm_core,c	𝒰(0.0, 1.0)^a	${0.11}_{- 0.10}^{+ 0.13}$ $0.11_{ - 0.10}^{ + 0.13}$
fm_mantle,c	𝒰(0.0, 1.0)^a	${0.60}_{- 0.26}^{+ 0.19}$ $0.60_{ - 0.26}^{ + 0.19}$
fm_water,c	𝒰(0.0, 0.5)^a	${0.28}_{- 0.24}^{+ 0.20}$ $0.28_{ - 0.24}^{ + 0.20}$
log m_gas,c (M_⊕)	𝒰(−12, log (0.5 M_c))	$- {1.53}_{- 0.74}^{+ 0.40}$ $- 1.53_{ - 0.74}^{ + 0.40}$
Si_mantle,c^b		${0.41}_{- 0.06}^{+ 0.08}$ $0.41_{ - 0.06}^{ + 0.08}$
Mg_mantle,c^b		${0.44}_{- 0.10}^{+ 0.11}$ $0.44_{ - 0.10}^{ + 0.11}$
Fe_core,c	𝒰(0.81, 1.00)	${0.90}_{- 0.08}^{+ 0.09}$ $0.90_{ - 0.08}^{ + 0.09}$

Notes. Uniform priors are defined as 𝒰(min, max).

^(a) As mentioned in Section 4.4, the priors on the mass fractions are not independent. Instead, samples are drawn uniformly from the tringular simplex where the sum of the three mass fractions is equal to one.

^(b) Priors are applied on the Si/Fe and Mg/Fe bulk ratios, which are sampled using a Gaussian prior from the stellar values (see Table 2).

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