Table 1
Planetary systems identified around stars from all three surveys.
| HIP | M* | log ɡ | L* | [Fe/H] | evol. | MP sin(i) | P | KRV | a | e | fR | fC | Detection reference |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) | (cm s–2) | (L⊙) | (dex) | stage | (MJup) | (d) | (m s–1) | (AU) | (%) | (%) | |||
| 5364 | 1.4 ± 0.2 | 2.3 ± 0.1 | 74.2±1.0 | 0.07 ± 0.10 | HB | 2.3 ± 0.1 | 405.4±0.7 | 49.8 ± 2.4 | 1.2 ± 0.1 | 0.06 ± 0.03 | 100 | 66 | Trifonov et al. (2014) |
| 3.0 ± 0.1 | 751.9 ± 3.3 | 54.1 ± 2.4 | 1.8 ± 0.1 | 0.14 ± 0.05 | 100 | 66 | Trifonov et al. (2014) | ||||||
| 8541 | 1.0 ± 0.1 | 2.8 ± 0.1 | 21.0 ± 2.9 | –0.15 ± 0.08 | RGB | 4.6 ± 0.2 | 1563.7 ± 18.5 | 83.8 ± 3.6 | 2.6 ± 0.1 | 0.13 ± 0.04 | 100 | 72 | Jones et al. (2016) |
| 16335 | 1.5 ± 0.2 | 1.5 ± 0.1 | 357.6 ± 15.2 | –0.20 ± 0.10 | RGB | 7.0 ± 0.5 | 574.7 ± 3.2 | 129.8±8.6 | 1.6 ± 0.1 | 0.18 ± 0.07 | 100 | 94 | Lee et al. (2014b) |
| 19011 | 2.1 ± 0.6 | 2.5 ± 0.1 | 88.0 ± 6.1 | –0.03 ± 0.10 | HB | 2.4 ± 0.1 | 456.8±1.2 | 38.8 ± 2.3 | 1.5 ± 0.2 | 0.09 ± 0.05 | 100 | 68 | Tala Pinto et al. (2020) |
| 20889 | 2.5 ± 0.3 | 2.7 ± 0.1 | 84.3±1.6 | 0.05 ± 0.10 | HB | 7.0 ± 0.2 | 581.8 ± 2.1 | 93.4 ± 2.4 | 1.8 ± 0.1 | 0.09 ± 0.03 | 100 | 94 | Sato et al. (2007) |
| 24275 | 1.4 ± 0.1 | 3.2 ± 0.1 | 11.3±1.3 | 0.17 ± 0.10 | RGB | 1.7 ± 0.2 | 555.4 ± 7.1 | 34.5 ± 2.9 | 1.5 ± 0.1 | 0.14 ± 0.05 | 100 | 44 | Wittenmyer et al. (2016b) |
| 1.5 ± 0.2 | 851.7 ± 31.8 | 26.7 ± 4.2 | 2.0 ± 0.1 | 0.00 ± 0.07 | 100 | 29 | Wittenmyer et al. (2016b) | ||||||
| 31592 | 1.4 ± 0.2 | 3.2 ± 0.1 | 11.6 ± 0.3 | 0.21 ± 0.10 | RGB | 1.9 ± 0.1 | 744.1 ± 3.6 | 34.7 ± 1.3 | 1.8 ± 0.1 | 0.18 ± 0.05 | 100 | 41 | Wittenmyer et al. (2011a) |
| 0.8 ± 0.1 | 1027.4 ± 15.8 | 13.0±1.3 | 2.2 ± 0.1 | 0.16 ± 0.09 | 100 | 8 | Luque et al. (2019) | ||||||
| 34693 | 2.5 ± 0.2 | 2.0 ± 0.1 | 229.5 ± 9.0 | 0.14 ± 0.10 | HB | 21.3 ± 0.2 | 305.5 ± 0.1 | 350.2 ± 3.1 | 1.2 ± 0.1 | 0.03 ± 0.01 | 100 | 99 | Mitchell et al. (2013) |
| 36616 | 1.7 ± 0.5 | 2.6 ± 0.2 | 72.8 ± 3.0 | 0.15 ± 0.10 | HB | 6.4 ± 0.2 | 299.4 ± 0.2 | 136.9 ± 2.9 | 1.0 ± 0.2 | 0.00 ± 0.02 | 100 | 96 | Ortiz et al. (2016) |
| 37826 | 2.1 ± 0.2 | 2.9 ± 0.1 | 39.2 ± 0.2 | 0.07 ± 0.10 | HB | 3.1 ± 0.1 | 598.2±1.3 | 46.1 ± 1.4 | 1.8 ± 0.1 | 0.06 ± 0.03 | 100 | 76 | Hatzes et al. (2006); Reffert et al. (2006) |
