\begin{table}%t5
%\centering
\par
\caption{Comparison between mean values of the NG~parameters
derived from models with constant $A_{\rm{1}}, A_{\rm{2}}$,
$A_{\rm{3}}$ and from models with a rotating spherical nucleus for
the investigated sample of long-period (LP) comets and~20
short-period comets. Comets C/1991~T2 and C/1995~Y1 were excluded
from the basic statistical analysis (17 LP comets) because another
relations of $h(r)$ ($g^*$($r$) with $k=0$ i.e. the power law or
$g$($r$)-like function with $r_{\rm {0}}\neq 2.808$~AU) probably are
more adequate for them (see Table~\ref{tab2}). Two next two comets
(C/1998~P1 and C/1993 A1) with the greatest NG parameters and
$(1/a)_{\bf{ori}} < 10^{-4}$ are excluded from the sample of 15~LP
comets. LP models of a rotating spherical nucleus are taken from
Table~\ref{tab4}.\label{tab5}} 
{\small
\begin{tabular}{lccccc}
  \hline\hline
  % after \\: \hline or \cline{col1-col2} \cline{col3-col4} ...
  &&&&& \\
   \multicolumn{6}{c}{\bf I. Long period comets; models with constant $\vec{A_1, A_{{2}}}$ and $\vec{A_{{3}}}$}   \\
  &&&&& \\
    & \multicolumn{3}{c}{\bf 17 LP comets} & {\bf 19 LP comets} & {\bf 15 LP comets}  \\
      \multicolumn{1}{r}{Models with:}  & $g$($r$) & $g_{\rm{S}}$($r$) & $f$($r$) & $g$($r$)$_{{\rm best}\; r_{\rm {0}}}$ & $g$($r$) \\
      &&&& \\
 ${\big <}A^*{\big >}_{\rm{weighted}}\times 10^{8}$~AU~day$^{-2}$        & 1.75~$\pm$~0.02   & 1.59~$\pm$~0.02   & 1.21~$\pm$~0.02   & 1.89~$\pm$~0.02   & 1.53~$\pm$~0.02 \\
 ${\big <}|A^*_{\rm{2}}/A^*_{\rm{1}}|{\big >}_{\rm{weighted}}$                              & 0.065~$\pm$~0.003 & 0.056~$\pm$~0.003 & 0.054~$\pm$~0.003 &0.052~$\pm$~0.003  & 0.081~$\pm$~0.004 \\
 ${\big <}F/F_{\odot}{\big >}_{\rm{weighted}}\times 10^{5}$                    & 5.94~$\pm$~0.07   & 5.71~$\pm$~0.07   & 4.42~$\pm$~0.07   & 5.80~$\pm$~0.07   & 5.20~$\pm$~0.07 \\
   &&&& \\
 ${\big <}A^*{\big >}\times 10^{8}$~AU~day$^{-2}$                   & 6.43~$\pm$~0.13   & 2.85~$\pm$~0.17   & 2.40~$\pm$~0.07   & 4.52~$\pm$~0.09   & 4.07~$\pm$~0.15 \\
 ${\big <}|A^*_{\rm{2}}/A^*_{\rm{1}}|{\big >}$                                         & 0.16~$\pm$~0.02   & 0.20~$\pm$~0.05   & 0.20~$\pm$~0.03   & 0.23~$\pm$~0.02   & 0.17~$\pm$~0.02 \\
 ${\big <}F/F_{\odot}{\big >}\times 10^{5}$                               & 21.8~$\pm$~0.4    & 14.1~$\pm$~0.6    & 11.6~$\pm$~0.2    & 15.0~$\pm$~0.2    & 13.8~$\pm$~0.4 \\
  \hline
  &&&&& \\
   \multicolumn{6}{c}{\bf II. Models of a rotating spherical nucleus}   \\
  &&&&& \\
  & \multicolumn{3}{c}{\bf 14 long-period comets} & \multicolumn{2}{c}{\bf 20 short-period comets} \\
  & \multicolumn{3}{c}{\bf (spherical nucleus)} & \multicolumn{2}{c}{\bf (non-spherical nucleus)}  \\
    &&&&& \\
    \multicolumn{1}{r}{Models with:}  & $g$($r$) & $g_{\rm{S}}$($r$) & $f$($r$) &\multicolumn{2}{c}{ $g$($r$)} \\
    &&&&& \\
  ${\big <}A^*{\big >}_{\rm{weighted}}\times 10^{8}$~AU~day$^{-2}$        & 2.27~$\pm$~0.03 & 2.16~$\pm$~0.03 & 2.35~$\pm$~0.02 &\multicolumn{2}{c}{ 0.3321~$\pm$~0.0007}    \\
  ${\big <}\eta {\big >}_{\rm{weighted}}$                                      & 9\fdg4~$\pm$~0\fdg3 & 7\fdg3~$\pm$~0\fdg22 & 7\fdg5~$\pm$~0\fdg2 &\multicolumn{2}{c}{ 7\fdg14~$\pm$~0\fdg02}  \\
  ${\big <}F/F_{\odot}{\big >}_{\rm{weighted}}\times 10^{5}$                    & 7.70~$\pm$~0.07 & 7.35~$\pm$~0.07 & 7.97~$\pm$~0.07 &\multicolumn{2}{c}{ 1.128~$\pm$~0.002}      \\
  &&&&& \\
  ${\big <}A^*{\big >}\times 10^{8}$~AU~day$^{-2}$                   & 7.45~$\pm$~0.20 & 4.44~$\pm$~0.11 & 4.05~$\pm$~0.10 &\multicolumn{2}{c}{ 0.49~$\pm$~0.04}        \\
  ${\big <}\eta {\big >}$                                                 & 18\fdg8~$\pm$~1\fdg32 & 16\fdg0~$\pm$~1\fdg2 & 16\fdg3~$\pm$~1\fdg1 &\multicolumn{2}{c}{ 15\fdg1~$\pm$~1\fdg2} \\
  ${\big <}F/F_{\odot}{\big >}\times 10^{5}$                               & 25.3~$\pm$~0.7  & 15.1~$\pm$~0.4  & 13.8~$\pm$~0.3  &\multicolumn{2}{c}{ 1.66~$\pm$~0.14}        \\
  \hline
\end{tabular}
}
\end{table}