\begin{table}%T3
      \caption{Characteristics of possible late-type field dwarf
      contaminants from the literature$^{a}$.} 
         \label{MLT}
    \small%\centerline
{
         \begin{tabular}{l c c c c c}
            \hline
            \hline
            \noalign{\smallskip}
Spectral	& $M_I$		& $I-J$		& $J-K_{\rm s}$ 	& $n_\odot$		& $d_{I=25}^{b}$ 	\\  
type   		& (mag)  	& (mag)		& (mag)			& (10$^{-3}$ pc$^{-3}$)	& (pc)	   	\\ 
             \hline 
M3--4~V	&  9.07  	& 1.83	& 0.84	&19.6		& 7700 \\ % 
M4--5~V 	& 10.14 	& 1.80	& 0.86	&16.3	       	& 5700 \\ %
M5--6~V  	& 11.91  	& 2.47	& 0.90	& 9.81         	& 3100 \\ %
M6--7~V  	& 12.90  	& 2.72	& 0.93	& 4.90         	& 2200 \\ %
M7--8~V  	& 14.16  	& 3.24	& 0.98	& 1.907        	& 1300 \\ %
M8--9~V  	& 14.68  	& 3.54	& 1.06	& 1.285        	& 1100 \\ %
M9--L0~V 	& 15.23  	& 3.80	& 1.12	& 0.768        	&  840 \\ % 
L0--1~V  	& 15.27  	& 3.55	& 1.27	& 0.637        	&  820 \\ %
L1--2~V  	& 15.69  	& 3.50	& 1.38	& 0.861        	&  680 \\ %
L2--3~V  	& 16.19  	& 3.62	& 1.43	& 1.000	       	&  550 \\ %
L3--4~V  	& 16.67  	& 3.72	& 1.49	& 0.834        	&  450 \\ %
L4--5~V  	& 17.14  	& 3.81	& 1.54	& 0.819        	&  360 \\ %
L5--6~V  	& 17.61  	& 3.90	& 1.60	& 0.869        	&  290 \\ %
L6--7~V  	& 18.07  	& 4.06	& 1.66	& 0.785        	&  240 \\ %
L7--8~V  	& 18.52  	& 4.12	& 1.71	& 0.644        	&  190 \\ %
L8--9~V  	& 18.90  	& 4.22	& 1.81	& 0.462        	&  160 \\ %
L9--T0~V 	& 18.95  	& 4.40	& 1.73	& 0.308        	&  160 \\ %
T0--1~V  	& 19.01  	& 4.63	& 1.58	& 0.220        	&  160 \\ %
T1--2~V  	& 19.04  	& 4.94	& 1.17	& 0.241        	&  150 \\ %
T2--3~V  	& 19.04  	& 5.19	& 0.81	& 0.406        	&  150 \\ %
T3--4~V  	& 19.07  	& 5.23	& 0.51	& 0.788        	&  150 \\ %
T4--5~V  	& 19.22  	& 5.01	& 0.29	& 1.42 	       	&  140 \\ %
T5--6~V  	& 19.61  	& 4.76	& 0.11	& 2.38         	&  120 \\ %
T6--7~V  	& 20.35  	& 5.25	& 0.00	& 3.45         	&   85 \\ %
T7--8~V  	& 21.60  	& 5.50	&--0.06	& 4.82         	&   48 \\  	  
             \hline
         \end{tabular}}
  \smallskip
 $^{a}$  
The sources of the $M_I$ absolute magnitude, $I-J$, and $J-K_{\rm s}$ colours,
and spatial densities are obtained or derived by us from data in the literature
(Kirkpatrick et~al. \cite{Kirkpatrick1994}; Dahn et~al. \cite{Dahn2002}; Hawley et~al. \cite{Hawley2002}; Cruz et~al.
\cite{Cruz2003}; Tinney et~al. \cite{Tinney2003}; Vrba et~al. \cite{Vrba2004}; Bochanski et~al. \cite{Bochanski2007}; Burgasser
\cite{Burgasser2007}; West et~al. \cite{West2008}). 
See the text for further details.
 $^{b}$~$d_{I=25}$ is the heliocentric distance of a dwarf with an apparent magnitude
$I = 25.0$~mag, assuming an interstellar extinction proportional to the
heliocentric distance. 
At the end of Sect.~\ref{thecontaminants} there is a brief discussion on this
assumption. 
   \end{table}