4. Results

Table 1 (available in electronic form only; see footnote to title page) gives our main results for the 530 single-lined stars for which reliable radial velocities could be obtained (all velocity data in km s^-1).

In Table 1, Cols. 1-3 give HD numbers and J2000 coordinates, Col. 4 indicates the atmospheric parameters of the adopted synthetic template spectrum (t followed by the temperature and g by 10 log g ), and Col. 5 the rotational velocity of the star determined as described above.

Columns 6 and 7 give the number of observations, n, and the time span (days) between the first and last observation.

Columns 8-13 list, respectively, the mean radial velocity and its standard error, the standard deviation of the individual velocities, the average uncertainty of a single observation as computed by XCSAO (see Paper I), the ratio of observed to expected rms error, the observed  and the probability that it is due to the random errors of n observations of an otherwise constant star. If the observed standard deviation is less than predicted by XCSAO (which often happens by chance when small numbers of observations are involved), the error of the mean velocity is given as the latter divided by . Columns 14 and 15 list, for reference, the average values of the goodness-of-fit statistic <R> (Kurtz et al. 1992) and the height of the correlation peak.

Results for the 65 double-lined systems treated with TODCOR are given in Table 2 (click here). The first three columns are as in Table 1, while Cols. 4 and 5 give the parameters of the two templates (i.e. temperature and rotation; log g  = 4.0 in all cases). Column 6 lists the mean luminosity parameter provided by TODCOR, and Col. 7 the number of observations. The systemic velocity and its mean error are given in Cols. 8-9, derived, in order of preference, from a full orbital solution, from the available pairs of primary and secondary velocities using the Wilson (1941) method (in which the systemic velocity and mass ratio are derived from a fit of V₂ vs. V₁, assuming only momentum conservation), or as a straight mean. For systems with an orbital solution or analysed by the Wilson method, the mass ratio (q) and its mean error are given in the following two columns. The remarks in the final column indicate double-lined (SB2) or triple (SB3) systems with either no significant velocity variation observed (C), analysed by the Wilson method (W), or with an orbital solution (O). For the triple systems, only a single-lined orbit for the short-period pair has been determined.

   

[d]    [HJD-2 440 000] [km s^-1] [km s^-1] [km s^-1] [km s^-1]

005843 9.17607 7868.883 -5.64 73.00 79.26 0.005 185.2 1.18

0.00016 1.792 0.24 0.33 1.35 0.004 70.4 4.96

022054 10.41302 7478.887 17.44 71.17 77.90 0.129 130.6 5.89

0.00038 0.146 0.89 2.40 0.78 0.010 4.3 0.91

024623 19.66227 7861.470 9.47 63.92 65.08 0.491 130.0 0.53

0.00037 0.014 0.09 0.19 0.22 0.002 0.3 0.64

037603B 27.76205 7886.104 20.62 20.43 21.79 0.405 349.6 2.71

0.00621 0.226 0.38 0.88 0.66 0.024 4.1 1.95

039166 15.86860 7568.472 9.01 61.97 62.16 0.232 304.3 0.75

0.00037 0.034 0.12 0.26 0.27 0.003 0.8 0.80

054901 41.00333 7709.088 -9.86 44.46 58.45 0.638 349.3 0.72

0.00125 0.024 0.15 0.26 0.72 0.004 0.5 2.36

074425 1.585232 7797.961 16.88 101.93 118.97 0.011 184.0 1.77

0.000008 0.100 0.35 0.64 0.79 0.005 22.6 2.19

075638 5.81667 7558.279 11.05 28.92 0.083 322.0 2.96

0.00086 0.452 0.91 1.20 0.056 28.2

087810 12.94724 7442.274 -0.24 55.50 55.68 0.439 48.6 0.47

0.00012 0.008 0.07 0.17 0.18 0.002 0.3 0.49

088162 24.74771 7764.323 -27.67 23.85 25.05 0.603 17.4 0.78

0.00310 0.038 0.15 0.32 0.44 0.009 0.93 1.10

121648 4.99167 7750.057 -29.50 89.85 92.02 0.007 219.4 1.86

0.00003 0.512 0.27 0.56 0.72 0.004 36.9 2.39

134193 5.76930 7572.411 4.77 77.40 87.61 0.004 73.7 1.14

0.00006 0.930 0.22 0.50 0.48 0.005 57.9 1.07

147428 75.55870 7784.165 -19.66 27.28 38.46 0.089 186.7 0.70

0.02198 1.059 0.18 0.25 0.83 0.014 5.3 2.71

156458 17.11603 7990.970 -30.65 60.58 63.07 0.161 279.1 0.54

0.00030 0.078 0.18 0.24 3.06 0.004 1.7 8.74

159172 13.87687 7674.910 2.60 54.89 66.78 0.218 204.1 3.61

0.00033 0.055 0.58 1.49 0.37 0.010 1.8 0.75

171275 15.40365 7839.525 -30.87 58.78 71.37 0.083 305.4 0.91

0.00058 0.116 0.18 0.23 0.73 0.005 2.9 2.91

177005 11.10549 7943.389 2.79 53.24 72.04 0.333 143.3 2.86

0.00063 0.078 0.49 1.52 1.53 0.011 2.6 1.93

198226 1.49941 7773.106 -16.03 90.51 0.021 93.7 10.1

0.00004 0.421 2.25 3.27 0.034 101.3

203031 48.73828 7760.086 6.43 27.49 40.59 0.493 159.0 1.29

0.00442 0.080 0.19 0.53 0.55 0.009 1.0 1.11

222995 85.83454 7819.892 -20.28 31.73 41.20 0.335 175.0 2.17

0.02771 0.392 0.25 0.86 0.51 0.008 1.8 1.18

   

    HD     HD     HD     HD     HD

  4086    27832   81725    125488  181656

  4856 30315   84667 127457 182246

  6696 36844   88829 130353 190004

  7138 38610   89866 130667 196386

  8302 38753   91728 131160 198028

  8607 42313BC   94206 131721 198047

11284 46318   99946 135282 198346

13179 51832 103846 141652 203405

16453 54269 104622 142124 212048

17613A 63795 110220 145873 213619

18570 72984 110456 150340A 217855

19759 74781 111005 166600 218010

23290 77214 118703 168066 219712

26757 79725 119603 179280

27743 80678 121136 180005

The elements of the 18 double-lined and 2 single-lined spectroscopic orbits derived here are given in Table 3 (click here), and the orbits are shown in Fig. 2 (click here). The 73 stars rotating more rapidly than 120 km s^-1  and for which no velocities could be obtained are listed in Table 4 (click here) (HD numbers only).

Finally, the individual radial-velocity observations for single-lined and double-lined stars are listed in Tables 5 and 6, respectively (provided in electronic form only).

      
Figure 2: Spectroscopic orbits and observed radial velocities for 20 binary systems. The orbital elements are given in Table 3 (click here)