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 1

Surveys considered for the construction of the NACO-LP archive sample.

Name	Telescope	Instrument	Techniques^a	Band	N_survey ^b	N_NaCo−LP	Reference

M05	VLT	NaCo	DI	H,K	18	5	Masciadri et al. (2005)
L05	HST	NICMOS	COR	H	45	17	Lowrance et al. (2005)
S06	HST	NICMOS	ADI	H	116	47	Song et al. (unpublished)^c
K07	VLT	NaCo	ADI, RDI	L	22	6	Kasper et al. (2007)
B07	VLT	NaCo	SDI	H	45	24	Biller et al. (2007)
L07	Gemini	NIRI	ADI	H	85	50	Lafrenière et al. (2007)
C10	VLT	NaCo	DI	H,K	91	29	Chauvin et al. (2010)
H10	MMT	Clio	ADI	L,M	54	27	Heinze et al. (2010)
V12	Gemini, VLT	NIRI, NaCo	ADI	H,K	42	4	Vigan et al. (2012)
R13	VLT	NaCo	ADI	L	59	21	Rameau et al. (2013)
B13	Gemini	NICI	ASDI	H	80	22	Biller et al. (2013)
B14	Subaru	HiCIAO	ADI	H	63	29	Brandt et al. (2014)
C15	VLT	NaCo	ADI	H	85	47	Chauvin et al. (2015)

Notes.

^(a)

Techniques: ADI = angular differential imaging, usually coupled with saturated imaging; ASDI = angular and spectral differential imaging; COR = coronagraphy; DI = direct imaging (saturated); RDI = reference differential imaging; SDI = spectral differential imaging.

^(b)

The sum of N_survey for all surveys is larger than 199, the total number of stars considered in our analysis, because some stars were observed by several surveys.

^(c)

HST, cycle 13, GO10176.

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