Monitoring the magnetospheric accretion of the classical T Tauri star DO Tau with SPIRou

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Table 4

MCMC results of the modeling of LBL RVs.

Parameter	No planet	Planet b	Prior
θ₁ (kms⁻¹)	${0.50}_{- 0.10}^{+ 0.13}$ $Mathematical equation: $0.50^{+0.13}_{-0.10}$$	${0.53}_{- 0.11}^{+ 0.13}$ $Mathematical equation: $0.53^{+0.13}_{-0.11}$$	Mod Jeffreys (σ_RV)
θ₂ (d)	5.129 ± 0.003	5.130 ± 0.003	Gaussian (5.1; 0.3)
θ₃ (d)	600	600	Fixed
θ₄	0.7	0.7	Fixed
θ₅ (kms⁻¹)	0.21 ± 0.04	0.13 ± 0.04	Mod Jeffreys (σ_RV)
K_b (kms⁻¹)		0.22 ± 0.04	Mod Jeffreys (σ_RV)
P_b (d)		21.14 ± 0.02	Gaussian (21.1; 0.2)
T_b (2459000+)		1318.1 ± 0.6	Gaussian (1318; 5)
M_b sin i (M_♃ )		2.0 ± 0.4	From K_b, P_b, M_*
M_b (M_♃ )		2.8 ± 0.6	Assuming i = 45°
a_b (au)		0.12 ± 0.01
$χ_{r}^{2}$ $Mathematical equation: $\chi^2_{\rm r}$$	1.71	1.07
rms (km s⁻¹ )	0.26	0.21
log L_M	−28.1	−14.8
∆ log L_M	0.0	13.3

Notes. We list the recovered GP and candidate planet parameters with their error bars, as well as the priors used where relevant, for the model without planet (Column 2) and the best model with a candidate planet at 21.14 d (Column 3). The last four rows report the $χ_{r}^{2}$ $Mathematical equation: $\chi^2_{\rm r}$$ , the rms of the best fit to the RV data, the associated marginal logarithmic likelihood, log L_M, and the marginal logarithmic likelihood variation, ∆ log L_M, relative to the case without planet.

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