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Table C.4.

Values of masses and eccentricities needed to carve the gaps for the systems in the sample assuming one, two, or three planets.

Name One planet Two planets Three planets
Circular Eccentric Circular Eccentric Circular
MP∕MJ MP∕MJ eP MP∕MJ MP∕MJ e1 e2 MP∕MJ
HD 1466 ≥50 2.7 0.89 ≥50 2.7 0.59 0.61 ≥15
HD 3003 ≥50 1.7 0.66 ≥50 1.7 0.36 0.36 9.3
HD 15115 ≥50 3.5 0.55 49.8 3.5 0.33 0.29 5.1
HD 30447 ≥50 5.9 0.24 15.4 5.9 0.15 0.16 1.5*
HD 35114 ≥50 2.2 0.69 ≥50 2.2 0.39 0.39 7.7
ζ Lep ≥50 6.5 0.56 ≥50 6.5 0.34 0.29 8.3
HD 43989 ≥50 2.8 0.93 ≥50 2.8 0.65 0.65 ≥15
HD 61005 ≥50 2.7 0.42 21.3 2.7 0.29 0.29 2.1*
HD 71155 ≥50 11.2 0.80 ≥50 11.2 0.48 0.48 ≥15
HD 75416 ≥50 4.3 0.50 ≥50 4.3 0.30 0.27 7.8
HD 84075 ≥50 2.3 0.83 ≥50 2.3 0.51 0.51 12.7
HD 95086 ≥50 2.0 0.70 ≥50 2.0 0.39 0.39 9.3
β Leo ≥50 1.6 0.68 ≥50 1.6 0.38 0.39 9.6
HD 106906 ≥50 1.9 0.36 28.0 1.9 0.24 0.25 2.8
HD 107301 ≥50 5.0 0.27 18.7 5.0 0.18 0.20 2.0*
HR 4796 ≥50 1.2 0.64 ≥50 1.2 0.35 0.35 9.6
ρ Vir ≥50 6.0 0.89 ≥50 6.0 0.59 0.59 ≥15
HD 122705 ≥50 7.0 0.66 ≥50 7.0 0.36 0.36 12.6
HD 131835 ≥50 4.0 0.65 ≥50 4.0 0.36 0.35 10.5*
HD 133803 ≥50 10.0 0.61 ≥50 10.0 0.32 0.33 11.6
β Cir ≥50 13.4 0.45 ≥50 13.4 0.26 0.30 7.7*
HD 140840 ≥50 5.4 0.70 ≥50 5.4 0.39 0.40 15
HD 141378 ≥50 9.0 0.86 ≥50 9.0 0.54 0.55 ≥15
π Ara ≥50 11.8 0.48 50 11.8 0.29 0.33 5.1*
HD 174429 ≥50 2.4 0.99 ≥50 2.4 0.83 0.82 ≥15
HD 178253 ≥50 9.9 0.55 ≥50 9.9 0.32 0.29 10*
η Tel ≥50 3.8 0.36 30.2 3.8 0.25 0.25 3.4*
HD 181327 ≥50 4.3 0.28 16.6 4.3 0.04 0.29 1.6*
HD 188228 ≥50 3.3 0.57 ≥50 3.3 0.30 0.31 8.0
ρ Aql ≥50 10.1 0.84 ≥50 10.1 0.52 0.52 ≥15
HD 202917 ≥50 8.7 0.87 ≥50 8.7 0.56 0.56 ≥15
HD 206893 ≥50 4.2 0.93 ≥50 4.2 0.66 0.67 ≥15
HR 8799 ≥50 2.7 0.61 ≥50 2.7 0.33 0.33 6.7
HD 219482 ≥50 7.5 0.90 ≥50 7.5 0.60 0.61 ≥15
HD 220825 ≥50 12.0 0.30 26.9 12.0 0.2 0.2 3.2*

Notes. We indicate with an asterisk undetectable objects. Since for the eccentric case of one single planet solutions are not univocally determined, in Col. 3 we show only (MP, eP) at the boundary between detectability and undetectability. We adopt the same criterion in Col. 5 for two equal-mass planets on eccentric orbits. However, for this last case we obtained, given a fixed value of the mass, different possible combinations of the eccentricities of the two planets. Thus, for each system, we show only the combination for which values for e1 and e2 are similar.

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