Table 4
Priors used for modelling the HIRES, HARPS, and CARMENES VIS radial velocities.
| Parameter | Prior |
|---|---|
| Stellar activity – QP kernel | |
| h (m s−1) | U(0,10)(a) |
| θ (d) | U(20,50) |
| λQP (d) | U(0,1000) |
| w | U(0,1) |
| Stellar activity – QPC kernel | |
| h1 (m s−1) | U(0,10)(a) |
| h2 ( m s−1) | U(0,10)(a) |
| θ(d) | U(20,50) |
| λQPC (d) | U(0,1000) |
| w | U(0,1) |
| Stellar activity – dSHO kernel | |
| log A | U(0.05,10)(a) |
| θ(d) | U(20,50) |
| log Q0 | U(−10,10) |
| log ∆Q | U(−10,10) |
| f | U(0,10) |
| First Keplerian | |
| Kb (m s−1) | U(0,5) |
| Pb (d) | U(0,200)(b) |
| U(100,200)(c) | |
| Tconj, b (BJD-2450000) | U(8500,8750) |
 |
U(−1,1) |
 |
U(−1,1) |
| Second Keplerian (innermost) | |
| Kc (m s−1) | U(0,5) |
| Pc (d) | U(0,100) |
| Tconj, c (BJD-2450000) | U(8500,8650) |
 |
U(−1,1) |
 |
U(−1,1) |
| Third Keplerian (outermost)(d) | |
| Kd (m s−1) | U(0,5) |
| Pd (d) | U(200,4350) |
| Tconj, d (BJD-2450000) | U(4500,9000) |
 |
U(−1,1) |
 |
U(−1,1) |
| Additional sinusoid(e) | |
| K365–d (ms−1) | U(0,10) |
| P365-d (d) | U(340,370) |
| T0,365–d (BJD-2 450000) | U(8500,8900) |
| Instrument-related | |
| γ (m s−1) | U(−20,20)(a) |
| σjit (m s−1) | U(0,10)(a) |
Notes. (a)The same prior was used for the corresponding parameter related to HIRES, HARPS (pre- and post-2015), and CARMENES-VIS data. (b)Prior used when modelling only one Keplerian. (c)Prior used when including a second Keplerian to model planetary signals with P < 200 days. (d)Priors for a planetary signal with period longer than 200 days, which we modelled combining HIRES+HARPS+CARMENES RVs. (e)Priors used to model the yearly signal only seen in the CARMENES-VIS RVs.
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