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 A.1

Companion and stellar properties from the literature.

Param.	Unit	AF Lep b	HR 8799 e	HR 8799 c	1RXSJ1609 b	ROXs 42 B b	AB Pic b	HR 2562 B
SpT_S		F8	F0		M0	M0	K1	F5
Age	Myr	24 ± 3	20–40		5–11	2–3	13–45	450–600
$T_{S}^{eff}$ $Mathematical equation: $\[T_{\mathrm{S}}^{\text {eff}}\]$$	K	5901	$7339_{- 5}^{+ 4}$ $Mathematical equation: $\[7339_{-5}^{+4}\]$$		4543	7894	$5285_{- 9}^{+ 10}$ $Mathematical equation: $\[5285_{-9}^{+10}\]$$	$6785_{- 27}^{+ 29}$ $Mathematical equation: $\[6785_{-27}^{+29}\]$$
log(g)_S	cgs	4.2	${4.19}_{- 0.02}^{+ 0.01}$ $Mathematical equation: $\[4.19_{-0.02}^{+0.01}\]$$		4.1	4.3	${4.53}_{- 0.01}^{+ 0.01}$ $Mathematical equation: $\[4.53_{-0.01}^{+0.01}\]$$	${4.40}_{- 0.05}^{+ 0.04}$ $Mathematical equation: $\[4.40_{-0.05}^{+0.04}\]$$
C/O_S			0.54–0.59
[Fe/H]_S		−0.5	$- {0.65}_{- 0.01}^{+ 0.02}$ $Mathematical equation: $\[-0.65_{-0.01}^{+0.02}\]$$		−0.4	−1.2	0.04 ± 0.02	${0.21}_{- 0.03}^{+ 0.02}$ $Mathematical equation: $\[0.21_{-0.03}^{+0.02}\]$$
K_S	mag	4.93 ± 0.02	5.24 ± 0.02		8.92 ± 0.02	8.67 ± 0.02	6.98 ± 0.02	5.02 ± 0.02
A₀	mag	0.0	0.0		1.4	5.6	0.0	0.0
d	pc	26.8	40.8		136.3	144.7	50.1	33.9
RV	km⁻¹	21.1 ± 0.4	−10.4 ± 0.2		−11.7 ± 2.0	−0.7 ± 13.4	22.0 ± 0.2	26.2 ± 0.2

ρ	mas	335–339	368 ± 9	957 ± 10	2140 ± 110	1169–1170	5450–5520	618–665
K_P	mag	16.73 ± 0.11	15.91 ± 0.22	16.11 ± 0.10	16.23 ± 0.06	15.01 ± 0.05	14.14 ± 0.08	15.62 ± 0.10
ΔK	mag	11.80 ± 0.11	10.67 ± 0.22	10.87 ± 0.10	7.43 ± 0.04	6.38 ± 0.01	7.16 ± 0.08	10.60 ± 0.10
SpT_P		L6			L4	L1–M8	L0–L1	L7
M_P	M_J	3.8 ± 0.5	7.6 ± 0.9	7.7 ± 0.7	8.4–10.0	10.0–13.0	11.0–13.5	13.5 ± 5.5
a	au	9.0 ± 0.1	15 ± 0	39 ± 0	292 ± 15	169	273–277	19–30
$T_{P}^{eff}$ $Mathematical equation: $\[T_{\mathrm{P}}^{\text {eff}}\]$$	K	800 ± 50	1138 ± 30	1159 ± 12	2000 ± 100	2270 ± 155	1700 ± 50	1255 ± 15
C/O_P		0.55 ± 0.10	0.87 ± 0.02	0.60 ± 0.02		0.48 ± 0.08	0.58 ± 0.08
[Fe/H]_P		0.8 ± 0.2	1.9 ± 0.2	1.3 ± 0.1		0.0 ± 0.6	0.4 ± 0.2
log(g)	cgs	3.7 ± 0.2	4.2 ± 0.1	4.3 ± 0.0	3.5 ± 0.5	3.5–4.0	4.5 ± 0.3	4.6 ± 0.1
R_P	R_J	1.3 ± 0.1	1.1 ± 0.1	1.1 ± 0.0			1.7 ± 0.5	0.9 ± 0.0
¹²C/¹³C
Ref.		1–3	4–10	4–8, 10, 11	12–15	13, 15–19	6, 15, 20–23	6, 24–29

Notes. The first ten rows describe the stellar parameters, whilst the rest describes the parameters of the companions. The targets are sorted by order of increasing companion mass. Notation: the subscript S indicates the stellar parameters, whilst P indicates the parameters of the companions; SpT denotes the spectral type; T^eff is the effective temperature; log(g) is the surface gravity; C/O is the atmospheric carbon-to-oxygen ratio; [Fe/H] is the atmospheric metallicity; K is the K-band apparent magnitude; A₀ is the ISM extinction measured towards the host star; d is the distance between the Sun and the stellar system; RV is the radial velocity of the star relative to the barycentre of the Solar System; ρ is the angular separation; ΔK is the K-band contrast; M_P is the mass of the companion; a is the projected separation (or the physical separation if available from an orbital fit); R_P is the planetary radius; ¹²C/¹³C is the carbon isotopologue ratio; and Ref. indicates the studies from which the values were taken over. References. 1. Balmer et al. (2025a), 2. Mesa et al. (2023), 3. De Rosa et al. (2023), 4. Baines et al. (2012), 5. Zuckerman et al. (2011), 6. Swastik et al. (2021), 7. Wang et al. (2023), 8. Baburaj et al. (2025), 9. Marois et al. (2010), 10. Nasedkin et al. (2024), 11. Marois et al. (2008), 12. Lafrenière et al. (2008), 13. Kraus et al. (2014a), 14. Lachapelle et al. (2015), 15. Martinez & Kraus (2022), 16. Currie et al. (2014c), 17. Bowler et al. (2014), 18. Xuan et al. (2024), 19. Inglis et al. (2024), 20. Chauvin et al. (2005), 21. Bonnefoy et al. (2014), 22. Stone et al. (2016), 23. Palma-Bifani et al. (2023), 24. Konopacky et al. (2016), 25. Mesa et al. (2018), 26. Sutlieff et al. (2021), 27. Godoy et al. (2024), 28. Maire et al. (2018), 29. Zhang et al. (2023a).

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