Three warm Jupiters orbiting TOI-6628, TOI-3837, and TOI-5027 and one sub-Saturn orbiting TOI-2328

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Table 11

Interior modeling parameters of TOI-6628 b, TOI-3837 b, TOI-5027 b, and TOI-2328 b, calculated using GASTLI and MESA.

	CMF		log(Fe/H)_p		Z_env		Z_p		Z_p/Z_∗
Planet	GASTLI	MESA	GASTLI	MESA	GASTLI	MESA	GASTLI	MESA	GASTLI	MESA
TOI-6628 b	${0.11}_{- 0.08}^{+ 0.11}$ $0.11_{ - 0.08}^{ + 0.11}$	${0.12}_{- 0.07}^{+ 0.06}$ $0.12_{ - 0.07}^{ + 0.06}$	$- {0.55}_{- 1.00}^{+ 1.04}$ $- 0.55_{ - 1.00}^{ + 1.04}$	–	${0.01}_{- 0.01}^{+ 0.05}$ $0.01_{ - 0.01}^{ + 0.05}$	–	${0.14}_{- 0.08}^{+ 0.11}$ $0.14_{ - 0.08}^{ + 0.11}$	${0.12}_{- 0.07}^{+ 0.06}$ $0.12_{ - 0.07}^{ + 0.06}$	4.4±2.7	${3.5}_{- 3.0}^{+ 1.7}$ $3.5_{ - 3.0}^{ + 1.7}$
TOI-3837 b	${0.08}_{- 0.05}^{+ 0.08}$ $0.08_{ - 0.05}^{ + 0.08}$	${0.12}_{- 0.08}^{+ 0.06}$ $0.12_{ - 0.08}^{ + 0.06}$	$- {0.77}_{- 0.84}^{+ 0.95}$ $- 0.77_{ - 0.84}^{ + 0.05}$	–	${0.01}_{- 0.01}^{+ 0.02}$ $0.01_{ - 0.01}^{ + 0.02}$	–	${0.10}_{- 0.06}^{+ 0.08}$ $0.10_{ - 0.06}^{ + 0.08}$	${0.12}_{- 0.08}^{+ 0.06}$ $0.12_{ - 0.08}^{ + 0.06}$	13.2±8.3	${15.0}_{- 10.0}^{+ 7.5}$ $15.0_{ - 10.0}^{ + 7.5}$
TOI-5027 b	${0.47}_{- 0.24}^{+ 0.19}$ $0.47_{ - 0.24}^{ + 0.19}$	0.14±−0.13	$- {0.20}_{- 1.29}^{+ 1.59}$ $- 0.20_{ - 1.29}^{ + 1.59}$	–	${0.01}_{- 0.01}^{+ 0.28}$ $0.01_{ - 0.01}^{ + 0.28}$	–	${0.54}_{- 0.21}^{+ 0.17}$ $0.54_{ - 0.21}^{ + 0.17}$	0.14 ± 0.13	48.6±17.1	13.2±12.2
TOI 2328 b	${0.29}_{- 0.16}^{+ 0.20}$ $0.29_{ - 0.16}^{ + 0.20}$	–	$- {0.30}_{- 1.18}^{+ 1.16}$ $- 0.30_{ - 1.18}^{ + 1.16}$	–	${0.01}_{- 0.01}^{+ 0.09}$ $0.01_{ - 0.01}^{ + 0.09}$	–	0.34 ± 0.17	–	18.5± 8.2	–

Notes. GASTLI mean and 1σ uncertainties of the free parameters are derived from the posterior distribution functions obtained by the interior structure MCMC retrieval. These parameters correspond to the core-mass fraction (CMF), the atmospheric metallicity (× solar), the envelope metal-mass fraction Z_env , and the total bulk metal mass fraction Z_planet. MESA mean and 1σ uncertainties of the interior model parameters are calculated following Jones et al. (2024).

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