Evidence of a gap in the envelope mass fraction of sub-Saturns

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Table A.1

Input properties and ages from the stardate modeling of host stars.

Star	T_eff[K]	Fe/H	R_*[R_⊙]	Lit. Age [Gyr]	v sin (i)	P_rot [days]	References	Age [Gyr]
EPIC 211945201	6025 ± 100	0.1 ± 0.1	$1 . 38_{- 0.018}^{+ 0.017}$ $1.38_{-0.018}^{+0.017}$	$3 . 99_{- 0.7}^{+ 0.85}$ $3.99_{-0.7}^{+0.85}$	2.93 ± 0.58	24.0 ± 4.7	1, 2	$4 . 4_{- 1.0}^{+ 0.7}$ $4.4_{-1.0}^{+0.7}$
K2-24	5726 ± 65	0.41 ± 0.05	1.185 ± 0.011	4.9 ± 1.7	1.503 ± 1.0	40.1 ± 27.0	3, 4	$13 . 4_{- 0.4}^{+ 0.9}$ $13.4_{-0.4}^{+0.9}$
K2-280	5500 ± 100	0.33 ± 0.08	1.28 ± 0.07	8.96 ± 1.7	2.6 ± 0.61	25.1 ± 6.0	5, 2	$10 . 2_{- 1.3}^{+ 7.0}$ $10.2_{-1.3}^{+7.0}$
KOI-1783	5922 ± 60	0.11 ± 0.04	$1 . 14_{- 0.03}^{+ 0.04}$ $1.14_{-0.03}^{+0.04}$	-	2.8 ± 1.0	20.8 ± 7.4	6, 4	3.4 ± 0.07
KOI-94	$6184_{- 160}^{+ 110}$ $6184_{-160}^{+110}$	0.11 ± 0.07	$1 . 43_{- 0.10}^{+ 0.09}$ $1.43_{-0.10}^{+0.09}$	-	7.1 ± 0.77	10.3 ± 1.3	7, 2	$2 . 5_{- 0.7}^{+ 0.4}$ $2.5_{-0.7}^{+0.4}$
Kepler-103	$6047_{- 70}^{+ 50}$ $6047_{-70}^{+50}$	0.15 ± 0.04	$1 . 492_{- 0.022}^{+ 0.024}$ $1.492_{-0.022}^{+0.024}$	-	3.34 ± 0.55	22.7 ± 3.8	8, 2	${5.2}_{- 1.0}^{+ 0.5}$ $5.2^{+0.5}_{-1.0}$
Kepler-111	5914 ± 90	0.237 ± 0.06	1.145 ± 0.04	$3 . 4_{- 2.2}^{+ 3.1}$ $3.4_{-2.2}^{+3.1}$	2.8 ± 1.0	20.8 ± 7.5	9, 10	$2 . 6_{- 0.8}^{+ 0.9}$ $2.6_{-0.8}^{+0.9}$
Kepler-117	6150 ± 110	−0.04 ± 0.1	1.61 ± 0.05	5.3 ± 1.4	7.4 ± 1.0	10.8 ± 1.5	11, 10	$3 . 58_{- 0.27}^{+ 0.4}$ $3.58_{-0.27}^{+0.4}$
Kepler-1513	5491 ± 100	0.17 ± 0.06	$0 . 95_{- 0.06}^{+ 0.08}$ $0.95_{-0.06}^{+0.08}$	$7 . 0_{- 4.2}^{+ 4.0}$ $7.0_{-4.2}^{+4.0}$	1.7 ± 0.5	28.4 ± 8.7	12, 13	4.1 ± 1.9
Kepler-450	6152 ± 100	0.13 ± 0.02	${1.64}_{- 0.11}^{+ 0.08}$ $1.64_{-0.11}^{+0.08}$	−	13.4 ± 1.0	6.2 ± 0.6	7, 4	$3 . 67_{- 017}^{+ 0.11}$ $3.67_{-017}^{+0.11}$
Kepler-849	$5950_{- 130}^{+ 140}$ $5950_{-130}^{+140}$	0.145 ± 0.06	$1 . 82_{- 0.08}^{+ 0.07}$ $1.82_{-0.08}^{+0.07}$	${4.7}_{- 1.6}^{+ 1.8}$ $4.7_{-1.6}^{+1.8}$	4.6 ± 0.52	20.1 ± 2.4	9, 2	$3 . 90_{- 0.23}^{+ 0.3}$ $3.90_{-0.23}^{+0.3}$
Kepler-9	5774 ± 60	0.05 ± 0.07	0.96 ± 0.02	$2 . 0_{- 1, 3}^{+ 2.0}$ $2.0_{-1,3}^{+2.0}$	2.78 ± 0.6	17.5 ± 3.8	14, 2	$2 . 5_{- 1.1}^{+ 0.9}$ $2.5_{-1.1}^{+0.9}$
TIC 139270665	6033 ± 90	0.19 ± 0.06	1.34 ± 0.05	${3.7}_{- 1.7}^{+ 2.1}$ $3.7_{-1.7}^{+2.1}$	4.2 ± 1.0	16 ± 6	15	3.8 ± 0.5
TOI-1386	5793 ± 80	0.16 ± 0.06	1.02 ± 0.03	${3.3}_{- 2.2}^{+ 3.5}$ $3.3_{-2.2}^{+3.5}$	4.0 ± 2.0	12.9 ± 6.5	16	${4.2}_{- 1.2}^{+ 1.5}$ $4.2_{-1.2}^{+1.5}$
TOI-1439	5841 ± 70	$0 . 23_{- 0.07}^{+ 0.06}$ $0.23_{-0.07}^{+0.06}$	1.62 ± 0.03	$4 . 6_{- 0.7}^{+ 1.6}$ $4.6_{-0.7}^{+1.6}$	5.0 ± 2.0	16.5 ± 6.6	17	$5 . 0_{- 0.4}^{+ 0.4}$ $5.0_{-0.4}^{+0.4}$
TOI-1836	6198 ± 100	−0.1 ± 0.1	1.66 ± 0.03	$3 . 5_{- 0.5}^{+ 1.3}$ $3.5_{-0.5}^{+1.3}$	5.9 ± 1.0	14.3 ± 2.5	18	${4.8}_{- 0.1}^{+ 0.9}$ $4.8_{-0.1}^{+0.9}$
