\begin{table}%T7
\caption{\label{t:tab7}Comparison between various determinations of the luminosity of the
horizontal branch (from Cacciari \& Clementini \cite{Cacciari2003}).}
%\centering
\par
\begin{tabular}{lc}
\hline\hline
Method& $M_{V}$(RR)\\
      & at $\rm [Fe/H]=-1.5$\\
\hline
Statistical parallaxes& 0.78~$\pm$~0.12\\ 
Trigonometric parallaxes (RR Lyr)& 0.58~$\pm$~0.13\\ 
Trigonometric parallaxes (HB stars)& 0.62~$\pm$~0.11\\ 
Baade-Wesselink (RR Cet)& 0.55~$\pm$~0.12\\
HB stars: Evolutionary models -- bright& 0.43~$\pm$~0.12\\
HB stars: Evolutionary models -- faint& 0.56~$\pm$~0.12\\
Pulsation models (visual) & 0.58~$\pm$~0.12\\
Pulsation models ($PL_{\rm K}Z$) & 0.59~$\pm$~0.10\\
Pulsation models (double-modes) & 0.57~$\pm$~0.06\\
Fourier parameters& 0.61~$\pm$~0.05\\
\hline
Main Sequence Fitting& 0.56~$\pm$~0.07\\
\hline
\end{tabular}
\end{table}