Table 2
Fractions of stars hosting super-Earths and cold Jupiters.
| Probability | Observed(a) | Full population(b) | [Fe/H] < −0.2 | −0.2 < [Fe/H] < 0.2 | 0.2 < [Fe/H] |  |
ē |
|---|---|---|---|---|---|---|---|
| P(SE) | 0.30(c) | 0.29 ± 0.02 | 0.13 ± 0.02 | 0.31 ± 0.02 | 0.43 ± 0.05 | 1.8 ± 0.9 | 0.08 ± 0.10 |
| P(CJ) | 0.11(d) | 0.14 ± 0.01 | <0.01 | 0.12 ± 0.01 | 0.42 ± 0.05 | 1.3 ± 0.5 | 0.18 ± 0.19 |
| P(SE ∩ CJ) | 0.09 | 0.05 ± 0.01 | <0.01 | 0.05 ± 0.01 | 0.10 ± 0.03 | 3.7 ± 0.9 | 0.11 ± 0.13 |
 |
0.69(c) | 0.62 ± 0.02 | 0.87 ± 0.07 | 0.62 ± 0.03 | 0.25 ± 0.04 | 1.8 ± 0.8 | 0.09 ± 0.10 |
 |
0.21(c) | 0.24 ± 0.02 | 0.12 ± 0.02 | 0.26 ± 0.02 | 0.32 ± 0.05 | 2.2 ± 1.0 | 0.06 ± 0.10 |
 |
0.01(e) | 0.09 ± 0.01 | <0.01 | 0.07 ± 0.01 | 0.32 ± 0.05 | 2.1 ± 0.9 | 0.19 ± 0.18 |
| P(SE|CJ) | 0.90 ± 0.20 | 0.34 ± 0.06 | 1.0 ± 1.41 | 0.41 ± 0.09 | 0.25 ± 0.07 | – | – |
| P(CJ|SE) | 0.32 ± 0.08 | 0.16 ± 0.03 | 0.04 ± 0.04 | 0.15 ± 0.03 | 0.24 ± 0.07 | – | – |
 |
0.10 ± 0.20 | 0.66 ± 0.09 | <0.01 | 0.59 ± 0.11 | 0.75 ± 0.14 | – | – |
 |
0.68 ± 0.08 | 0.84 ± 0.07 | 0.96 ± 0.27 | 0.85 ± 0.09 | 0.76 ± 0.14 | – | – |
Notes. The top part shows the fraction of stars harboring (lacking) super-Earths (SE), cold Jupiters (CJ), and combinations thereof at an age of 5 Gyr. The bottom panel shows conditional probabilities P(A|B) where A denotes the existence of at least one instanceof planet type A in a given system and 
denotes its non-existence. Uncertainties of probabilities are based on Poisson errors. The last two columns list the mean planet multiplicity
and mean eccentricity ē with their standard deviations. While for P(SE) (P(CJ)), this takes into account only super-Earths (cold Jupiters); for the other classes we consider all planets with K > 2 ms−1. (a) If not stated otherwise, probabilities are from Zhu & Wu (2018) using their “nominal” super-Earth definition where MP sin i < 20 M⊕. (b) Population NG76 in the NGPPS series. (c)Quoting for P(SE) the fraction of Kepler systems hosting super-Earths in Zhu et al. (2018). (d) As estimated by Cumming et al. (2008). (e)Order of magnitude estimate by Zhu & Wu (2018).
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