\begin{table}%T7
%\centering
\small
  \caption{The five known binaries in \sco{} with an orbital period less than two days. Columns 1--3 list the primary star, the primary spectral type, and the measured orbital period. Columns 4 and 5 list the primary mass estimate as derived from the $V$-band magnitude, under the assumption that the mass ratio is $q\approx0$ and $q=1$, respectively. Columns~6 and~7 list extremes for the semi-major axis of the binary, as derived using Kepler's third law, under the assumption of a mass ratio $q\approx0$ (6th column), and $q=1$ (7th column). Finally, Cols.~8 and 9 list the subgroup of which the binary is a member and the reference for the orbital period. It is possible that a small number of closer, yet undiscovered binaries exist in \sco{}. \label{table: recovering_amin}}
  \begin{tabular}{ll l cc cc ll}
    \hline
    \hline
    Member   & Spectral   & $P$    &  \multicolumn{2}{c}{$M_1~({M}_\odot)$}    & \multicolumn{2}{c}{$a~({R}_\odot)$} & Subgroup & Reference \\
    HIP      & type      & day    &   ($q\approx0$) & ($q=1$)     & ($q\approx0$) & ($q=1$) \\ 
    \hline
    74449 & B3~IV& 0.90 & 5.2 & 4.0 & 6.8  & 7.8  & UCL  & \cite{buscombe1962} \\
    77911 & B9~V & 1.26 & 3.5 & 2.2 & 7.5  & 8.0  & US   & \cite{levato1987} \\
    78265 & B1~V & 1.57 & 10.9& 8.3 & 12.6 & 14.5 & US   & \cite{levato1987} \\
    74950 & B9~IV& 1.85 & 4.2 & 3.2 & 10.2 & 11.8 & UCL  & \cite{andersen1993} \\
    77858 & B5~V & 1.92 & 4.5 & 3.4 & 10.7 & 12.3 & US   & \cite{levato1987} \\
    \hline
  \end{tabular}
\end{table}