The ESPRESSO transmission spectrum of HD189733 b - Extracting the planetary sodium and lithium signatures amid stellar contamination

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Volume 700 (August 2025)

A&A, 700 (2025) A41

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Table 2

Physical and orbital parameters of the system HD 189733.

Parameter	Symbol [Unit]	Value
Stellar Parameters
Stellar mass	M_★ [M_⊙]	0.783 ± 0.0041
Stellar radius	R_★ [R_⊙]	0.784 ± 0.007
Effective temperature	T_eff [K]	4969 ± 43
Metallicity	[Fe/H] [dex]	-0.07 ± 0.02
Surface gravity	log g_★ [cgs]	4.51 ± 0.03
Limb darkening coefficient	u₁	0.6617
Limb darkening coefficient	u₂	-0.3940
Limb darkening coefficient	u₃	1.0507
Limb darkening coefficient	u₄	-0.4533
– Planetary Parameters –
Planet mass	M_p [M_J]	1.123 ± 0.045
Planet radius	R_p [R_J]	1.187 ± 0.011
– System Parameters –
Transit epoch	T_c [BJD_TDB]	2459446.498519
		$_{- 0.000013}^{+ 0.000012}$ $^{+0.000012}_{-0.000013}$
Orbital period	P [d]	2.2185751979
		$_{- 0.0000000728}^{+ 0.0000000698}$ $^{+0.0000000698}_{-0.0000000728}$
Transit duration (P₁ to P₄)	T₁₄ [h]	1.806 ± 0.033
Transit duration (P₂ to P₃)	T₂₃ [h]	0.992 ± 0.037
Planet-to-star radius ratio	R_p/R_★	0.15565 $_{- 0.00021}^{+ 0.00024}$ $^{+0.00024}_{-0.00021}$
Orbital semi-major axis	a [R_★]	8.8843 $_{- 0.0177}^{+ 0.0173}$ $^{+0.0173}_{-0.0177}$
Orbit inclination	i [deg]	85.705 ± 0.016
Eccentricity	e	0 (fixed)
Stellar RV semi-amplitude	K_★ [m s⁻¹]	201.3 ± 1.6
Planet RV semi-amplitude	K_p [km s⁻¹]	150.038 ± 2.619
Systemic velocity (Night 1)	γ₁ [km s⁻¹]	-2.2203 ± 0.0004
Systemic velocity (Night 2)	γ₂ [km s⁻¹]	-2.2290 ± 0.0005
– Rossiter-McLaughlin Parameters –
Projected spin-orbit angle	λ [deg]	-0.81 ± 0.07
Star rotational velocity	v_eq [km s⁻¹]	3.65 $_{- 0.27}^{+ 0.25}$ $^{+0.25}_{-0.27}$
Stellar inclination	i_★ [deg]	91.2 $_{- 6.7}^{+ 4.5}$ $^{+4.5}_{-6.7}$
Convective blueshift velocity	v_CB [m s⁻¹]	-174 $_{- 33}^{+ 37}$ $^{+37}_{-33}$
Differential rotation coefficient	α_rot	0.32 $_{- 0.22}^{+ 0.14}$ $^{+0.14}_{-0.22}$

Notes. All parameters were taken or derived from Krenn et al. (2023), except for K_★, M_p (from Bonomo et al. 2017), the limb darkening coefficients (derived from Pont et al. 2013), the RM parameters, and the systemic velocities, which were derived from our analysis described in Sect. 3.

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