\begin{table}%t3
%\centering
\par
\caption{\label{results} Derived parameters from model comparisons.}
\par
\begin{tabular}{llllll}
\hline\hline \noalign{\smallskip}
ID, LHS    & MK  & M/H & Mass        & Age         & $V_{\rm tan}$     \\             & Type &       & ($M_\odot$)  & (Gyr)       &   (km~s$^{-1}$) \\   %     &                    \\   %           based on comparison\\        %& 
\hline   \\                                                                                                                     %      
1,1047\tablefootmark{*}&M4\tablefootmark{1}     & 0   &  0.16--0.18    & 0.08--0.17   & 22  $\pm$ 1   \\ % M5   (M)   &  ...                 MS Star\\                    %&  
2,~1050	 &  M3.5\tablefootmark{1}   & 0   &  0.21--0.23    & 0.125--10    & 37  $\pm$ 1   \\ % M3   (M3)	 &  ...                MS Star\\                    %&   
3,~1104	 &  	       & 0   &  0.42--0.46    & 0.12--10     & 59  $\pm$ 3   \\ % M3   (M)	 &  ...                MS Star\\                    %&   
4,~1475	 &  M1\tablefootmark{1}     & 0   &  0.55--0.58    & 0.12--0.30   & 48  $\pm$ 4   \\ % M2   (M3)	 &  Variable Star      MS star\\                    %&   
5,~228	 &  	       & --1  &  0.10--0.14    & 0.05--0.20   & 206 $\pm$ 10  \\ % M2   (M)	 &   ...               Subdwarf\\                  %&    
6,~1923	 &  M6\tablefootmark{2}     & 0   &  0.10--0.11    & 0.4--10      & 98  $\pm$ 4   \\ % M6   (M6)	 &  ...                Low mass star on MS\\        %&   
7,~243	 &  	       & --.5 &  0.08--0.11    & 0.11--0.25   & 179 $\pm$ 5   \\ % M5   (M)	 &  ...                Young MS star\\              %&   
8,~1976\tablefootmark{*}&	       & 0   &  0.53--0.61    & 0.055--10    & 83  $\pm$ 10  \\ % M2.5 (M)	 &  Double or multiple MS Star\\                    %&   
9,~2065	 &  M9e\tablefootmark{3}    & 0   &  0.06--0.07    & 0.25--0.45   & 23  $\pm$ 1   \\ % M9   (M9)	 &  Flare star         Star at the end of MS\\      %&   
10,~306	 &  M5.5\tablefootmark{4}   & 0   &  0.10--0.13    & 0.04--10     & 80  $\pm$ 18  \\ % M5   (M4.5)&  ...                 MS Star / Binary\\           %&  
11,~2472	 &  M3.5\tablefootmark{1}   & 0   &  0.18--0.21    & 0.12--10     & 43  $\pm$ 2   \\ % M5.5 (M3.5)&  Flare star          MS Star\\                    %&  
12,~326	 &  	       & --.5 &  0.34--0.44    & 0.035--10    & 582 $\pm$ 238 \\ % M2.5 (M)	 &   ...               Subdwarf\\                  %&    
13,~334	 &  	       & --1  &  0.09--0.10    & 0.3--10      & 286 $\pm$ 51  \\ % M3   (M)	 &  ...                Subdwarf\\                  %&    
14,~2632	 &  M7.5\tablefootmark{5}   & 0   &  0.08--0.10    & 0.6--10      & 60  $\pm$ 3   \\ % M7.5 (M7.5)&  ...                 Star at the low end of MS\\  %&  
15,~...	 &  M4\tablefootmark{1}     & 0   &  0.11--0.14    & 0.12--10     & 19  $\pm$ 1   \\ % M4   (M4)	 &  Flare star         MS star\\                    %&   
16,~2686	 &             & 0   &  0.08--0.10    & 0.09--0.18   & 36  $\pm$ 2   \\ % M6   (M)	 &  ...                MS star\\                    %&   
17,~2719	 &             & 0   &  0.14--0.16    & 0.2--10      & 114 $\pm$ 11  \\ % M5   (M)	 &  ...                MS star / Binary \\          %&   
18,~360	 &             & --1  &  0.20--0.35    & 0.2--10      & 304 $\pm$ 51  \\ % M1.5 (M)	 &  ...                Subdwarf\\                  %&    
19,~369	 &  M4\tablefootmark{1}     & 0   &  0.18--0.22    & 0.060--0.105 & 70  $\pm$ 4   \\ % M3.5 (M3.5)&  ...                 Young MS Star\\              %&  
20,~2924	 &  M9e\tablefootmark{3}    & 0   &  0.07--0.08    & 0.6--10      & 43  $\pm$ 3   \\ % M9   (M9)	 &  Flare star         Star at the low end of MS \\ %&   
21,~3343	 &  M3\tablefootmark{6}     & 0   &  0.37--0.42    & 0.070--0.105 & 41  $\pm$ 1   \\ % M3   (M3)	 &  ...                Young MS Star\\              %&   
22,~3445\tablefootmark{*}&M3\tablefootmark{1}     & 0   &  0.36--0.45    & 0.03--0.05   & 63  $\pm$ 3   \\ % M3   (M)	 &  Flare star         Young star or Binary\\       %&   
23,~3482	 &  M1.5\tablefootmark{3}   & 0   &  0.60--0.62    & 0.2--10      & 38  $\pm$ 2   \\ % M1   (M1)	 &  ...                MS Star\\                    %&   
24,~3494\tablefootmark{*}&M5.5e\tablefootmark{3}  & 0   &  0.09--0.11    & 0.12--0.20   & 12  $\pm$ 0   \\ % M5.5 (M5.5)&  Flare star          Young star/Binary\\          %&   
25,~528	 &  M3\tablefootmark{1}     & 0   &  0.39--0.45    & 0.065--0.1   & 97  $\pm$ 4   \\ % M2.5 (M2.5)&  ...                 Young MS Star\\              %&  
26,~3872	 &  M4\tablefootmark{6}     & 0   &  0.23--0.28    & 0.06--0.125  & 82  $\pm$ 9   \\ % M4   (M4)	 &  ...                Young MS Star\\              %&   
27,~535	 &  M3.5\tablefootmark{6}   & --.5 &  0.16--0.20    & 0.05--0.12   & 26  $\pm$ 1   \\ % M2.5 (M3.5)&  ...                 MS star\\  
\hline 
\end{tabular}
\tablebib{\tablefoottext{1}{\citet{1985ApJS...59..197B};} \tablefoottext{2}{\citet{1993ApJ...410..387F};}	
  \tablefoottext{3}{\citet{Leggett1992};}
  \tablefoottext{4}{\citet{1991AA...244..409M};}
  \mbox{\tablefoottext{5}{\citet{1995AJ....109..797K};}}
  \tablefoottext{6}{\citet{1991adc..rept.....G}.}}
\tablefoot{{The mass and age ranges
    are based only on the errors in the parallax and photometry and do not
    include the systematic error of uncertain metallicity. The latter can have
    a large impact on mass and age as described in Sect.~4.2.} \tablefoottext{*}{These are known or suspect unresolved binary systems while the parameters
    are based on an assumption of being single stars. Unaccounted multiplicity
    will tend to increase the predicted age and decrease the predicted mass.}}
\end{table}