| 39177 | 2.9 ± 0.4 | 1.7 ± 0.1 | 478.8 ± 97.9 | 0.06 ± 0.10 | HB | 20.8 ± 1.0 | 853.6 ± 4.4 | 216.7 ± 9.8 | 2.5 ± 0.1 | 0.05 ± 0.04 | 100 | 98 | Tala Pinto et al. (2020) |
| 43803 | 1.1 ± 0.1 | 2.7 ± 0.1 | 30.2 ± 0.4 | -0.11 ± 0.10 | RGB | 3.9 ± 0.3 | 416.3 ± 0.3 | 175.8 ± 13.2 | 1.1 ± 0.1 | 0.83 ± 0.02 | 100 | 87 | Wittenmyer et al. (2017a) |
| 49129 | 1.2 ± 0.6 | 2.4 ± 0.3 | 53.2±1.1 | 0.04 ± 0.10 | HB | 2.9 ± 0.3 | 1268.1 ± 35.5 | 49.8 ± 5.2 | 2.4 ± 0.5 | 0.17 ± 0.08 | 100 | 54 | Wittenmyer et al. (2017b) |
| 56640 | 1.0 ± 0.1 | 3.1 ± 0.1 | 9.8±1.2 | 0.09 ± 0.09 | RGB | 3.7 ± 0.1 | 2596.8±81.8 | 53.8 ± 2.2 | 3.7 ± 0.2 | 0.15 ± 0.05 | 100 | 41 | Jones et al. (2021) |
| 60202 | 1.9 ± 0.2 | 2.3 ± 0.1 | 114.7 ± 4.2 | -0.24 ± 0.10 | HB | 15.2 ± 0.4 | 323.6 ± 0.8 | 302.1 ± 8.0 | 1.1 ± 0.1 | 0.25 ± 0.02 | 100 | 99 | Liu et al. (2008) |
| 63242 | 1.1 ± 0.1 | 2.6 ± 0.1 | 31.7 ± 3.0 | -0.31 ± 0.09 | RGB | 6.4 ± 0.2 | 125.9 ± 0.1 | 248.0 ± 7.8 | 0.5 ± 0.1 | 0.05 ± 0.03 | 100 | 98 | Jones et al. (2013) |
| 65891 | 1.9 ± 0.1 | 2.9 ± 0.1 | 36.2 ± 3.6 | 0.16 ± 0.10 | HB | 5.9 ± 0.2 | 1108.5 ± 17.9 | 74.5 ± 2.8 | 2.6 ± 0.1 | 0.04 ± 0.03 | 100 | 86 | Jones et al. (2015b) |
| 67537 | 1.9 ± 0.1 | 2.9 ± 0.1 | 34.8 ± 1.6 | 0.15 ± 0.08 | HB | 8.5 ± 0.7 | 2390.6 ± 305.0 | 107.8 ± 6.7 | 4.3 ± 0.4 | 0.64 ± 0.07 | 98 | 79 | Jones et al. (2017) |
| 67851 | 1.3 ± 0.2 | 3.1 ± 0.1 | 14.0 ± 0.6 | 0.00 ± 0.10 | RGB | 1.2 ± 0.1 | 89.0 ± 0.1 | 44.9 ± 2.0 | 0.4 ± 0.1 | 0.13 ± 0.04 | 100 | 63 | Jones et al. (2015a) |
| 4.8 ± 0.3 | 2123.1 ± 127.6 | 62.6 ± 3.3 | 3.5 ± 0.2 | 0.03 ± 0.05 | 100 | 64 | Wittenmyer et al. (2015) | ||||||
| 74890 | 1.4 ± 0.2 | 3.2 ± 0.1 | 12.0±1.0 | 0.20 ± 0.13 | RGB | 2.1 ± 0.1 | 827.1 ± 14.9 | 38.0 ± 1.9 | 1.9 ± 0.1 | 0.13 ± 0.05 | 100 | 46 | Jones et al. (2016) |
| 75092 | 1.2 ± 0.1 | 3.3 ± 0.1 | 8.0 ± 0.8 | 0.09 ± 0.11 | RGB | 1.5 ± 0.1 | 1048.9 ± 38.0 | 29.5 ± 2.4 | 2.1 ± 0.1 | 0.35 ± 0.08 | 100 | 26 | Jones et al. (2021) |
| 75458 | 1.3 ± 0.2 | 2.4 ± 0.1 | 57.2 ± 0.8 | 0.11 ± 0.10 | HB | 10.0 ± 0.1 | 511.0 ± 0.0 | 307.6 ± 2.0 | 1.4 ± 0.1 | 0.72 ± 0.00 | 100 | 98 | Frink et al. (2002) |
