The GAPS Programme at TNG - LIX. Characterisation study of the ∼300 Myr-old multi-planetary system orbiting the star BD+40 2790 (TOI-2076)

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Volume 690 (October 2024)

A&A, 690 (2024) A235

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Table 4

Best-fit values of the free parameters of the model that includes a multi-dimensional GP regression, using the activity diagnostic BIS and the HARPS-N RVs calculated with SERVAL for the wavelength range no. 3 (see Table 1).

Parameter	Best-fit value^(a)
Multi-dimensional GP parameters:
A_RV^(b) (m/s)	${3.3}_{- 1.4}^{+ 1.8}$ $3.3_{ - 1.4}^{ + 1.8}$
B_RV (m/s)	${31.4}_{- 2.8}^{+ 3.3}$ $31.4_{ - 2.8}^{ + 3.3}$
A_BIS (m/s)	${2.5}_{- 1.5}^{+ 1.6}$ $2.5_{ - 1.5}^{ + 1.6}$
B_BIS (m/s)	$- {33.5}_{- 1.5}^{+ 1.6}$ $- 33.5_{ - 1.5}^{ + 1.6}$
λ (d)	${28.1}_{- 1.5}^{+ 1.7}$ ${28.1_{ - 1.5}^{ + 1.7}}$
w	${0.46}_{- 0.02}^{+ 0.03}$ ${0.46_{ - 0.02}^{ + 0.03}}$
θ (d)	7.33 ± 0.01
Planet-related parameters:
K_b (ms⁻¹)	1.1 ± 0.6
Orbital period, P_b (d)	10.35523 ± 0.00001
T_{con j,b} (BJD-2450000)	8950.8289 ± 0.0005
Semi-major axis ^(c), a_b (au)	0.0880 ± 0.0009
Mass, m_b (M_⊕)	3.4 ± 1.8 (<9.0, 3σ)
Bulk density, ρ_b (g/cm⁻³)	${1.2}_{- 0.6}^{+ 0.7}$ $1.2_{ - 0.6}^{ + 0.7}$
K_c (m s⁻¹)	1.2 ± 0.6
Orbital period, P_c (d)	21.01549 ± 0.00003
T_{con i.c} (BJD-2450000)	8937.8283 ± 0.0007
Semi-major axis ^(c), a_c (au)	${0.1411}_{- 0.0014}^{+ 0.0015}$ $0.1411_{ - 0.0014}^{ + 0.0015}$
Mass, m_c (M_⊕)	4.6 ± 2.3 (<11.8, 3σ)
Bulk density, ρ_c (g/cm⁻³)	${0.7}_{- 0.3}^{+ 0.4}$ $0.7_{ - 0.3}^{ + 0.4}$
K_d (ms⁻¹)	1.6 ± 0.6
Orbital period, P_d (d)	35.12551 ± 0.00007
T_{con j, d} (BJD-2450000)	8938.296 ± 0.001
Semi-major axis ^(c), a_d (au)	${0.1988}_{- 0.0020}^{+ 0.0021}$ $0.1988_{ - 0.0020}^{ + 0.0021}$
Mass, m_d (M_⊕)	7.3 ± 2.8 (<14.8, 3σ)
Bulk density, ρ_d (g/cm⁻³)	${1.1}_{- 0.4}^{+ 0.5}$ $1.1_{ - 0.4}^{ + 0.5}$
Acceleration, $\dot{γ}$ ${\dot \gamma }$ (m s⁻¹d⁻¹)	$- {0.0072}_{- 0.0025}^{+ 0.0029}$ $- 0.0072_{ - 0.0025}^{ + 0.0029}$
RV and BIS-related parameters
σ_{jit Rv, HSRPS–N} (ms⁻¹)	${3.9}_{- 0.9}^{+ 0.8}$ $3.9_{ - 0.9}^{ + 0.8}$
γ_{Rv, HARPS–N} (ms⁻¹)	2.8 ± 0.8
σ_{jit BIS, HARPS–N} (m s⁻¹)	16.2 ± 0.8
γ_{BIS, HARPS–N} (m s⁻¹)	20.8 ± 1 .2

Notes. ^(a)The uncertainties are given as the 16^th and 84^th percentiles of the posterior distributions. For some of the parameters, we provide the 95^th percentile in parenthesis. ^(b)The posteriors for A_RV, B_RV, A_BIS, and B_BIS are bimodal. A_RV and B_RV are positively correlated, and we have selected values >0 to calculate the percentiles. A_BIS and B_BIS are anti-correlated, and we have selected positive values for A_BIS and negative values for B_BIS to calculate their percentiles. ^(c)We note that our derived semi-major axis values are larger than those reported by Hedges et al. (2021); Osborn et al. (2022), and Zhang et al. (2023); Gaidos et al. (2023) for planet b.

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