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 E.1

List of archival spectroscopic data used in this work.

Target	Observatory	Instrument	Band	Wavelength [μm]	λ/Δλ	Reference
AF Lep b	VLT	SPHERE	YJH	1.0 − 1.6	70	[1]
AF Lep b	VLT	GRAVITY	K	2.0 − 2.5	1000	[1]
HR 8799 e	VLT	SPHERE	YJH	1.0 − 1.7	70	[2]
HR 8799 e	Gemini	GPI	H	1.5 − 1.8	200	[2]
HR 8799 e	VLT	GRAVITY	K	2.0 − 2.5	1000	[2]
HR 8799 c	Gemini	GPI	H	1.5 − 1.8	200	[2]
HR 8799 c	VLT	CHARIS	JHK	1.2 − 2.4	30	[2]
HR 8799 c	VLT	GRAVITY	K	2.0 − 2.5	1000	[2]
HR 2562 B	VLT	SPHERE	YJ	1.0 − 1.3	110	[3]
HR 2562 B	VLT	SPHERE-IFS	YJ	1.0 − 1.3	110	[4]
HR 2562 B	Gemini	GPI	J	1.1 − 1.3	190	[3]
HR 2562 B	Gemini	GPI	H	1.5 − 1.8	200	[3]
HR 2562 B	Gemini	GPI	K1	1.9 − 2.1	240	[3]
HR 2562 B	Gemini	GPI	K2	2.1 − 2.4	280	[3]
HIP 78530 B	Gemini	GNIRS	YJ	0.9 − 1.3	740	[5]
HIP 78530 B	Gemini	GNIRS	H	1.4 − 1.8	1100	[5]
HIP 78530 B	Gemini	GNIRS	K	2.0 − 2.4	1400	[5]
AB Pic b	VLT	SINFONI	J	1.1 − 1.4	8500	[6]
AB Pic b	VLT	SINFONI	H	1.5 − 1.8	3300	[6]
AB Pic b	VLT	SINFONI	K	2.0 − 2.5	4400	[6]
AB Pic b	LCO	MagAOClio	L	2.9 − 4.0	820	[7]
ROXs 42 B b	Gemini	NIFS	J	1.1 − 1.4	11800	[8]
ROXs 42 B b	Keck	OSIRIS	H	1.5 − 1.8	8200	[9]
ROXs 42 B b	Gemini	NIFS	H	1.5 − 1.8	10200	[8]
ROXs 42 B b	Keck	OSIRIS	K	2.0 − 2.4	8700	[8]
ROXs 42 B b	VLT	SINFONI	K	1.9 − 2.5	9000	[9]
ROXs 12 b	Gemini	NIFS	J	1.1 − 1.4	11800	[10]
ROXs 12 b	Keck	OSIRIS	J	1.2 − 1.3	8500	[10]
ROXs 12 b	Keck	OSIRIS	H	1.5 − 1.8	8200	[10]
ROXs 12 b	Keck	OSIRIS	K	2.0 − 2.4	8700	[10]
VHS 1256 b	JWST	NIRSpec	g140h–g395h	1.0 − 5.3	6100	[11]
VHS 1256 b	JWST	MIRI	1A–3C	4.9 − 18.0	5300	[11]
2M J0219 b	LCO	FIRE	YJ	0.9 − 1.3	5100	[12]
2M J0219 b	LCO	FIRE	H	1.4 − 1.8	5000	[12]
2M J0219 b	LCO	FIRE	K	2.0 − 2.4	5000	[12]
CT Cha b	VLT	SINFONI	J	1.1 − 1.3	8500	[13]

Notes. References: [1] Balmer et al. (2025a), [2] Nasedkin et al. (2024), [3] Godoy et al. (2024), [4] Mesa et al. (2018), [5] Lachapelle et al. (2015), [6] Palma-Bifani et al. (2023), [7] Stone et al. (2016), [8] Bowler et al. (2014), [9] Currie et al. (2014c), [10] Bowler et al. (2017), [11] Miles et al. (2023), [12] Artigau et al. (2015), [13] Bonnefoy et al. (2014).

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