\begin{table}%t4
  %\begin{center}
\par
    \caption{Object specific TPM input parameters. The $\lambda_{\rm ecl}$
             and $\beta_{\rm ecl}$ values are the ecliptic coordinates of
             the spin vector direction, with $\beta_{\rm ecl}$ counted
             from the equator.
         \label{tbl:tpm_input}}
  \begin{tabular}{ccrcl}
 % \noalign{\smallskip} 
 \hline \hline %\noalign{\smallskip}
  Object      & [$H$, $G$]              & $P_{\rm sid}$ [h] & $\lambda_{\rm ecl}$, $\beta_{\rm ecl}$ & Source of shape \& spin vector\\
   \hline \noalign{\smallskip}
   (1) Ceres  & [3.28, 0.05]$^{1}$  &  9.074184 & 331.51$^{\circ}$, +77.88$^{\circ}$ & HST observations$^{4}$ \\
   (2) Pallas & [4.13, 0.16]$^{2}$  &  7.813225 &  34.80$^{\circ}$, --11.75$^{\circ}$ & Lightcurve inversion techniques$^{5,6}$ \\
   (4) Vesta  & [3.20, 0.34]$^{3}$  &  5.342129 & 319.45$^{\circ}$, +59.23$^{\circ}$ & HST observations$^{7}$ \\
  (10) Hygiea & [5.43, 0.07]$^{2}$  & 27.623265 & 117.01$^{\circ}$, --28.53$^{\circ}$ & Lightcurve inversion techniques$^{8}$ \\
 \hline 
  \end{tabular}
  %\end{center}
\par
  $^{1}$ \citet{Lagerkvist:1992}; %Lagerkvist et al.\ (1992);
  $^{2}$ \citet{Lagerkvist:2001}; % et al.\ (2001);
  $^{3}$ \citet{Muller:1998}; % \& Lagerros (1998);
  $^{4}$ \citet{Thomas:2005}; % et al.\ (2005);
  $^{5}$ M.\ Kaasalainen, priv.\ comm.\ 22/Sep./2005;
  $^{6}$ \citet{Torppa:2003}; % et al.\ (2003);
  $^{7}$ \citet{Thomas:1997}; % et al.\ (1997), Note added in proof;
  $^{8}$ M.\ Kaasalainen, priv.\ comm.\ 31/Jan./2006;
  \end{table}