The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits - IV. Gravitational instability rarely forms wide, giant planets

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Table 3

Fraction of stars that host a planetary system based on the GI populations described in Sect. 5.

Mass	N_det ^a	F_best ^b	[F_min,F_max] ^c
(M_Jup)		(%)	CL = 68%	CL = 95%
Non-scattered population

≤75	3	2.65	[1.85, 5.10]	[1.00, 7.50]
≤14	1	1.60	[1.15, 5.20]	[0.40, 8.70]
Scattered population

≤75	3	3.00	[2.15, 5.85]	[1.10, 8.60]
≤14	1	1.95	[1.40, 6.20]	[0.50, 10.45]

Notes. Numbers are provided for the best stellar ages. Values for the minimum and maximum ages are provided in Appendix B.

^(a)

Number of detections in the considered mass range.

^(b)

Best value of the planet frequency compatible with the observations.

^(c)

Minimum and maximum values of the frequency compatible with the results for a given confidence level (CL).

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