\begin{table}%t1 
\par
\caption {Program  stars and their  basic stellar parameters.\label{tab1}}
%\centerline
 {\begin{tabular}{ r l c c c }
\hline \hline
\noalign{\smallskip}
Obj(BS/HD) & Sp. type& $T_{\rm eff}^{a}$ & $M_{\rm bol}^{b}$ & 
${\rm Mass}^{c}$ \\
          &            &  K~           & mag              & $M_{\odot}$\\   
\noalign{\smallskip}
\hline
\noalign{\smallskip}
  $\alpha$ Tau (1457) & K5+III& 3874 & --1.7 $\pm$ 0.2 & 1.5 $\pm$ 0.3   \\
  $\delta$ Oph (6056)& M0.5III & 3790 & --2.2 $\pm$ 0.3 & 1.6 $\pm$ 0.3\\
  $\nu$  Vir (4517) & M1III & 3812 & --2.2 $\pm$ 0.4 & 1.7 $\pm$ 0.4 \\
  $\alpha$ Cet (911) & M1.5IIIa & 3909 & --3.2 $\pm$ 0.3 & 3.6 $\pm$ 0.4\\
  $\sigma$ Lib (5603) & M2.5III & 3596 & --3.4 $\pm$ 0.5 & 2.2 $\pm$ 0.5\\
%\noalign{\smallskip}
  $\lambda$ Aqr (8698)& M2.5III & 3852 & --3.4 $\pm$ 0.7 & 3.7 $\pm$ 1.2\\
  $\beta$ Peg (8775) & M2.5II-III & 3603 & --3.3 $\pm$ 0.2 & 2.2 $\pm$ 0.3\\
  $\tau^4$ Eri (1003) & M3+IIIa & 3712 & --2.9 $\pm$ 0.4 & 2.0 $\pm$ 0.4\\
  $\mu$ Gem (2286) & M3III & 3643 & --3.3 $\pm$ 0.3 & 2.3 $\pm$ 0.5\\
  $\delta$ Vir (4910) & M3III & 3643 & --2.4 $\pm$ 0.3 & 1.4 $\pm$ 0.3\\
%\noalign{\smallskip}
  10 Dra (5226) & M3.5III & 3730 &  --2.9 $\pm$ 0.3 & 2.1 $\pm$ 0.4\\
  $\rho$ Per (921) & M4II &    3523 & --4.1 $\pm$ 0.4 & 3.2 $\pm$ 0.5\\
  BS6861 (6861)  & M4   &  3600  & --5.2 $\pm$ 2.0 &  6.3 $\pm$ 4.0\\
  $\delta^2$ Lyr (7139) & M4II & 3420 & --5.5 $\pm$ 0.8 & 5.5 $\pm$ 2.0\\
  RR UMi (5589) & M4.5III &   3397 &  --3.4 $\pm$ 0.3 & 1.6 $\pm$ 0.3\\
%\noalign{\smallskip}
  $\alpha$ Her (6406) & M5Ib-II & 3293 & --5.8 $\pm$ 1.6 & 5.0 $\pm$ 2.0\\
  OP Her (6702)  & M5II  &   3325 &  --4.4 $\pm$ 0.8 &  2.3 $\pm$ 1.0\\
  XY Lyr (7009)  & M5II  &  3300 & --5.1 $\pm$ 1.1 &  3.7 $\pm$ 1.5\\
  R Lyr (7157) &  M5III &   3313  & --4.3 $\pm$ 0.3 &  2.1 $\pm$ 0.5\\
  RZ Ari (867) & M6III &  3341 &  --3.5 $\pm$ 0.6 &  1.5 $\pm$ 0.4\\
%\noalign{\smallskip}
  30g Her (6146) & M6-III &  3298 & --4.2 $\pm$ 0.4 & 2.0 $\pm$ 0.6\\
  SW Vir (114961) & M7-III: &  2886 &  --4.4 $\pm$ 0.9 &  1.3 $\pm$ 0.3\\
  RX Boo (126327) & M7.5-8 &  2850 & --4.6 $\pm$ 0.8 &  1.3 $\pm$ 0.3\\
 \hline
\end{tabular}}
\par
\smallskip
 $^{{a}}$   
Based on the infrared flux method. The
			uncertainty in~$T_{\rm eff}$ for individual
                        objects is estimated to be $\pm$100~K; 
 $^{{b}}$   based on the Hipparcos trigonometric parallaxes
                        and measured bolometric fluxes;
 $^{{c}}$   based on the evolutionary tracks of Fig.~\ref{fig1}.  
\end{table}