\begin{table}%t1
   \caption{\label{fits}The polynomial fit used in the model. }
         \small%\centerline
{
\begin{tabular}{lcccccccc}
\hline\hline
&$a_0$&$a_1$&$a_2$&$a_3$&$a_4$&$a_5$&$a_6$&rms error\\
\hline
$M_R$&1.063e+01&--1.265e+01&6.343e+00&--1.333e+00&1.438e--01&--7.656e--03&1.591e--04&0.433\\
$M_I$&8.075e+00&--9.450e+00&4.890e+00&--1.031e+00&1.102e--01&--5.768e--03&1.175e--04&0.315\\
$M_J$&1.064e+00&--5.835e--01&8.581e--01&--1.886e--01&2.033e--02&--1.063e--03&2.160e--05&0.076\\
$M_H$&1.202e-01&8.509e--01&7.639e--02&--1.412e--02&1.294e--03&--5.493e--05&8.356e--07&0.039\\
\hline
\end{tabular}}
\smallskip
The fits take the form $M_X = \sum_i a_i M_K^i$. As in the SIPSII survey the 
   $R/I$~bands are photographic $R_{\rm 59F}$/$I_{\rm IVN}$ and the $J$, $H$, and $K_{\rm s}$ bands are on the 2MASS system. Objects in the fit in different photometric systems had their magnitudes converted using Bessell (\cite{Bessell1986}) for the optical data and Carpenter (\cite{Carpenter2001}) for the infrared.
\end{table}