\begin{table}%t1
%\centering
\par
\caption{\label{tab:models}Key initial model parameters and some results.} 
\begin{tabular}{c c c c c c r l c l c c } 
\hline\hline \noalign{\smallskip}       
Model & $Q$ & $\cal{C}$ & $M_{{\rm BH}}$ & $R_{{\rm NS}}$ & $d_{{\rm i}}$ & $L$ & $\Delta x$ & $M_{{\rm u}}$ & $M_{{\rm b}}$ & $M_{{\rm g}}$  & $|$h/l$|$ \\ 
& && $M_\odot$ & km & km & km & km & $M_\odot$  & $M_\odot$ & $M_\odot$  &  \\ 
\hline
 M5.145 & 5 & 0.145 & 7.0 & 14.3 & 92 & 1550 & 0.77 & 0.07 & 0.08 
  &  0.15     & N  \\ 
 M4.145 & 4 & 0.145 & 5.6 & 14.3 & 80 & 1400 & 0.68 & 0.08 & 0.10 
  & 0.18      & Y  \\
 M3.145 & 3 & 0.145 & 4.2 & 14.3 & 68 & 1100 & 0.54 & 0.06 & 0.09 
  & 0.15      & Y \\
 M2.145 & 2 & 0.145 & 2.8 & 14.3 & 56 &  880 & 0.43 & $<$$10^{-2}$ & 0.07 
  & 0.08      & Y \\  
 M5.160 & 5 & 0.160 & 7.0 & 12.9 & 92 & 1550 & 0.77 & 0.01 & 0.05 
  & 0.06      &  --  \\
 M4.160 & 4 & 0.160 & 5.6 & 12.9 & 76 & 1250 & 0.61 & 0.03 & 0.06 
  & 0.09      &  N  \\
 M3.160 & 3 & 0.160 & 4.2 & 12.9 & 66 & 1100 & 0.54 & 0.03 & 0.06 
  & 0.09      &  N  \\
 M2.160 & 2 & 0.160 & 2.8 & 12.9 & 52 &  820 & 0.40 & $<$$10^{-2}$ & 0.04 
  & 0.05       & Y  \\  
 M5.180 & 5 & 0.180 & 7.0 & 11.5 & 88 & 1500 & 0.73 & $<$$10^{-3}$ & $<$$10^{-3}$
  & $<$$10^{-3}$ & N \\
 M4.180 & 4 & 0.180 & 5.6 & 11.5 & 76 & 1250 & 0.61 & $<$$10^{-3}$ & $<$$10^{-3}$
  & $<$$10^{-3}$ & N \\
 M3.180 & 3 & 0.180 & 4.2 & 11.5 & 64 & 1050 & 0.51 & $<$$10^{-2}$ & 0.01 
  & 0.01       & N  \\
 M2.180 & 2 & 0.180 & 2.8 & 11.5 & 50 &  780 & 0.38 & $<$$10^{-3}$ & 0.004
  & 0.004      & N  \\  
\hline                  
\end{tabular}
\tablefoot{Initial parameters: mass ratio $Q$, compactness $\cal{C}$,
  black hole mass $M_{{\rm BH}}$, neutron star radius $R_{{\rm NS}}$, initial orbital distance $d_{{\rm i}}$, size of largest 
  grid $L$, size of finest zone $\Delta x = L/2048$. 
  The mass of the NS is $1.4~M_\odot$ in all cases.
  Values at the end of the simulation, only for high-resolution models: 
  unbound+ejected gas mass $M_{{\rm u}}$, 
  bound neutron star mass around BH~$M_{{\rm b}}$, 
  neutron star mass not instantly accreted by BH~$M_{{\rm g}}$, 
   $|$h/l$|$ states whether the difference between values for
  $M_{{\rm g}}$ in low-resolution and high-resolution simulations
  is less than $20\%$ (Yes/No; `-' no low-res model computed). The
  spin-up of the BH~by accretion of matter is not taken into account.} 
\end{table}