TOI-2019	5588 ± 130	0.4 ± 0.1	1.73 ± 0.03	$6 . 0_{- 1.0}^{+ 1.0}$ $6.0_{-1.0}^{+1.0}$	1.6 ± 1.0	55.0 ± 34.4	18	$4 . 93_{- 0.11}^{+ 0.12}$ $4.93_{-0.11}^{+0.12}$
TOI-2134	4620 ± 80	0.13 ± 0.04	$0 . 71_{- 0.03}^{+ 0.02}$ $0.71_{-0.03}^{+0.02}$	$3 . 8_{- 2.7}^{+ 5.5}$ $3.8_{-2.7}^{+5.5}$	0.78 ± 0.1	46.6 ± 6.1	19	$7 . 1_{- 3.1}^{+ 2.3}$ $7.1_{-3.1}^{+2.3}$
TOI-2525	5096 ± 110	0.14 ± 0.05	0.78 ± 0.04	${3.99}_{- 2.6}^{+ 4.3}$ $3.99_{-2.6}^{+4.3}$	1.5 ± 0.3	26.6 ± 5.4	20	$10 . 6_{- 2.2}^{+ 3.6}$ $10.6_{-2.2}^{+3.6}$
TOI-4994	5640 ± 110	0.16 ± 0.09	1.06 ± 0.04	$6 . 3_{- 3.8}^{+ 4.2}$ $6.3_{-3.8}^{+4.2}$	−	46.2 ± 3.1	21	$12 . 7_{- 0.8}^{+ 2.2}$ $12.7_{-0.8}^{+2.2}$
TOI-5678	5485 ± 70	0.0 ± 0.01	0.938 ± 0.007	8.5 ± 3.0	3.1 ± 1.0	15.4 ± 5.0	22	$8 . 8_{- 1.0}^{+ 1.1}$ $8.8_{-1.0}^{+1.1}$
HD 332231	6089 ± 100	0.04 ± 0.06	1.28 ± 0.04	$4 . 3_{- 1.9}^{+ 2.5}$ $4.3_{-1.9}^{+2.5}$	5.3 ± 1.0	12.3 ± 2.3	23	$3 . 0_{- 0.5}^{+ 0.5}$ $3.0_{-0.5}^{+0.5}$
PH2	5711 ± 60	−0.03 ± 0.04	$0 . 961_{- 0.015}^{+ 0.016}$ $0.961_{-0.015}^{+0.016}$	−	2.0 ± 1.0	24.5 ± 12.2	8	5.0 ± 1.5
TOI-1898	6241 ± 90	−0.10 ± 0.08	1.62 ± 0.03	$3 . 4_{- 0.5}^{+ 1.0}$ $3.4_{-0.5}^{+1.0}$	7.0 ± 1.0	11.8 ± 1.7	18	${3.5}_{- 1.1}^{+ 0.3}$ $3.5_{-1.1}^{+0.3}$
TOI-2328	5525 ± 150	0.09 ± 0.03	0.90 ± 0.06	$4 . 0_{- 2.7}^{+ 2.3}$ $4.0_{-2.7}^{+2.3}$	2.61 ± 0.25	17.6 ± 2.0	24	${7.3}_{- 1.4}^{+ 1.5}$ $7.3_{-1.4}^{+1.5}$
NGTS-11	5050 ± 80	0.22 ± 0.08	0.832 ± 0.013	3.9 ± 1.6	1.1 ± 0.8	38.5 ± 28.0	25	$0 . 6_{- 1.5}^{+ 0.5}$ $0.6_{-1.5}^{+0.5}$
Kepler-30	5498 ± 60	0.18 ± 0.03	0.95 ± 0.12	−	2.2 ± 1.0	22 ± 10	26, 10	$0 . 9_{- 1.6}^{+ 0.7}$ $0.9_{-1.6}^{+0.7}$
Kepler-539	5820 ± 80	−0.01 ± 0.07	0.952 ± 0.034	$1 . 1_{- 0.1}^{+ 0.9}$ $1.1_{-0.1}^{+0.9}$	4.4 ± 0.5	11.0 ± 1.4	27	${0.9}_{- 0.7}^{+ 0.5}$ $0.9_{-0.7}^{+0.5}$
Kepler-1656	5731 ± 60	0.19 ± 0.04	1.10 ± 0.13	$6 . 31_{- 2.9}^{+ 2.1}$ $6.31_{-2.9}^{+2.1}$	2.8 ± 1.0	20 ± 8	28	$1 . 6_{- 1.2}^{+ 0.9}$ $1.6_{-1.2}^{+0.9}$
K2-139	5340 ± 110	0.22 ± 0.08	0.92 ± 0.04	1.8 ± 0.3	2.8 ± 0.6	16.7 ± 3.6	29	$1 . 6_{- 1.8}^{+ 1.1}$ $1.6_{-1.8}^{+1.1}$
TOI-216	5054 ± 110	−0.16 ± 0.09	0.757 ± 0.007	−	5.7 ± 1.0	6.8 ± 1.2	30, 31	$0 . 42_{- 0.22}^{+ + 0.14}$ $0.42_{-0.22}^{+0.14}$
TOI-1710	5665 ± 55	0.10 ± 0.07	$0 . 968_{- 0.014}^{+ 0.016}$ $0.968_{-0.014}^{+0.016}$	$4 . 2_{- 2.7}^{+ 4.1}$ $4.2_{-2.7}^{+4.1}$	2.3 ± 0.4	22 ± 4	32	$2 . 6_{- 2.1}^{+ 0.8}$ $2.6_{-2.1}^{+0.8}$
TOI-1823	4927 ± 60	$0 . 24_{- 0.09}^{+ 0.1}$ $0.24_{-0.09}^{+0.1}$	$0 . 805_{- 0.03}^{+ 0.04}$ $0.805_{-0.03}^{+0.04}$	$6 . 3_{- 4.4}^{+ 6.3}$ $6.3_{-4.4}^{+6.3}$	4.0 ± 2.0	10.2 ± 5.1	17	$1 . 8_{- 4.4}^{+ 1.5}$ $1.8_{-4.4}^{+1.5}$
TOI-2447	5730 ± 80	0.18 ± 0.08	1.006 ± 0.009	2 ± 1	3.5 ± 0.6	14.7 ± 2.5	33	$0 . 6_{- 0.4}^{+ 0.4}$ $0.6_{-0.4}^{+0.4}$
TOI-4010	4960 ± 40	0.37 ± 0.07	0.85 ± 0.02	6.3 ± 3.1	1.3 ± 0.5	33.3 ± 12.8	34	$1 . 5_{- 2.6}^{+ 1.2}$ $1.5_{-2.6}^{+1.2}$

