Search for associations containing young stars (SACY) - VI. Is multiplicity universal? Stellar multiplicity in the range 3–1000 au from adaptive-optics observations

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Volume 580 (August 2015)

A&A, 580 (2015) A88

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Table 2

Summary of the properties and frequency of visual multiple systems identified for the SACY associations studied in this work.

Name	ID	Dist.	Age^a	Max./Min.	N. of observed^b	N. of VBs^c	MF_3−1000au^d
		(pc)	(Myr)	(Myr)	objects	(this work)	(%)
AB Doradus	ABD	34 ± 26	100	100/50	16 (16)	5	31
Argus	ARG	106 ± 51	40	50/20	1	0	–
β–Pic MG	BPC	31 ± 21	22	30/10	17 (17)	5	29
Carina	CAR	85 ± 35	35	35/10	26 (24)	5	21
Columba	COL	82 ± 30	35	40/15	17 (16)	6	38
ϵ–Cha	ECH	108 ± 9	9	9/6	10 (10)	2	20
Octans	OCT	141 ± 34	38	38/10	11 (10)	5	50
Tuc–Hor	THA	48 ± 7	33	33/10	14 (14)	3	21

Notes. The minimum and maximum ages represent the dispersion found in the literature.

^(a)

Ages are derived from the convergence method described in Torres et al. (2006) using new radial velocity values, results to appear in Torres et al. (in prep.)

^(b)

Effective number used to calculate MF values shown in parentheses.

^(c)

Systems either confirmed from PM analysis or high probability (≥95% detections) based on single-epoch data.

^(d)

In the separation range 3–1000 au considering observed targets with sensitivities ≥95% of our sample.

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