\begin{table}%t2
\caption{\label{table:2} Integrated flux density, root-mean-square noise levels, and derived dust temperature, power-law exponent of the opacity law, mass, fractional dust luminosity, and characteristic radial dust distances for the 22 stars observed at 870-$\mu$m.}
 \small%\centering
\par
\begin{tabular}{l c c c c c c c}
\hline\hline\noalign{\smallskip}
Object ID & Integrated flux sensity, $F$ & RMS noise, $\sigma$ & $T_{{\rm dust}}$\tablefootmark{a} & $\beta$ & Dust mass\tablefootmark{b}, $M_{\rm dust}$ & $f_{\rm dust}$ & $R_{\rm dust}$\\
 & (mJy) & (mJy/beam) & (K) &  & ($M_{{\rm Moon}}$) & ($10^{-4}$) & (AU)\\
\hline
\multicolumn{8}{c}{DETECTIONS ($>$$3\sigma$)} \\
%\hline
HD~21997 & 17.6~$\pm$~8.0 & 4.6  & 52 & 0.7 & 33~$\pm$~15 & 4.9 & 240 \\ %R=148 for beta=0, given R is for beta=0.7
\par
HD~95086 & 41.3~$\pm$~18.4 & 10.4 & 150+(15$-$45)\tablefootmark{c} & ... & $>$76\tablefootmark{d} & 6.4$-$14 & 16+(250$-$1500) \\ %R=13+(140--1300) for beta=0, given R is for beta=0.5
\par
HD~98800 & 33.6~$\pm$~8.4 & 3.9 & 155\tablefootmark{e} & 0.1 & 8.5 & 470 & 2.4 \\ %R=2.2 for beta=0, given R is for beta=0.1
\par
HD~109573 & 21.5~$\pm$~6.6 & 3.1 & 88\tablefootmark{f} & 0.7 & 19.5~$\pm$~6.0 & 38 & 77 \\ %R=99 for beta=0, given R is for beta=0.7
\par
HD~131835 & 8.5~$\pm$~4.4 & 3.0 & 89 & 0.1 & 21~$\pm$~11 & 25 & 47 \\ %R=52 for beta=0, given R is for beta=0.1
\par
HD~141569 & 12.6~$\pm$~4.6 & 2.3 & 80\tablefootmark{g} & 0.8 & 27~$\pm$~10 & 73 & 110 \\
\par
HD~152404 & 42.9~$\pm$~9.8 & 3.7 & ...\tablefootmark{h} & ... & ... & ... & ... \\
\par
HD~161868 & 12.8~$\pm$~5.2 & 2.5 & 73 & 0.5 & 2.6~$\pm$~1.1 & 0.90 & 120 \\ %R=130 for beta=0, given R is for beta=0.5
\par
HD~170773 & 18.0~$\pm$~5.4 & 2.6 & 43 & 0.7 & 9.7~$\pm$~2.9 & 4.5 & 170 \\ %R=83 for beta=0, given R is for beta=0.7
\par
HD~207129 & 5.1~$\pm$~2.7 & 2.1 & 38 & 0.7 & 0.6~$\pm$~0.3 & 0.94 & 130 \\ %R=60 for beta=0, given R is for beta=0.7
%\hline
\multicolumn{8}{c}{MARGINAL DETECTIONS ($>$$2.5\sigma$)} \\
%\hline
HD~105 & 10.7~$\pm$~5.9 & 3.7 & 40 & 0.6 & 7.7~$\pm$~4.2 & 2.6 & 110 \\ %R=57 for beta=0, given R is for beta=0.6
\par
HD~30447 & 6.9~$\pm$~5.0 & 4.5 & 61 & 0.3 & 12.3~$\pm$~8.9 & 9.3 & 56 \\ %R=42 for beta=0, given R is for beta=0.3
\par
HD~195627 & 13.0~$\pm$~7.1 & 4.1 & 57 & 0.3 & 3.1~$\pm$~1.7 & 1.0 & 74 \\ %R=74 for beta=0, given R is for beta=0.3
%\hline
\multicolumn{8}{c}{NON-DETECTIONS} \\
%\hline
HD~17390 & ... & 6.8 & 55\tablefootmark{i} & ... & $<$13.4 & 1.9\tablefootmark{j} & ... \\
\par
HD~25457 & ... & 3.3 & 70\tablefootmark{k} & ... & $<$0.9 & 1.0\tablefootmark{k} & ... \\ %mark[11]=Hillenbrand2008a
\par
HD~31392 & ... & 4.7 & 49\tablefootmark{k} & ... & $<$3.4 & 1.6\tablefootmark{k} & ... \\
\par
HD~32297 & ... & 6.5 & 30\tablefootmark{l} & ... & $<$150 & 33\tablefootmark{j} & ... \\ %mark[10]=Moor2006
\par
HD~61005 & ... & 6.0 & 58\tablefootmark{k} & ... & $<$6.6 & 25\tablefootmark{k} & ... \\
\par
HD~78702 & ... & 4.2 & 36\tablefootmark{m} & 2.0\tablefootmark{m} & $<$39 & 2.6\tablefootmark{m} & ... \\ %mark13]=Williams2006
\par
HD~139664 & ... & 3.5 & 78\tablefootmark{n} & ... & $<$0.7 & 1.2\tablefootmark{n} & ... \\ %mark[14]=Beichman2006b
\par
HD~164249 & ... & 3.5 & 78 & ... & $<$5.3 & 5.9\tablefootmark{o} & ... \\
\par
HD~193307\tablefootmark{p} & ... & 3.8 & ... & ... & ... & ... & ...\\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{For detected and marginally detected sources we use the dust temperature derived from the best fit to the spectral energy distribution.}
\tablefoottext{b}{Upper $3\sigma$ limit on the dust mass for undetected sources.}
\tablefoottext{c}{In order not to be resolved the second dust belt should be at $<$1500~AU, which would mean $>$15~K, while a temperature $>$45~K would not be compatible with far-IR data.}
\tablefoottext{d}{Calculated for upper limit on dust temperature.}
\tablefoottext{e}{Ambiguous fit (see discussion in Sect.~\ref{sec:sed}).}
\tablefoottext{f}{Source appears spatially resolved (see discussion in Appendix~\ref{sec:appena}). See also more detailed modelling by \citet{Augereau1999} and SCUBA measurement by \citet{Sheret2004}.}
\tablefoottext{g}{Source appears spatially resolved (see discussion in Appendix~\ref{sec:appena}). See also modelling by \citet{Sheret2004}.}
\tablefoottext{h}{No simple debris disk model can be fitted (see Section~\ref{sec:sed}).}
\tablefoottext{i}{From \citet{Rhee2007}.}
\tablefoottext{j}{From \citet{Moor2006}.}
\tablefoottext{k}{From \citet{Hillenbrand2008a}.}
\tablefoottext{l}{From \citet{Maness2008}.}
\tablefoottext{m}{From \citet{Williams2006}.}
\tablefoottext{n}{From \citet{Beichman2006b}.}
\tablefoottext{o}{From \citet{Rebull2008}.}
\tablefoottext{p}{Not enough photometry data for reliable SED fit.}
}
\end{table}