Probing Na in giant exoplanets with ESPRESSO and 3D NLTE stellar spectra

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Volume 692 (December 2024)

A&A, 692 (2024) A43

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Table 2

Stellar, planetary, and orbital parameters adopted for the four ESPRESSO targets.

Parameter	HD 209458b	WASP-52b	WASP-76b	WASP-127b
Star
M_⋆ (M_⊙)	1.119 ± 0.033 ^(a)	0.87 ± 0.03 ^(g)	1.458 ± 0.021 ⁽ⁱ⁾	1.31 ± 0.05 ^(k)
R_⋆ (R_⊙)	1.155 ± 0.016 ^(a)	0.79 ± 0.02 ^(g)	1.756 ± 0.071 ⁽ⁱ⁾	1.33 ± 0.03 ^(k)
K_⋆ (m s⁻¹)	${84.27}_{- 0.70}^{+ 0.69}$ $\[84.27_{-0.70}^{+0.69}\]$ ^(b)	82.8 ± 2.1 ^(h)	${116.02}_{- 1.35}^{+ 1.29}$ $\[116.02_{-1.35}^{+1.29}\]$ ⁽ⁱ⁾	21.51 ± 2.78 ^(l)
T_eff (K)	$5996_{- 10}^{+ 20}$ $\[5996_{-10}^{+20}\]$	$5051_{- 29}^{+ 23}$ $\[5051_{-29}^{+23}\]$	$6220_{- 53}^{+ 47}$ $\[6220_{-53}^{+47}\]$	$5704_{- 11}^{+ 32}$ $\[5704_{-11}^{+32}\]$
log g (cm s⁻²)	4.237 ± 0.003	${4.525}_{- 0.007}^{+ 0.010}$ $\[4.525_{-0.007}^{+0.010}\]$	${4.007}_{- 0.037}^{+ 0.028}$ $\[4.007_{-0.037}^{+0.028}\]$	${4.230}_{- 0.003}^{+ 0.013}$ $\[4.230_{-0.003}^{+0.013}\]$
[Fe/H] (dex)	0.0 ± 0.2	0.28 ± 0.02	0.3 ± 0.2	−0.38 ± 0.05
A(Na) (dex)	6.21 ± 0.03	6.41 ± 0.03	6.79 ± 0.02	5.77 ± 0.06
[Na/Fe] (dex)	0.16 ± 0.03	−0.12 ± 0.03	0.38 ± 0.02	0.00 ± 0.06
v sin i_⋆ (km s⁻¹)	4.228 ± 0.007 ^(b)	2.622 ± 0.074 ^(h)	1.48 ± 0.28 ⁽ⁱ⁾	${0.53}_{- 0.05}^{+ 0.07}$ $\[0.53_{-0.05}^{+0.07}\]$ ^(m)
Planet
M_p (M_J)	0.685 ± 0.015 ^(a)	0.46 ± 0.02 ^(g)	${0.894}_{- 0.013}^{+ 0.014}$ $\[0.894_{-0.013}^{+0.014}\]$ ⁽ⁱ⁾	0.165 ± 0.021 ^(l)
R_p (R_J)	1.359 ± 0.019 ^(a)	1.27 ± 0.03 ^(g)	${1.854}_{- 0.076}^{+ 0.077}$ $\[1.854_{-0.076}^{+0.077}\]$ ⁽ⁱ⁾	1.311 ± 0.025 ^(l)
K_p (km s⁻¹)	145.0 ± 1.5	168.6 ± 1.9	198.4 ± 1.2	125.9 ± 3.5
i_p (deg)	86.78 ± 0.07 ^(c)	85.35 ± 0.20 ^(g)	${89.623}_{- 0.034}^{+ 0.005}$ $\[89.623_{-0.034}^{+0.005}\]$ ⁽ⁱ⁾	87.85 ± 0.35 ^(m)
λ (deg)	1.58 ± 0.08 ^(b)	1.1 ± 1.1 ^(h)	${61.28}_{- 5.06}^{+ 7.61}$ $\[61.28_{-5.06}^{+7.61}\]$ ⁽ⁱ⁾	$- {128.41}_{- 5.46}^{+ 5.60}$ $\[-128.41_{-5.46}^{+5.60}\]$ ^(m)
System
P_orb (days)	3.52474859 ± 0.00000038 ^(d)	1.7497798 ± 0.0000012 ^(g)	${1.80988198}_{- 0.00000056}^{+ 0.00000064}$ $\[1.80988198_{-0.00000056}^{+0.00000064}\]$ ⁽ⁱ⁾	4.17806203 ± 0.00000088 ^(l)
T_c (BJD)	2454560.80588 ± 0.00008 ^(c)	2455793.68143 ± 0.00009 ^(g)	${2458080.626165}_{- 0.000367}^{+ 0.000418}$ $\[2458080.626165_{-0.000367}^{+0.000418}\]$ ⁽ⁱ⁾	2456776.621238 ± 0.00023181 ^(l)
T₁₄ (days)	0.124 ± 0.002 ^(e)	0.0754 ± 0.0005 ^(g)	0.1564 ± 0.0005 ^(j)	0.18137185 ± 0.00035381 ^(l)
a (AU)	0.04707 ± 0.00047 ^(a)	0.0272 ± 0.0003 ^(g)	0.0330 ± 0.0002 ⁽ⁱ⁾	${0.04840}_{- 0.00095}^{+ 0.00136}$ $\[0.04840_{-0.00095}^{+0.00136}\]$ ^(l)
v_sys (km s⁻¹)	−14.741 ± 0.002 ^(f)	−0.8212 ± 0.0007 ^(h)	−1.11 ± 0.50 ⁽ⁱ⁾	−9.29546 ± 0.0014 ^(m)
		−0.8434 ± 0.0006 ^(h)
		−0.8357 ± 0.0006 ^(h)

Notes. M_⋆, R_⋆ and M_p, R_p are the mass and radius of the star and planet, respectively. K_⋆ is the semi-amplitude of the stellar RV signal, derived from ESPRESSO data. All values for the stellar effective temperature and surface gravity (T_eff, log g) were taken from the Gaia DR3 catalog. The metallicity values ([Fe/H]) are sourced from Gaia DR3, but the uncertainties were adjusted to account for the level of agreement or disagreement between the Gaia BP/RP and RVS values and those reported in the literature. The eccentricity was fixed to zero for all the systems. The two entries for the sodium abundance, A(Na) and [Na/Fe], were inferred by fitting the 3 D NLTE synthetic spectra to the Na D lines and the 6154/6160 Å lines, respectively (see Sect. 3). v sin i_⋆ is the stellar rotational velocity. K_p is the planet RV semi-amplitude (see Sect. 4.5). The inclination and projected obliquity of the orbit are i_p and λ, respectively. The other parameters represent the orbital period (P_orb), the time of conjunction (T_c), the transit duration (T₁₄), the semi-major axis (a), and the systemic velocity (v_sys) ^(a)Torres et al. (2008); ^(b)Casasayas-Barris et al. (2021); ^(c)Evans et al. (2015); ^(d)Knutson et al. (2007); ^(e)Richardson et al. (2006); ^(f)Naef et al. (2004); ^(g) Hébrard et al. (2013); ^(h) Chen et al. (2020); ⁽ⁱ⁾Ehrenreich et al. (2020); ^(j)Fu et al. (2021); ^(k)Lam et al. (2017); ^(l)Seidel et al. (2020); ^(m)Allart et al. (2020).

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