\begin{table}%t1
\caption{\label{t:models}\COBOLD\ radiation-hydrodynamics model atmospheres.}
%\centerline
 {\small \begin{tabular}{lllllllllllllll}
\hline\hline\noalign{\smallskip}
Model &  $T_{\rm eff}$ & \logg  & \moh & \Rstar & \lx,\ly & \lz & $T$ 
& $\tau_{\rm c}$ & $H_{{\rm p}}^{{\rm surf}}$ & \dirms & \siggran & $N_{\rm obm}$ & Modelcode\\
& [K] & [${\rm cm/s^2}$] & & [\Rsun] & [Mm] & [Mm] & [ks] & [s] & [Mm] & &[ppm]   &  & \\
\noalign{\smallskip}
\hline\noalign{\smallskip} 
\mohi     & 6~720  & 4.25 & \phantom{-}0.0 & 1.35 &           16.4 & 24.2           &           135.6 & 29.5 & 0.241 & 0.196 & 84 (17)& 5 & d3t68g43mm00n01\\
\molo     & 6~730  & 4.25 &           --1.0 & 1.35 &           16.1 & 24.2           & \phantom{1}73.8 & 29.1 & 0.238 & 0.229 & 64 (13)& 6 & d3t68g43mm10n01\\
\mosu     & 5~780  & 4.44 & \phantom{-}0.0 & 1.00 & \phantom{1}5.6 & \phantom{2}2.5 & \phantom{1}52.2 & 17.8 & 0.141 & 0.172 & 40 (8) & 5 & d3gt57g44n53\\
%\noalign{\smallskip}
\hline
\end{tabular}}
\medskip
``Model'' is the
model's name used in this paper, \Teff\ the effective temperature,
\logg\ the gravitational acceleration, \moh\ the metallicity, \Rstar\ an assumed stellar radius (not intrinsic to the simulation proper), $\lx=\ly$ the linear horizontal size of
    the square-shaped computational box, \lz\ its vertical extent, 
    $T$ the duration of the simulated time series, \tauc\ the sound crossing time over \Hpsurf, \Hpsurf\ the pressure scale height at Rosseland optical depth unity, \dirms\
    the relative spatial white light intensity contrast at disk-center,
    \siggran\ the temporal relative disk-integrated granulation-related brightness fluctuations in white light  (in parenthesis an estimate of the uncertainty),
   $N_{\rm obm}$ the number of  equivalent frequency points considered in the solution of the radiative  transfer equation, ``Modelcode'' an internal identifier of the model
    sequence.
\end{table}