\begin{table}%t5
\caption{\label{spectral_indices}Spectral indices and classifications for \epsba,~Bb.}
\small%\centerline
 {  
  \begin{tabular}{ccccccccc}
  \hline
  \hline\noalign{\smallskip}
  Source & H$_{2}$O$-J$ & CH$_{4}$$-J$ & H$_{2}$O$-H$ & CH$_{4}$$-H$ & CH$_{4}$$-K$ & Direct & M1 & M2\\
  \hline
  \multicolumn{9}{c}{Spectra smoothed to $R =150$} \\	
  $\varepsilon$~Indi~Ba   & 0.650 (T0.0) & 0.656 (T0.0) & 0.592 (T0.0) & 0.873 (T2.0) & 
  0.587 (T2.0) & T1.0 & T1.0 & ...  \\
  $\varepsilon$~Indi~Bb   & 0.172 (T6.0) & 0.305 (T6.5) & 0.308 (T5.5) & 0.295 (T6.0) & 
  0.178 (T5.5) & T6.0 & T6.0 & ...  \\
  \hline		
  \multicolumn{9}{c}{Spectra smoothed to $R =500$} \\	
  $\varepsilon$~Indi~Ba   & 0.652 (.../...) & 0.657 (T1.0/T1.5) & 0.589 (T1.0/T0.5) & 
  0.872 (T2.0/T2.0) & 0.588 (T2.0/T2.0) & T1.0 & T1.5 & T1.5  \\
  $\varepsilon$~Indi~Bb   & 0.171 (T6.0/T6.0) & 0.302 (T6.0/T6.0) & 0.303 (T6.0/T6.0) & 
  0.290 (T6.0/T6.0) & 0.180 (T5.5/T5.5) & T6.0 & T6.0 & T6.0  \\
  \hline	
  \multicolumn{9}{c}{Unsmoothed spectra} \\	
  $\varepsilon$~Indi~Ba   & 0.645  & 0.660  & 0.589  & 0.870  & 
  0.589 & T1.0 & ... & ...  \\
  $\varepsilon$~Indi~Bb   & 0.171 & 0.307 & 0.299 & 0.287 & 
  0.178 & T6.0 & ... & ...  \\
  \hline		
\end{tabular}}
\medskip
The spectra have been smoothed to two resolutions to emulate the observations of the spectral standard stars defined by \citet{Burgasser:2006}.  The indices derived from our unsmoothed data have been included to quantify the uncertainty when measuring indices from spectra at different resolutions. M1~refers to method~1 of \citeauthor{Burgasser:2006} where the measured spectral indices are compared to that of each of the standard stars, and~M2 refers to their method~2 where the measured spectral indices are compared to a range of values for each spectral type.  Direct classification compares the overall spectral shape to the standard star spectra. The spectral type derived from each index is shown in parentheses after each measurement with only M1 being defined for a resolution of $R=500$.  The average spectral type from each method is shown on the right-hand side. Only direct classification is possible for our unsmoothed spectra.  The range of the H$_{2}$O$-J$~index is ill-defined for the earliest T~dwarfs and is therefore omitted for~\epsba.
\end{table}