Table 2: Detection rate (expressed in %) as a function of orbital period and parallax. The percentage is given along with its binomial error; the total number of stars in the bin is listed between parentheses. For $\varpi > 5$ mas and $100 \le P(\rm d) \le 3000$, the detection rate comes close to 100% when removing SB2 systems, systems with composite spectra or with a poor-quality spectroscopic orbit.
Period range (d)
    0-100 100-2000 2000-3000 3000-5000 any P
  over 15 16 $\pm$ 3 (177) 69 $\pm$ 5 (81) 58 $\pm$ 14 (12) 9 $\pm$ 12 (12) 35 $\pm$ 3 (292)
Parallax (mas) 10-15 7 $\pm$ 2 (106) 69 $\pm$ 7 (42) 80 $\pm$ 18 (5) 18 $\pm$ 19 (5) 26 $\pm$ 3 (162)
  5- 10 8 $\pm$ 2 (232) 51 $\pm$ 6 (74) 65 $\pm$ 12 (17) 18 $\pm$ 14 (5) 21 $\pm$ 2 (336)
  0-5 7 $\pm$ 1 (351) 24 $\pm$ 3 (170) 4 $\pm$ 4 (25) 5 $\pm$ 5 (21) 12 $\pm$ 1 (584)
  any $\varpi$ 9 $\pm$ 1 (866) 45 $\pm$ 3 (367) 39 $\pm$ 6 (59) 28 $\pm$ 7 (43) 21 $\pm$ 1 (1374)


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Article Contents
1 Introduction
2 The Hipparcos data
3 The sample
4 Astrometric wobble detection
5 Orbit assessment
6 Some astrophysical implications
7 Conclusions
References
List of tables
List of figures