\begin{table}%t1
\par
\caption{\label{fluxes} The stellar properties, e.g. spectral type, temperature, 
  luminosity and age range are reported in the first columns (from Meyer et~al.~\cite{meyerFEPS2006},~\cite{Meyeretal2008}, Hillenbrand et~al.~\cite{Hillenbrandetal2008}). CSO 350~$\mu$m and IRAM 1.2~mm measured fluxes and upper limits are reported in the sixth and seventh column. The detected sources are highlighted in bold. In the ninth column are the references to the stellar distances (listed in the eighth column).} 
%\centerline
 {\tiny\begin{tabular}{lrrrrrrrr}
 \hline\hline
 \multicolumn{1}{l}{Source}&  
 \multicolumn{1}{c}{Spectral} &
 \multicolumn{1}{c}{$T_{\rm eff}$} &
 \multicolumn{1}{c}{log$(L_{\star}/L_{\sun}$)} &
 \multicolumn{1}{c}{log(Age)}&
 \multicolumn{1}{c}{$S_{350~\mu{\rm m}}^{\star}$} &
 \multicolumn{1}{c}{$S_{1.2~{\rm mm}}^{\star\star}$} &
 \multicolumn{1}{c}{Distance}& 
 \multicolumn{1}{c}{Ref.}\\
 \multicolumn{1}{c}{} &
 \multicolumn{1}{c}{Type} &
 \multicolumn{1}{c}{[$^{\rm o}$K]} &
 \multicolumn{1}{c}{} &
 \multicolumn{1}{c}{} &
 \multicolumn{1}{c}{[mJy]} &   
 \multicolumn{1}{c}{[mJy]} &   
 \multicolumn{1}{c}{[pc]}&   
 \multicolumn{1}{c}{}\\
 \hline
 \noalign{\smallskip}
 \multicolumn{8}{c}{FEPS sources older than 10~Myr}\\
  \noalign{\smallskip}  
 \object{HD~60737} 				   &      G0     &     5895   &  0.01    & 8.0--8.5 &&$<$4.5&$38\pm2$&(2)      \\                                
 \object{HII1101}  				   &      G0V    &     5988   &  0.08& 8.0--8.5    && $<$2.3 &$133\pm4$&(5)  \\
 \object{HII152}  				   &      G5V    &     5823   &  $-$0.10&  8.0--8.5  &&$<$2.7  &$133\pm4$&(5)  \\
 \object{HII1200}				   &      F6V    &     6217   &  0.35& 8.0--8.5  &&$<$2.3  &$133\pm4$&(5)    \\
 \object{HD~90905} 				   &      G1V    &     6028   &  0.16& 8.0--8.5 &&$<$3 &$32\pm1$&(2)         \\
 \object{HII514}   				   &     ---     &     5727   &  0.11&8.0--8.5 &&$<$2.6  &$133\pm4$&(5)      \\
  {\bf \object{HD~104860}} 			   &      F8     &     5950   &  0.12& 8.0--8.5 &$50.1\pm9.3$&$4.4 \pm1.1$  &$48\pm2$&(2)    \\
 {\bf   \object{HD~377} }   			   &      G2V    &     5852   &  0.09& 8.0--8.5 &&$4.0 \pm1.0$  &$40\pm2$&(2)\\
 {\bf \object{HD~61005}  }   			   &      G8V    &     5456   &  $-$0.25&8.0--8.5 &$95\pm12$  &&$35\pm1$&(2)\\
 {\bf \object{HD~107146} }   			   &      G2V    &     5859   &  0.04&8.0--8.5&$319\pm6$& &$29\pm1$&(2)\\
 \object{HD~72687}     				   &      G5V    &     5738   &  $-$0.05& 8.0--8.5 &$<$54&&$46\pm2$&(2)\\
 \object{HII250}       				   &     ---    &     5767    &  $-$0.04&8.0--8.5 &     & $<$3.28&$133\pm4$&(5)\\                    \object{HD~219498}   				   &      G5     &     5671   &  0.69  &  8.5--9.0  &&$<$4.8  &$150\pm13$&(3)   \\
 \object{HD~61994}  				   &      G6V    &     5538   &  0.01  & 8.5--9.0   &&$<$2.6 &$28\pm2$&(2)\\
 \object{HD~145229}   				   &      G0     &     5893   &  $-$0.02  & 8.5--9.0   &$<$22.5 &$<$2.8  &$33\pm1$&(2)\\
 \object{HD~150706} 				   &     G3(V)   &     5883   &  $-$0.02 & 8.5--9.0   &&$<$3.2  &$27\pm1$&(2)\\
 \object{HD~204277}    				   &      F8V    &     6190   &  0.29  & 8.5--9.0   &&$<$2.1  &$34\pm1$&(2)\\
 \object{HD~85301}   				   &      G5     &     5605   &  $-$0.15  & 8.5--9.0   &$<$17.4&$<$2.7  &$32\pm1$&(2)\\
  \object{HD~69076}     				   &      K0V    &     5405   &  $-$0.28  &  9.0--9.7  &$<$42   &$<$2.1  &$34\pm1$&(2)\\
 \object{HD~205905}   			           &      G2V    &     5925   &  0.04  & 9.0--9.7  &&$<$ 4.6 &$26\pm1$&(2)\\
 \object{HD~201219}    				   &      G5     &     5604   &  $-$0.16  & 9.0--9.7  && $<$4.1 &$36\pm2$&(2)\\
