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 6

Comparison between Keplerian model with two planets and Keplerian model with three planets.

Planets	K^b (m s⁻¹)	K^c (m s⁻¹)	K^d (m s⁻¹)	∆ ln 𝒵
2	${3.6}_{- 1.1}^{+ 1.1}$ ${3.6_{ - 1.1}^{ + 1.1}}$	${4.3}_{- 1.0}^{+ 1.0}$ ${4.3_{ - 1.0}^{ + 1.0}}$	…	−2218.4
3	${3.5}_{- 1.1}^{+ 1.1}$ ${3.5_{ - 1.1}^{ + 1.1}}$	${4.2}_{- 1.0}^{+ 1.0}$ ${4.2_{ - 1.0}^{ + 1.0}}$	${0.7}_{- 0.5}^{+ 0.8} (3.1)$ $0.7_{ - 0.5}^{ + 0.8}(3.1)$	−2222.1

Notes. The 99.7th percentile of the Keplerian amplitude for the AU Mic ‘d’ candidate is provided in parentheses. The activity model used for this comparison was the GP model.

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