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 2

Fraction of stars that host a planetary system, assuming linear flat mass and semi-major axis distributions.

SMA	Mass	N_det ^a	F_best ^b	[F_min,F_max] ^c
(AU)	(M_Jup)		(%)	CL = 68%	CL = 95%

5–500	5–75	3	2.45	[1.70, 4.70]	[0.90, 6.95]
5–500	5–14	1	1.00	[0.75, 3.30]	[0.25, 5.55]
20–300	0.5–75	3	2.10	[1.50, 4.05]	[0.80, 5.95]
20–300	0.5–14	1	1.15	[0.85, 3.65]	[0.30, 6.20]

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 and semi-major axis (SMA) 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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