Table 1: Parallaxes and proper motions for the CNS candidates in the Torino Program. Columns are: target name, positions at J2000, number of reference stars, number of frames, proper motions, absolute parallax, correction applied to the relative parallax to obtain an absolute parallax, the interval of time for which we have observations, apparent magnitude in the I band from in-house data unless discussed in Sect. 2, the CNS parallax along with the source.
Name RA     Dec     $N_*, N_{\rm f}$ $\mu_{\alpha}$ $\mu_{\delta}$ $\pi$ COR $\Delta T$ I   $\pi_{\rm CNS}^{\rm source}$
  h:m:s    d:$^\prime$: $^{\prime\prime}$   mas/yr mas/yr mas mas years   mas
LHS 1050 0:15:47 +13:33:08 8, 81 606.3 $\pm$ 1.5 336.9 $\pm$ 1.5 89.0 $\pm$ 3.5 1.84 5.07 10.04 86.6 $\pm$ 13.4Y
GD 806 1:12:28 -01:51:19 11, 64 14.9 $\pm$ 1.4 -73.7 $\pm$ 1.4 8.4 $\pm$ 3.3 2.04 5.41 13.55 99.0 $\pm$ 11.0w
GJ 3140 2:10:14 +11:32:11 8, 170 -20.0 $\pm$ 0.6 3.6 $\pm$ 0.8 5.3 $\pm$ 1.8 2.56 5.41 9.85 90.0 $\pm$ 30.0p
LP 475-70 4:25:53 +12:11:47 20, 67 -102.1 $\pm$ 1.1 -232.8 $\pm$ 1.1 59.4 $\pm$ 2.8 1.35 5.31 14.77 81.0 $\pm$ 11.0w
LHS 1675 4:31:07 -05:20:26 11, 39 -175.0$\pm$ 2.1 -507.8 $\pm$ 2.7 28.5 $\pm$ 3.6 1.83 5.32 11.00 87.0 $\pm$ 10.2H
Cl* Mel.a 4:35:00 +17:33:40 17, 31 3.4 $\pm$ 1.8 -18.0 $\pm$ 1.5 2.7 $\pm$ 3.8 1.62 5.24 12.55 94.0 $\pm$ 17.0p
LP 60-179 9:02:51 +68: 3:18 13, 48 182.9 $\pm$ 1.4 345.3 $\pm$ 2.0 85.3 $\pm$ 3.8 2.47 5.25 9.75 98.0 $\pm$ 10.6Y
LHS 295 10:52:04 +13:59:51 11, 71 -1119.0 $\pm$ 1.1 206.8 $\pm$ 1.6 80.2 $\pm$ 2.7 1.90 5.37 9.95 83.9 $\pm$ 25.7Y
GJ 3667 11:29:19 +18:16:35 10, 55 6.2 $\pm$ 1.2 6.5 $\pm$ 1.1 1.3 $\pm$ 2.9 2.21 6.09 13.23 114.0 $\pm$ 13.0w
LHS 2472 11:54:08 +09:48:56 5, 38 89.6 $\pm$ 2.0 -796.7 $\pm$ 1.9 82.7 $\pm$ 4.4 2.06 5.13 9.92 96.1 $\pm$ 19.7Y
GJ 1167a 13:09:36 +28:59:10 5, 15 -337.5 $\pm$ 2.4 -203.1 $\pm$ 2.3 83.1 $\pm$ 6.3 2.04 4.22 11.14 86.0 $\pm$ 12.5H
LHS 369 14:20:09 -09:36:35 8, 32 -607.0 $\pm$ 1.2 -826.8 $\pm$ 1.9 68.1 $\pm$ 3.8 1.85 6.15 10.25 91.1 $\pm$ 15.0Y
LHS 3872 22:54:45 -05:28:37 6, 32 610.1 $\pm$ 1.6 354.4 $\pm$ 2.1 40.4 $\pm$ 4.9 2.18 5.09 11.21 94.0 $\pm$ 23.0H
Source: $Y=\rm Yale$ Parallax catalog, w = photometric parallax assuming white dwarf with the McCook & Sion (1999) calibration, p = photometric parallax assuming main sequence star, H = Parallax from Heintz (1994), a = Cl* Mel. is Cl* Melotte 25 LH 27.

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