\begin{table}%t2%t3
\caption{\label{tab:results}Example table of results for 636 WD-M star binaries.}
\par
\small%\centerline
  \begin{tabular}{l|rrrrrcrcccrrccccccr}
    \hline \hline
%&&&&&&&&&&&&&&&&&&& \\[-8pt]
    Designation & $d_{\rm WD}$ [pc] & $d_{\rm M}$ [pc] & $\mathcal{C}$ & $T_{\rm eff}^{\rm WD}$ [K] & $T_{\rm eff}^{\rm M}$ [K] & $R_{\rm WD} [R_{\odot}]$ & $R_{\rm M} [R_{\odot}]$ & log $g_{\rm WD}$ & log $g_{\rm M}$ & $M_{\rm WD} [M_{\odot}]$ & $M_{\rm M} [M_{\odot}]$ & [Fe/H]$_{\rm M}$ & Emission & WD & Res. & $m$ & $N$ & $\chi^2_{\rm red,min}$\\
%&&&&&&&&&&&&&&&&&&& \\[-8pt]
    \hline
      J0017$-$0009 & 475.8 & 514.6 & $-$0.055 & 50000.0 & 3600.0 & 0.016 & 0.433 & 7.5 & 4.5 & 0.6 & 0.46 & $-$0.0 & \textit{H} & DA & $\bullet$ & 3783 & 1572 & 4.29\\ 
      J0017+0040 & 547.2 & 253.5 & 0.518 & 13000.0 & 3200.0 & 0.013 & 0.189 & 7.5 & 5.0 & 0.6 & 0.17 & $-$0.0 &  & DA & $\star$ & 3824 & 1599 & 4.10\\ 
      J0039+2548 & 370.9 & 335.9 & 0.070 & 34000.0 & 3200.0 & 0.015 & 0.189 & 8.0 & 5.0 & 0.6 & 0.17 & $-$0.0 &  & DA &  & 3838 & 1599 & 2.26\\ 
      J0041+1511A$^*$ & 1332.0 & 607.1 & 0.529 & 32000.0 & 3600.0 & 0.014 & 0.190 & 7.5 & 3.0 & 0.6 & 0.18 & $-$1.0 &  & DA &  & 3842 & 1602 & 2.74\\ 
{J0052$-$0053}$^*$ & 579.9 & $>$577.2 & $<$0.003 & 15000.0 & 3600.0 & 0.008 & $>$0.433 & 8.5 & 3.0 & 1.0 & $>$0.46 & +0.3 & \textit{H}, rm*& DA &  & 3843 & 1596 & 19.69\\
{J0054$-$0025} & 385.1 & $>$383.1 & $<$0.003 & 17000.0 & 3200.0 & 0.015 & $>$0.189 & 8.0 & 4.0 & 0.5 & $>$0.17 & +0.3 & \textit{H}, rm*& DA &  & 3843 & 1596 & 6.51\\ 
    \hline
  \end{tabular}
  \medskip
Typical uncertainties are mentioned in the text. The 11~PCEBs and PCEB candidates from \citet{2007MNRAS.382.1377R}, as well as the two CV~candidates mentioned in Sect.~\ref{subsec:emission}, are shaded in gray. $^*$:~M~component probably a giant due to the very low surface gravity of 3~dex. $^{\dag}$:~VLMO~candidates. \textit{H}: H$_\alpha$ and other Balmer line emission. rm*: WD~parameters taken from \citet{2007MNRAS.382.1377R}. $\bullet$: clearly resolved objects with projected angular distance $<$$1.5\arcsec$. $\circ$:~Objects with slight angular separation and without further treatment. $\star$: objects separated by more than $1.5\arcsec$, likely to be not those represented in the spectrum. ?:~the photometric data corresponding to the object id specified does not exist in the SDSS database. The complete table is available as Supplementary Material to the online version of this article at the CDS.
\end{table}