\begin{table}%t4
\par
\caption {\label{Tab:diagnostics}Binarity and photometric-variability diagnostics for stars from
sample~III (as well as binaries or suspected binaries from sample~IV).
}
%\centerline
 {\begin{tabular}{rrllccclcllll}
\hline\hline
\multicolumn{6}{l}{{\bf a. Spectroscopic binaries} (marked as black circles in Figs.~2 and 3)}\\
\hline
HD  & $N$ &  $\Delta t$ &  Sp  &  $\sigma_0(Vr)$ &
\multicolumn{1}{c}{$<\!\epsilon\!>$}
 & ${\it Sb}$ & Flag & Rem. & GCVS$^a$ & Var. & $\sigma(Hp)$ & $P_{\rm phot}$\\
    &     &   (d)       &  & (\kms) & (\kms) & (\kms) & & & & & (mag) & (d)\\
\hline
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 \\%(4 Dra)
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 
%& IV 
&   & * & & 0.015\\
16~058 &    5 & 4443 &  M3III &  3.70 & 0.26 & 3.65 & SB 
%& IV 
&   & NSV 866 & Lb: & 0.118\\
104~216&    5 & 3626 &  M2III &  1.99 & 0.27 & 3.43 & SB 
%& IV 
&   & FR Cam  & L   & 0.064\\ 
134~627&    5 & 3922 &  M0     & 1.82 & 0.28 & 3.31 & SB 
%& IV 
&   & FF Boo * &    & 0.031\\
142~804&    5 & 4964 &  M1III  & 2.64 & 0.27 & 2.68 & SB 
%& IV 
&   & NSV 7351& Irr & 0.026\\
219~215&    7 & 4741 &  M2III  & 0.87 & 0.24 & 1.72 & SB 
%& III
&$^c$  & *        &    & 0.010\\ 
\hline
\end{tabular}}
\par
\smallskip
\par
$^a$ 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~\ref{Tab:orbits}.\\
$^c$ HD~219~215: Preliminary orbital period: 2500~d.\\
 {\begin{tabular}{rrllcclclllll}
\hline\hline
\multicolumn{6}{l}{{\bf b. Suspected binaries} (marked as black triangles in Figs.~2 and 3)}\\
\hline
HD  & $N$ &  $\Delta t$ &  Sp  &   $\sigma_0(Vr)$ 
 & ${\it Sb}$ & Flag & \multicolumn{2}{c}{Rem.$^a$} & GCVS & Var. &$\sigma(Hp)$& $P_{\rm phot}$\\
    &     &   (d)       &  & (\kms) & (\kms) & & & & && (mag) & (d)\\
\hline 
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? & III$^d$&  & *        &    & 0.013\\ 
\hline 
\multicolumn{6}{l}{{\bf 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? & IV$^b$ &  & GO Eri &    & 0.035\\
66~875 &    8 & 4034 &  M3III & 1.06 & 4.47 &  ORB/jitter? & III$^b$&  & 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? & IV$^c$ & & *      &     & 0.022\\
149~165&    5 & 5087 &  M1III & 0.67 & 1.82 & SB/jitter? & IV$^c$ & & *      &     & 0.018\\
153~698&   12 & 4209 &  M4III & 0.86 & 4.09 & SB + jitter?&III&  & *      &     & 0.033\\ 
\hline
\multicolumn{6}{c}{{\bf 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\\
\hline
\end{tabular}}
\par
\smallskip
$^a$ This column specifies whether the
binarity suspicion resulted from campaign~III or IV (see
Table~\ref{Tab:sample}).\\
$^b$ 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.~\ref{Fig:Sb-sigma}.\\
$^c$ HD~129~902 and HD~149~165 are probably spectroscopic binaries, given
their location in Fig.~\ref{Fig:Sb-sigma} just above the dashed
line. Unfortunately, the radial-velocity data presented in
Fig.~\ref{Fig:SB?} are too scarce to confirm that conclusion. \\
$^d$ HD~189~063: Orbital period larger than 3600~d.
\end{table}