Revisiting the dynamical masses of the transiting planets in the young AU Mic system: Potential AU Mic b inflation at ~20 Myr

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Table 5

Comparison of activity models from the RV analysis of the AU Mic system using the difference between Bayesian log-evidences (∆ ln 𝒵).

	Activity model

	σ_jit			3 sin (P₁ P₂, P₃ ~4.9, 2.4, 1.6 d) + σ_jit			GP_QP + σ_jit

Planets	K^b (m s⁻¹)	K^c (m s⁻¹)	∆ ln 𝒵	K^b (m s⁻¹)	K^c (m s⁻¹)	∆ ln 𝒵	K^b (m s⁻¹)	K^c (m s⁻¹)	∆ ln 𝒵
0	…	…	−2660 2	…	…	−2522.0	…	…	−2226.5
2	${5.3}_{- 3.0}^{+ 3.3}$ $5.3_{ - 3.0}^{ + 3.3}$	${3.6}_{- 2.3}^{+ 2.8}$ $3.6_{ - 2.3}^{ + 2.8}$	−2662 7	${5.5}_{- 2.6}^{+ 2.7}$ $5.5_{ - 2.6}^{ + 2.7}$	${4.4}_{- 2.3}^{+ 2.2}$ $4.4_{ - 2.3}^{ + 2.2}$	−2543.5	$3 . 6_{- 1.1}^{+ 1.1}$ ${\bf{3}}.{\bf{6}}_{ - 1.1}^{ + 1.1}$	$4 . 3_{- 1.0}^{+ 1.0}$ ${\bf{4}}.{\bf{3}}_{ - 1.0}^{ + 1.0}$	−2218.9

Notes. In the model name, σ_jit refers to a jitter term added in quadrature to the RV error bars. All models assume circular orbits. The amplitudes are given with their 1σ uncertainty. ‘3 sin’ refers to three sinusoidal functions with their periods. The data used for the comparison are composed of the combination of RVs from CARMENES VIS, CARMENES NIR, HARPS, and SPIRou. The final adopted RV model in this paper is highlighted in bold.

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