| 79540 | 1.2 ± 0.1 | 1.7 ± 0.1 | 179.6 ± 11.1 | -0.01 ± 0.10 | RGB | 4.3 ± 0.2 | 578.2±1.9 | 91.5 ± 4.2 | 1.4 ± 0.1 | 0.05 ± 0.04 | 100 | 87 | Tala Pinto et al. (2020) |
| 84056 | 1.3 ± 0.1 | 3.2 ± 0.1 | 10.1 ± 0.7 | 0.08 ± 0.07 | RGB | 1.8 ± 0.2 | 877.0 ± 19.9 | 33.6 ± 2.9 | 1.9 ± 0.1 | 0.09 ± 0.07 | 100 | 36 | Wittenmyer et al. (2016a) |
| 88048 | 2.7 ± 0.1 | 2.6 ± 0.1 | 107.0 ± 2.3 | 0.06 ± 0.10 | HB | 22.4 ± 0.1 | 530.0 ± 0.1 | 288.5±1.1 | 1.8 ± 0.1 | 0.13 ± 0.00 | 100 | 99 | Quirrenbach (2011) |
| 24.4 ± 0.4 | 3168.1 ± 28.7 | 174.4 ± 2.2 | 5.9 ± 0.1 | 0.19 ± 0.01 | 100 | 84 | Quirrenbach (2011) | ||||||
| 90988 | 1.4 ± 0.2 | 3.3 ± 0.1 | 8.6±1.1 | 0.24 ± 0.14 | RGB | 2.2 ± 0.1 | 455.3 ± 3.2 | 49.3 ± 2.7 | 1.3 ± 0.1 | 0.17 ± 0.05 | 100 | 63 | Jones et al. (2021) |
| 95124 | 1.4 ± 0.1 | 3.3 ± 0.1 | 10.6±1.0 | 0.20 ± 0.08 | RGB | 2.3 ± 0.1 | 566.8 ± 5.3 | 44.7 ± 2.4 | 1.5 ± 0.1 | 0.08 ± 0.06 | 100 | 62 | Jones et al. (2016) |
| 105854 | 1.9 ± 0.1 | 2.8 ± 0.1 | 36.9±1.6 | 0.31 ± 0.18 | HB | 7.5 ± 0.3 | 184.9 ± 0.4 | 174.3 ± 6.0 | 0.8 ± 0.1 | 0.04 ± 0.03 | 100 | 98 | Jones et al. (2014) |
| 107773 | 1.7 ± 0.4 | 2.6 ± 0.2 | 58.8 ± 4.4 | 0.03 ± 0.10 | HB | 1.5 ± 0.1 | 144.0 ± 0.4 | 42.1 ± 2.7 | 0.6 ± 0.1 | 0.11 ± 0.05 | 100 | 68 | Jones et al. (2015b) |
| 114855 | 1.1 ± 0.1 | 2.4 ± 0.1 | 50.7±1.0 | –0.03 ± 0.10 | HB | 2.7 ± 0.1 | 181.4 ± 0.1 | 91.6 ± 2.3 | 0.6 ± 0.1 | 0.03 ± 0.02 | 100 | 87 | Mitchell et al. (2013) |
| 114933 | 1.3 ± 0.1 | 3.3 ± 0.1 | 8.9±1.1 | 0.14 ± 0.08 | RGB | 2.1 ± 0.2 | 1502.5 ± 29.2 | 31.4 ± 4.0 | 2.8 ± 0.1 | 0.26 ± 0.09 | 100 | 32 | Jones et al. (2021) |
| 116630 | 1.2 ± 0.2 | 3.4 ± 0.1 | 6.8 ± 0.5 | 0.16 ± 0.14 | RGB | 1.8 ± 0.1 | 876.8 ± 14.3 | 33.1 ± 2.4 | 1.9 ± 0.1 | 0.09 ± 0.05 | 100 | 36 | Wittenmyer et al. (2017b) |
| 11791 | 1.9 ± 0.2 | 2.8 ± 0.1 | 45.3 ± 3.5 | 0.01 ± 0.08 | HB | 3.0 | 691.9 ± 3.6 | 38.3 ± 2.0 | 2.1 | 0.12 ± 0.05 | Sato et al. (2012) | ||
| 31674 | 1.4 ± 0.2 | 2.9 ± 0.1 | 28.2 ± 0.4 | –0.07 ± 0.10 | RGB | 1.8 ± 0.2 | 363.3 ± 2.5 | 33.6 ± 3.2 | 1.2 ± 0.1 | 0.09 ± 0.07 | Sato et al. (2016) | ||
| 1.9 ± 0.2 | 684.7 ± 5.0 | 30.1 ± 2.0 | 1.9 ± 0.1 | 0.28±0.08 | Sato et al. (2016) | ||||||||
| 40526 | 1.5 ± 0.2 | 1.2 ± 0.1 | 632.5 ± 17.2 | –0.19 ± 0.10 | RGB | 7.8 ± 0.8 | 605.2 ± 4.0 | 133.0 ± 8.8 | 1.7 ± 0.1 | 0.08±0.02 | Lee et al. (2014a) | ||
