Observational constraints on the chemical tracers of planet formation history - A systematic survey of 13 directly imaged low-mass companions with VLT/ERIS

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Table J.1

Log evidence, preferred grid and free models, and Bayes factor for the presence of ¹³CO in the atmosphere of our targets.

	Grid models				Free models

Target	SD	ER	BT	Sel.	CD	CDCL	FC	FC13	Sel.	log(K_13/12)
AF Lep b	*	4759	*	ER	−336	−323	−299	−299	FC	−0.2
HR 8799 e	5682	6953	*	ER	−117	−118	−104	−99	FC13	5.1
HR 8799 c	6840	7214	*	ER	−334	−328	−265	−265	FC	−0.6
ROXs 42 B b	7037	*	−11686	SD	−3908	−3898	−3245	−3245	FC13	0.3
AB Pic b	15338	16243	15405	ER	−1326	−1315	−1051	−1061	FC	−9.4
HR 2562 B	8050	8123	8056	ER	203	192	199	225	FC13	25
2M J0219 b	11619	12813	13484	BT	−775	−777	−797	−797	CD	−0.4
VHS 1256 b	−4781251	−2045586	*	ER	−1169574	−870506	−569354	−572657	FC	−3303
CT Cha b	*	*	3116	BT	−1216	−1215	−309	−1160	FC	−851
ROXs 12 b	*	*	8017	BT	−2848	−3187	−2622	−2741	FC	−118
HIP 78530 B	*	*	17591	BT	−2022	−2181	−2111	−2112	CD	−0.6
HIP 79098 AB b	167	*	169	BT	226	225	234	233	FC	−1.1

Notes. The two columns called ‘Sel.’ refer to the preferred grid (respectively free) models. The last column indicates the logarithm of the Bayes factor log(K_13/12) between the free model with the isotopologue ¹³CO and the one without it. A positive value, as is the case for HR 8799 e and HR 2562 B, represents evidence of the presence of the isotopologue. The columns named after the abbreviations of each model report the logarithm of the evidence of the corresponding spectral fit. The abbreviated model names are defined in Table 3 and are repeated here for convenience: SD: Sonora-Diamondback, ER: Exo-REM, BT: BT-Settl CIFIST, CD: Chemical (dis)equilibrium (clear), CDCL: Chemical (dis)equilibrium + cloudy, FC: Free chemistry (clear), FC13: Free chemistry (clear) + ¹³CO.

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