Table 2
Main characteristics of RV datasets analysed in this work.
| Spectrograph | λ range | NRV(a) | rmsRV | Median σRV | NRV/Prot T(b) | TAC(c) | Pipeline |
|---|---|---|---|---|---|---|---|
| (nm) | (m s−1) | (m s−1) | |||||
| CARMENES VIS | 520–960 | 88 (86) | 93.7 | 7.8 | 3.1 | Yes | serval(c) |
| CARMENES NIR | 960–1710 | 89 (87) | 84.9 | 23.4 | 3.1 | Yes | serval(c) |
| HARPS | 380–690 | 122 (117) | 148.6 | 3.2 | 3.0 | No | serval(d) |
| HIRES | 480–600 | 40 | 130.9 | 2.6 | 1.1 | No | Howard et al. (2010) |
| iSHELL | 2180–2470 | 28 | 39.6 | 4.8 | 1.0 | Yes | pychell(e) |
| SPIRou | 950–2350 | 179 (176) | 32.5 | 3.8 | 2.1 | Yes | LBL(f) |
| TRES | 390–910 | 43 | 106.0 | 22.6 | 1.5 | No | Fürész (2008) |
| Full dataset | … | 478 (466) | … | … | 3.9 | … | … |
Notes. (a)Total numbers of RV epochs. The number of RV epochs used in the final analysis is provided in parentheses. (b)Number of RV epochs used in the final analysis per stellar rotation period and per total time range. The instruments used to derive the planetary parameters of the system are represented in bold face.(c)Telluric absorption corrected.(d)Zechmeister et al. (2018).(e)Cale et al. (2019).(f)Artigau et al. (2022).
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