\begin{table}%t1
%\centering
\par
\caption{\label{sample}The sample.} 
\begin{tabular}{ccccll}
\hline\hline\noalign{\smallskip}
Star name & Stellar type & Age &
Distance\tablefootmark{a} &  \multicolumn{2}{c}{IRAS fluxes (mJy)\tablefootmark{b}}\\ 
 &  & Myr & pc & 12~$\mu$m & 25~$\mu$m   \\
\hline
HD 3003 & A0V & 50\tablefootmark{c} & 47 & 148 + 16 ($\pm$20) & 34 + 241 ($\pm$20)
\\  
HD 23281 & A6V & 626\tablefootmark{d} & 43 & 251 + 36 ($\pm$20) & 59 + 107
($\pm$28)  \\  
HD 23432 & B8V & 100\tablefootmark{e} & 119 & 127 + 256 ($\pm$43) & 29 + 1159
($\pm$42)  \\ 
HD 31295 & A0V & 100\tablefootmark{e} & 37 & 336 + 238 ($\pm$65) & $78 - 110$
($\pm$121)  \\ 
HD 38206 & A0V & 9\tablefootmark{f} & 69 & 130 + 7 ($\pm$23) & 30 + 67 ($\pm$21)
\\ 
$\lambda$ Gem\tablefootmark{g} & A3V & 560$^f$ & 29 & 1166 + 214 ($\pm$28) & 271 +
161 ($\pm$52) \\ 
HD 71155 & A0V & 169\tablefootmark{c} & 38 & 675 + 162 ($\pm$31) & 157 + 249
($\pm$41)  \\ 
HD 75416 & B8V & 5\tablefootmark{f} & 97 & 134 + 86 ($\pm$22) & 31 + 86 ($\pm$38)
\\ 
HD 80950 & A0V & 80\tablefootmark{f} & 81 & $120 - 5$ ($\pm$26) & 28 + 101 ($\pm$17)
\\ 
HD 141795 & Am & 450\tablefootmark{e} & 22 & 1154 + 67 ($\pm$25) & 269 + 141
($\pm$28)  \\ 
$\eta$ Tel\tablefootmark{i} & A0V & $12^h$ & 48 & 263 + 138 ($\pm$34) & 61 + 394
($\pm$22)  \\ 
\hline
\end{tabular} 
\tablefoot{\tablefoottext{a}{Distance from parallax in Hipparcos;}
\tablefoottext{b}{fluxes are shown as star +
 excess ($\pm$error);}  
 \tablefoottext{c}{age taken from \citet{song01};} 
 \tablefoottext{d}{age taken
 from \citet{kunzli};} 
 \tablefoottext{e}{age determined from
 theoretical evolutionary tracks of \citet{song01}, see discussion
 in text;} 
 \tablefoottext{f}{age taken from \citet{rieke};} 
 \tablefoottext{g}{HD 56537;} 
 \tablefoottext{h}{Age from $\beta$ Pictoris association membership, \citet{zuckermanEA};} 
 \tablefoottext{i}{HD 181296.  For those sources without ages listed in the literature (HD 23432, HD 31295 and HD~141795) the $\beta$ and $c_1$ magnitudes as listed in \citet{hauck} were used to determine $T_{\rm{eff}}$ and $\log(g)$ from the grids of \citet{moon}. Then the theoretical evolutionary tracks of \citet{song01} were used to determine the approximate ages for these stars.}}
\end{table}