Table 1
Frequency of giant planets reported by various surveys around the full spectral type range.
Sample | Technique | Sep. range | Mass range | Frequency | Distribution | Reference |
(AU) | (MJ) | (%) | (AU) | |||
|
||||||
102 M | RV | ≲1 | ≲3 | 1−5 | observed | Bonfils et al. (2013) |
822 FGK | RV | ≤5 | ≥0.3 | 14 | observed | Mayor et al. (2011) |
31 old-A | RV | 0.1−3 | 0.5−14 | 9−14 | observed | Johnson et al. (2010) |
585 F-M | RV | ≤3 | 0.3−10 | 10.5 | observed | Cumming et al. (2008) |
|
||||||
42 AF | AO | 5−320 | 3−14 | 5.9−18.8 | flat/Cu08a | Vigan et al. (2012) |
85 F-M | AO | 5−500 | ≤100 | ≤10 | flat + GIb | Janson et al. (2012) |
15 BA | AO | ≤300 | ≤100 | ≤32 | flat + GI | Janson et al. (2011) |
118 F-M | AO | 25−856 | ≥4 | ≤20 | flat/Cu08 | Nielsen & Close (2010) c |
88 B-M | AO | ≥40 | 5−13 | ≤10 | Cu08 | Chauvin et al. (2010) |
88 FGKM | AO | 50−250 | 0.5−13 | ≤9.3 | power laws in m and ad | Lafrenière et al. (2007) |
22 GKM | AO | ≥30 | ≥3 | ≤5 | power laws in m and ad | Kasper et al. (2007) |
Notes. Results on the frequency of giant planets are reported at 68% confidence level, except for those from Janson et al. (2011, 2012), which are stated at 99% confidence level.
They inferred the planet population from boundaries in a planet mass-semi major axis grid considering a disk instability model.
They performed their analysis using results from surveys of Masciadri et al. (2005), Biller et al. (2007), and Lafrenière et al. (2007).
They inferred the planet population from power law distributions with different coefficients of m and a that were used in Cumming et al. (2008). See these publications for details.
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