A sub-Earth-mass planet orbiting Barnard’s star | Astronomy & Astrophysics (A&A)

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Volume 690 (October 2024)

A&A, 690 (2024) A79

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Table 3

Bayesian evidence of different models.

Name	Model	N_pl	N_par	ln $Z$ $\[\mathcal{Z}\]$	Δ ln $Z$ $\[\mathcal{Z}\]$
E18,E19 (N_point = 149 × 2)

A	GP	0	18	−449.3	−2.1
AD	GP	0	18	−466.5	−19.3
AL	GP	0	18	−452.3	−5.1
AT	GP	0	18	−450.5	−3.3
C1c	A+lpcLU50	1	21	−443.7	+3.5
C1e	A+lpeLU50	1	23	−445.5	+1.7
D	A+cycN	0	26	−447.2	0.0
DD	AD+cycN	0	26	−463.8	−16.6
DL	AL+cycN	0	26	−453.6	−6.4
DT	AT+cycN	0	26	−448.2	−1.0
E1c	D+1pcLU50	1	29	−439.5	+7.7
E1cT	DT+1pcLU50	1	29	−440.7	+6.5
E1e	D+1peLU50	1	31	−438.6	+8.6
E1eD	DD+1peLU50	1	31	−460.1	−12.9
E1eL	DL+1peLU50	1	31	−446.7	+0.5
E1eT	DT+1peLU50	1	31	−442.2	+5.0
E12c	D+1pcLU20	1	29	−440.5	+6.7
E12e	D+lpeLU20	1	31	−440.2	+7.0
E22c	D+2pcLU20	2	32	−443.8	+3.4
E22e	D+2peLU20	2	36	−443.6	+3.6

E18, E19, H15, HAN (N_point = 298 × 2)

I1	GP+cycU	0	35	−1074.1	0.0
I2	GP+cycN	0	35	−1073.1	+1
J1	I1+1peLU50	1	40	−1061.7	+12.4
J2	I2+2peLU50	2	45	−1063.9	+10.2

E18, E19, H15, HAN, CAR (N_point = 792 × 2)

K1	GP+cycU	0	39	−4123.0	0.0
K2	GP+cycN	0	39	−4122.0	+1.0
L1	Kl+1peLU50	1	44	−4110.7	+12.3
L2	K2+1peLU50	1	44	−4109.9	+13.1
M2	K2+2peLU20	2	49	−4108.8	+14.2

Notes. Model selection based on Bayesian evidence of the analysis of CCF FWHM and TM RV measurements. A, AD, and AL are models for ESPRESSO TM, DRS, and LBL RVs, respectively. Models with T are for TMtc RVs computed using telluric-corrected ESPRESSO spectra (see Section 2.1). Different models: cyc indicates cycle, and N, U, and LU indicate normal, uniform, and log-uniform priors. LUx indicates priors $L$ $\[\mathcal{L}\]$ $U$ $\[\mathcal{U}\]$ (0.5, x) with x = 20 and 50 d. npe and npc indicate n Keplerian and circular orbits. We highlight in bold font the reference activity-only model in each group of datasets.

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