Table B.9
Occurrence rates of giant planets for different ranges of orbital periods from different studies. All values are in percent.
| Orbital periods | 0.8 d | 2.0 d | 3.4 d | 5.9 d | 10 d | 17 d | 29 d | 50 d | 85 d | 145 d | 245 d |
| – | – | – | – | – | – | – | – | – | – | – | |
| 2.0 d | 3.4 d | 5.9 d | 10 d | 17 d | 29 d | 50 d | 85 d | 145 d | 245 d | 400 d | |
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| This work | 0.051 | 0.10 | 0.21 | 0.11 | 0.025 | 0.23 | 0.16 | 0.49 | 1.05 | 0.88 | 1.27 |
| ±0.023 | ±0.03 | ±0.06 | ±0.05 | ±0.017 | ±0.11 | ±0.09 | ±0.22 | ±0.35 | ±0.36 | ±0.63 | |
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| Fressin et al. (2013) | 0.015 | 0.067 | 0.17 | 0.18 | 0.27 | 0.23 | 0.35 | 0.71 | 1.25 | 0.94 | 1.05 |
| ±0.007 | ±0.018 | ±0.03 | ±0.04 | ±0.06 | ±0.06 | ±0.10 | ±0.17 | ±0.29 | ±0.28 | ±0.30 | |
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| Mayor et al. (2016) | – | 0.26 | 0.28 | 0.29 | 0.17 | 0.39 | 0.12 | 0.96 | 0.70 | 0.83 | 1.36 |
| – | ±0.19 | ±0.20 | ±0.20 | ±0.17 | ±0.28 | ±0.12 | ±0.43 | ±0.35 | ±0.42 | ±0.48 | |
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| Orbital periods | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d | 0.8 d |
| – | – | – | – | – | – | – | – | – | – | – | |
| 2.0 d | 3.4 d | 5.9 d | 10 d | 17 d | 29 d | 50 d | 85 d | 145 d | 245 d | 400 d | |
|
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| This work | 0.051 | 0.15 | 0.36 | 0.47 | 0.49 | 0.72 | 0.88 | 1.36 | 2.41 | 3.29 | 4.55 |
| ±0.023 | ±0.04 | ±0.07 | ±0.08 | ±0.09 | ±0.12 | ±0.14 | ±0.21 | ±0.33 | ±0.43 | ±0.57 | |
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| Fressin et al. (2013) | 0.015 | 0.08 | 0.25 | 0.43 | 0.70 | 0.93 | 1.29 | 2.00 | 3.24 | 4.19 | 5.24 |
| ±0.007 | ±0.02 | ±0.04 | ±0.05 | ±0.08 | ±0.10 | ±0.14 | ±0.22 | ±0.37 | ±0.46 | ±0.55 | |
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| Mayor et al. (2016) | – | 0.26 | 0.54 | 0.83 | 1.00 | 1.39 | 1.51 | 2.47 | 3.18 | 4.01 | 5.37 |
| – | ±0.19 | ±0.27 | ±0.34 | ±0.38 | ±0.46 | ±0.48 | ±0.64 | ±0.73 | ±0.84 | ±0.96 | |
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| Reference | Hot Jupiters | Period-valley giants | Temperate giants | Instrument | Stellar population∗ |
| P< 10 d | 10 <P< 85 d | 85 <P< 400 d | |||
|
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| Wright et al. (2012) | 1.20 ± 0.38 | – | – | Keck+Lick | FGK V/SNH |
| Mayor et al. (2016) | 0.83 ± 0.34† | 1.64 ± 0.55 | 2.90 ± 0.72 | HARPS+CORALIE | F5 – K5 V/SNH |
|
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| Bayliss & Sackett (2011) | 0.10 |
– | – | SuperLupus | dwarfs/Lupus-FOV |
| Santerne (2012) | 0.95 ± 0.26‡ | – | – | CoRoT | FGK V/center |
| Santerne (2012) | 1.12 ± 0.31‡ | – | – | CoRoT | FGK V/anti-center |
| Howard et al. (2012) | 0.4 ± 0.1 | – | – | Kepler | GK V/K-FOV |
| Santerne et al. (2012b) | 0.57 ± 0.07 | – | – | Kepler | FGK V/K-FOV |
| Fressin et al. (2013) | 0.43 ± 0.05 | 1.56 ± 0.11 | 3.24 ± 0.25 | Kepler | FGK V/K-FOV |
| This work | 0.47 ± 0.08 | 0.90 ± 0.24 | 3.19 ± 0.73 | Kepler | F5 – K5 V/K-FOV |
Notes. The horizontal line separates the values determined by RV surveys (above the line) from the ones determined by photometric transit surveys (below the line).
SNH refers to solar neighborhood; center refers to the FOVs observed by CoRoT toward the galactic center during the prime mission; anti-center refers to the FOVs observed by CoRoT toward the galactic anti-center during the prime mission; IRa01 and LRa01 are two FOVs toward the galactic anti-center observed by CoRoT K-FOV refers to the Kepler prime mission FOV.
This value slightly differs from the one provided in Mayor et al. (2016) for planets up to 11 days of period. The difference is the planet HD 108147b (P = 10.89 d) that we included in the population of the period-valley giants and not in the hot jupiters.
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