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Home All issues Volume 498 / No 2 (May I 2009) A&A, 498 2 (2009) 627-640 Full HTML
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Table 4:

Binarity and photometric-variability diagnostics for stars from sample III (as well as binaries or suspected binaries from sample IV).
a. Spectroscopic binaries (marked as black circles in Figs. 2 and 3)              
HD N $\Delta t$ Sp $\sigma _0(Vr)$ $<\!\epsilon\!>$ ${\it Sb}$ Flag Rem. GCVSa Var. $\sigma(Hp)$ $P_{\rm phot}$
    (d)   (km s-1) (km s-1) (km s-1)         (mag) (d)
83 069 9 4450 M2III 1.63 0.22 2.68 ORB   NSV 04545   0.015  
89 758 7 6632 M0III 3.57 0.25 3.68 ORB b NSV 04829 SR 0.019  
108 907 15 6821 M4III 2.57 0.25 3.84 ORB   CQ Dra CV 0.053  
111 129 10 3633 M2III 6.81 0.23 4.20 ORB   BY CVn * Irr 0.070  
113 406 12 4324 M1III 2.54 0.23 2.94 ORB   *   0.017  
132 813 5 3639 M4.5III 4.93 0.27 4.89 ORB b RR UMi SR 0.107 43.3
137 853 11 3794 M1III 1.66 0.22 2.94 ORB   *   0.014  
159 608 16 3981 M2III 7.87 0.25 3.55 ORB   *   0.018  
165 374 37 7349 M2III 5.03 0.33 3.61 ORB   V980 Her * Irr 0.031  
182 190 24 4197 M1III 3.15 0.22 2.88 ORB   *   0.010  
187 372 16 5787 M1III 2.42 0.26 3.21 ORB   *   0.015  
199 871 10 3964 M0III 7.47 0.24 2.33 ORB       0.012  
203 525 10 4741 M0III 1.68 0.23 0.88 ORB :   *   0.010  
212 009 9 5008 M0III 4.72 0.23 3.66 ORB   KT Aqr *   0.028  
212 047 12 3984 M4III 7.22 0.22 4.19 ORB   PT Aqr SR 0.046  
220 088 15 4743 M0III 1.88 0.22 1.67 ORB   *   0.010  
4301 5 4607 M0III 1.18 0.25 2.02 SB   *   0.015  
16 058 5 4443 M3III 3.70 0.26 3.65 SB   NSV 866 Lb: 0.118  
104 216 5 3626 M2III 1.99 0.27 3.43 SB   FR Cam L 0.064  
134 627 5 3922 M0 1.82 0.28 3.31 SB   FF Boo *   0.031  
142 804 5 4964 M1III 2.64 0.27 2.68 SB   NSV 7351 Irr 0.026  
219 215 7 4741 M2III 0.87 0.24 1.72 SB c *   0.010  
a An asterisk in this column means that the variability of the star has been discovered by Hipparcos.
b HD 89 758, HD 132 813: an orbit is also available in the literature, as listed in Table 8.
c HD 219 215: Preliminary orbital period: 2500 d.

b. Suspected binaries (marked as black triangles in Figs. 2 and 3)              
HD N $\Delta t$ Sp $\sigma _0(Vr)$ ${\it Sb}$ Flag Rem.a GCVS Var. $\sigma(Hp)$ $P_{\rm phot}$
    (d)   (km s-1) (km s-1)           (mag) (d)
65 275 9 4442 M0 0.84 3.50 SB? III       0.022  
111 946 9 5040 M1/2III 1.59 3.02 SB? III   VW Crv* Irr 0.132 45.6:
112 142 5 4613 M3III 1.14 3.42 SB? IV   $\psi$ Vir Lb 0.025  
114 961 5 4608 M7III 3.50 8.60 SB? IV   SW Vir SRb 0.198 150
189 063 8 3642 M0III 0.80 3.16 SB? IIId   *   0.013  
c. Binarity doubtful (marked as crosses in Figs. 2 and 3)              
5920 8 4157 M4III 0.77 4.83 SB/jitter? III   AK Cet Lb 0.061  
12 292 5 4606 M5III 1.00 4.83 SB/jitter? IV   AR Cet SR: 0.054  
17 491 6 4075 M5III 1.62 6.21 SB/jitter? IV   Z Eri SRb 0.157 80.0
24 693 6 4762 M1III 0.79 3.11 ORB/jitter? IVb   GO Eri   0.035  
66 875 8 4034 M3III 1.06 4.47 ORB/jitter? IIIb   BL Cnc L 0.062  
75 157 4 3626 M0 1.01 3.86 SB/jitter? IV   FW Cnc* Irr 0.040  
97 876 9 4841 M4III 1.56 4.22 ORB/jitter? III   UU Crt* SR 0.115  
129 902 5 4605 M1III 0.57 1.87 SB/jitter? IVc   *   0.022  
149 165 5 5087 M1III 0.67 1.82 SB/jitter? IVc   *   0.018  
153 698 12 4209 M4III 0.86 4.09 SB + jitter? III   *   0.033  
d. Non-SB (radial-velocity jitter) (marked as open squares in Figs. 2 and 3)              
2411 6 4171 M3III 1.03 4.58       TV Psc SR 0.085 49.1
6262 9 3702 M3III 1.04 4.51       V360 And * SR 0.066  
69 229 7 4819 M1III 0.44 2.32           0.018  
80 567 8 3627 M3 1.04 5.78       IN Hya SRb 0.129 277.8
107 397 9 3746 M3III 1.35 5.42       RY UMa SRb 0.284 295.7
112 264 6 3022 M5III 1.08 6.02       TU CVn SRb 0.077 50.0
115 322 9 3627 M6III 1.49 5.93       FH Vir SR 0.104 70.0
124 304 9 4361 M3III 0.90 5.05       EV Vir SR 0.154 120.0
125 357 8 4361 M2/3III 1.78 4.35       MZ Vir Irr 0.151  
166 253 10 3631 M0 1.11 3.96       V566 Her SRb 0.091 137.0
186 776 11 5981 M4III 0.94 4.47       V973 Cyg SRb 0.100 40.0
a This column specifies whether the binarity suspicion resulted from campaign III or IV (see Table 1).
b HD 24 693 and HD 66 875: Orbital solutions with an eccentricity of about 0.5 and periods of $845\pm7$ and $668\pm4$ d, respectively, are possible, but their reality is questionable. The stars are irregular (Lb) variables (varying from Hp = 7.13 to 7.26 and 5.94 to 6.11, respectively, in the Hipparcos catalogue) falling right on the dividing line in Fig. 2.
c HD 129 902 and HD 149 165 are probably spectroscopic binaries, given their location in Fig. 2 just above the dashed line. Unfortunately, the radial-velocity data presented in Fig. 6 are too scarce to confirm that conclusion.
d HD 189 063: Orbital period larger than 3600 d.

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