| 53261 | 2.2 ± 0.4 | 1.5 ± 0.1 | 569.6 ± 56.3 | –0.21 ± 0.10 | HB | 12.1 ± 0.6 | 785.7 ± 4.8 | 158.7 ± 8.6 | 2.2 ± 0.1 | 0.11 ± 0.06 | Tala Pinto et al. (2020) | ||
| 107089 | 1.4 ± 0.1 | 3.2 ± 0.1 | 13.3 ± 0.3 | 0.08 ± 0.10 | RGB | 2.1 ± 0.1 | 414.8 ± 3.1 | 38.7 ± 1.1 | 1.3 ± 0.1 | 0.09 ± 0.04 | Ramm et al. (2009, 2016) | ||
| 108513 | 1.4 ± 0.1 | 3.2 ± 0.1 | 12.6 ± 0.2 | 0.13 ± 0.10 | RGB | 1.4 ± 0.1 | 352.7 ± 1.7 | 34.7 ± 2.2 | 1.0 ± 0.1 | 0.07 ± 0.06 | Yılmaz et al. (2017) | ||
| 9884 | 1.6 ± 0.3 | 2.3 ± 0.1 | 81.2 ± 1.0 | –0.13 ± 0.10 | RGB | 1.8 ± 0.2 | 380.8 ± 0.3 | 41.1 ± 0.8 | 1.2 | 0.25 ± 0.03 | Lee et al. (2011) | ||
| 41704 | 2.7 ± 0.1 | 2.5 ± 0.1 | 138.1 ± 2.1 | –0.16 ± 0.10 | HB | 4.1 | 1630.0 ± 35.0 | 33.6 ± 2.1 | 3.9 | 0.13 ± 0.06 | Sato et al. (2012) | ||
| 48455 | 1.5 ± 0.1 | 2.5 ± 0.1 | 51.5 ± 0.7 | 0.29 ± 0.10 | HB | 2.4 ± 0.4 | 357.8 ± 1.2 | 52.0 ± 5.4 | 1.1 ± 0.1 | 0.09 ± 0.06 | Lee et al. (2014a) | ||
| 70791 | 1.0 ± 0.1 | 2.4 ± 0.1 | 60.8 ± 2.2 | –0.70 ± 0.10 | HB | 0.9 ± 0.1 | 30.4 ± 0.1 | 59.9 ± 3.2 | 0.2 ± 0.1 | 0.04 ± 0.04 | Takarada et al. (2018) | ||
Notes. The 37 systems in the first block will be considered for the analysis. The host stars of the second block are removed by our cuts (#RVs ≤ 10 or - in the cases of HIP 40526 and HIP 53261 - log(ɡ) ≤ 1.5). For the four stars in the third block, our data do not allow for detection with comparable confidence to the systems in the first block; they are hence excluded from the analysis (this includes the outer planet in the multiple system around HIP 19011). The stellar parameters are derived with the method of Stock et al. (2018). For the first block, we quote the orbital parameters as determined from our RV data with RVLIN (Wright & Howard 2009), and the completeness fraction fc and recovery rate fR used for the incompleteness corrections (see Sect. 6). Uncertainties on the orbital parameters are determined via bootstrapping using the BOOTTRAN package (Wang et al. 2012). For completeness, we also list the orbital parameters of the planets in the second and third block as given in their respective reference. For simplicity, asymmetric uncertainties were averaged into a single error estimate.
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