\begin{table}%t3
%\centering
\par
\caption{\label{results}The results.}
\begin{tabular}{*{8}{c}}
\hline\hline\noalign{\smallskip}
Star name & \multicolumn{3}{c}{Fit as dust disc} & 
\multicolumn{2}{c}{Limit on extension} & 
$f_{IR} = L_{\rm{dust}}/L{\ast}$ & $f_{\rm{max}}$\tablefoottext{a} \\
& Temp, K & AU & \arcsec\  & AU & $D_{\rm{grain}}, \mu$m\tablefoottext{b} & $\times$$10^{-5}$ &  $\times 10^{-5}$  \\
\hline 
\multicolumn{8}{l}{Photometric confirmation of excess} \\ 
HD 3003 & 265 & 4.00 & 0.086 & $<$$6.5^{+2.1}_{-0.9}$ & 0.55 & 20.1 & 0.053 \\
HD 80950 & 180 & 13.6 & 0.17 & $<$$24.5^{+7.5}_{-3.5}$ & 0.01 & 9.62 & 0.544 \\
$\eta$ Tel\tablefootmark{c} &  & 3.90 & 0.081 & $<$$6$ & & 15.7 & 0.210 \\ 
       &  & 21--26 & 0.44--0.54 & -- & & 13.9 & 12.52 \\
\hline
\multicolumn{8}{l}{Constraints on radial extent of disc} \\ 
%\hline
HD 71155 & 500 & 1.98 & 0.052 & $<$$8.2^{+5.7}_{-0.5}$ & -- & 8.95 & 0.0034 \\
      & 90 & 61.03 & 1.59 & -- & -- & 1.92 & 7.60 \\
$\lambda$ Gem$^d$ & 420 & 2.16 & 0.07 & $<$$6.1^{+0.2}_{-0.3} $ & 0.012 &
5.64 & 0.002  \\ 
HD 23281 & 210 & 5.36 & 0.12 & $<$$9.5^{+4.2}_{-0.7}$ & 0.68 & 3.82 & 0.024  \\
HD 75416 & 250 & 11.1 & 0.11 & $<$$55.2^{+1.5}_{-1.5}$ & -- & 7.98 & 2.44 \\
HD 141795 & 250 & 4.64 & 0.22 & $<$$6.1^{+0.3}_{-0.4} $ & 0.73 & 4.43 & 0.008 \\
\hline
\multicolumn{8}{l}{Unconstrained by these observations} \\
%\hline
HD 31295 & 80 & 52.6 & 1.4 & -- &-- & 5.85 & 9.216 \\
HD 38206 & 90 & 48.4 & 0.70 & -- & -- & 15.1 & 84.96 \\
\hline
\end{tabular} 
\tablefoot{Note that the objects with no extension limits have too low a
fractional excess for the extension to have been detected in the
images regardless of size. Estimates of radius are based on blackbody
fits and could be up to three times larger if the grains responsible
for the emission are small. Limits on extension shown here are for a
narrow face-on discs. Errors on this limit arise from 3 $\sigma$
photometric errors and errors on the determination of the photospheric
emission at the observed wavelength.   These sources are combined to
give 3$\sigma$ uncertainties on $F_{\rm{disc}}$, which in turn give a
range of radii at which a disc could have been detected as extended emission. 
Horizontal lines indicate division into photometrically
confirmed debris discs, and sources
for which our results provide constraints on the discs (Sects.~4.1 and~4.2 respectively). \tablefoottext{a}{See Sect.~\ref{s:dis} for details of this limit;} 
\tablefoottext{b}{the minimum grain diameter (for the composition assumed in Sect.~3.3) such that grains at the maximum radius
given by the extension testing limits do not exceed the temperature of
the blackbody fit to the excess emission (where limits on the disc radius
are large compared to the blackbody radius no limit can be placed on the
minimum grain size, as even the smallest grains cannot reach the
fitted temperature at the extension limit radius);}
\tablefoottext{c}{These disc locations are taken from \citet{smitheta};}
\tablefoottext{d}{binary detected. }}
\end{table}