Notes: The second reference for each star is for the v sin (i) value. v sin (i) values for TOI-1386, TOI-1439, and TOI-1823 were calculated from TRES spectra published on Exofop (Kurucz 1992; Fűrész 2008; Buchhave et al. 2010; Buchhave et al. 2012). For comparison, we list the ages calculated in the reference papers of the stellar parameters (if available). At the bottom of the table, we list the stars that did not satisfy the age requirement.

References: 1 Chakraborty et al. (2018); 2 Rainer et al. (2023); 3 Nascimbeni et al. (2024); 4 Abdurro’uf et al. (2022); 5 Nowak et al. (2020); 6 Vissapragada et al. (2020); 7 Stassun et al. (2019); 8 Dubber et al. (2019); 9 Dalba et al. (2024); 10 Petigura et al. (2022); 11 Bruno et al. (2015); 12 Yahalomi et al. (2024); 13 Brewer & Fischer (2018); 14 Borsato et al. (2019); 15 (Dalba & Peluso, private communication); 16 Hill et al. (2024); 17 MacDougall et al. (2023); 18 Chontos et al. (2024); 19 Rescigno et al. (2024); 20 Trifonov et al. (2023); 21 Rodríguez Martínez et al. (2025); 22 Ulmer-Moll et al. (2023); 23 Dalba et al. (2020); 24 Tala Pinto et al. (2025); 25 Gill et al. (2020); 26 Fabrycky et al. (2012); 27 Mancini et al. (2016); 28 Brady et al. (2018); 29 Barragán et al. (2018); 30 Dawson et al. (2019); 31 Sharma et al. (2018); 32 König et al. (2022); 33 Gill et al. (2024); 34 Kunimoto et al. (2023).

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