 \object{HD~206374}      			   &     G6.5V   &     5580   & $-$0.17 & 9.0--9.7 &&$<$3.9  &$27\pm1$&(2)\\
 \object{HD~38529}     				   &   G8III/IV  &     5361   &  0.82 & 9.0--9.7 & &$<$3.2  &$42\pm2$&(2)\\
 \object{HD~136923}     				   &      G9V    &     5343   &  $-$0.29  &9.0--9.7  && $<$3.2 &$20\pm1$&(2)\\    
 \object{HD~6963}      				   &      G7V    &     5517   &  $-$0.26  &9.0--9.7 && $<$4.2 &$27\pm1$&(2)\\
 \object{HD~122652}    				   &      F8     &     6157   &  0.18  &9.0--9.7 &$<$19.5&3.2  &$37\pm1$&(2)\\
 \object{HD~187897}    				   &      G5     &     5875   &  0.12  &9.0--9.7& &$<$2.4  &$33\pm1$&(2)\\        
\hline
\noalign{\smallskip}
\multicolumn{8}{c}{FEPS sources older than 10~Myr not included in the statistical analysis}   \\
 \object{HD~134319}			   &     G5(V)   &     5660   & $-$0.14  & 7.5--8.0  &$<$25.2&$<$8.5&$44\pm1$&(2)   \\ 
 {\bf \object{HD~191089}}		   &      F5V    &     6441   &  0.50 &   8.0--8.5   &$54\pm15$&$<$3.6  &$54\pm3$&(2)        \\
 \object{HD~25457}			   &      F7V    &     6172   &  0.32& 8.0--8.5 && $<$2.2 &$19\pm1$&(2)    \\
 {\bf \object{HD~8907}}			   &      F8     &     6250   & 0.32  & 8.5--9.0   &&$3.2\pm0.9$ &$34\pm1$&(2)\\
 \hline
 \noalign{\smallskip}
\multicolumn{8}{c}{FEPS sources younger than 10~Myr}   \\
\noalign{\smallskip}
 {{\bf  \object{[PZ99] J161411.0-230536}}}   &      K0     &     4963   &  0.50  & 6.5--7.0&$<$21.9&$3.5\pm1.1$  &$145\pm2$&(1) \\ 
 {\bf  \object{RXJ1612.6-1859a}}			   &     K0IV    &     5372   &  0.38  & 6.5--7.0&$43\pm8.7$&  $5.9 \pm1.4$&$145\pm2$&(1)   \\ 
 {\bf \object{HD~143006} }			   &     G6/8    &     5884   &  0.39  & 6.5--7.0&$1400 \pm39$  &&$145\pm2$&(1)  \\ 
 \object{SCOPMS214} 				   &     K0IV    &     5318   &  0.26  & 6.5--7.0& $<$72  &&$145\pm2$&(1)\\ 
 {\bf \object{RX J1842.9-3532}}                     &     K0IV    &     4995   &  $-$0.01 & 6.5--7.0 &$650\pm29$&&$130\pm10$&(3)  \\ 
 {\bf \object{RX J1852.3-3700} } 		   &      K3     &     4759   &  $-$0.23  & 6.5--7.0 &$1200 \pm45$ &&$130\pm10$&(3)   \\                                                       %     
 \object{HD~35850}   				   &     F7/8V   &     6047   &  0.25 &  7.0--7.5 &&$<$3.7  &$27\pm1$&(2)         \\
 \object{HE848}  				   &      F9V    &     6309   &  0.47 &  7.5--8.0   &&$<$3.1 &$176\pm5$&(4)  \\ 
 \object{HD~77407}   				   &     G0(V)   &     5986   &  0.08  & 7.5--8.0  & &$<$3.45  &$30\pm1$&(2)  \\
 \object{HD~22179}   				   &      G0     &     5986   &  0.36  & 7.5--8.0 & &$<$3.3  &$100\pm20$&(3)   \\
 \object{HD~12039}   				   &     G3/5V   &     5688   &  $-$0.05& 7.5--8.0 & &$<$2.7  &$42\pm2$ &(2)     \\ 
 \object{HD~70573}   				   &     G1/2V   &     5896   &  0.14&  7.5--8.0& &$<$2.73 & $46\pm15$&(3) \\
 \object{HE750}      				   &      F5     &     6421   &  0.28 & 7.5--8.0  &      &$<$4.60& $176\pm5$&(4)  \\
 \object{HD~135363}  				   &     G5(V)   &     4728   &  $-$0.48  &  7.5--8.0  &      &   $<$2.22   & $29\pm1$&(2)       \\
 \hline
 \noalign{\smallskip}
 \multicolumn{8}{c}{Not in the FEPS list}   \\
 \noalign{\smallskip}
  \object{HD~82943}  &&&&&&$<$27.9 &&     \\
  \object{HD~38207} 				   &      F2V    &     6769   &  0.72& 8.0--8.5  &&$<$0.33  &$127\pm25$&(3)  \\
 \object{HD~117176}&&&&&&$<$14.1& &  \\
 \object{HD~218738} &&&&&$<$21.9 &$<$3.3 & & \\
 \hline
\end{tabular}}
\smallskip
\noindent
 {$^{\star}$  The errors and the upper
limits refer to the statistical errors (flux rms) and do not include the calibration
uncertainty (between 12 and 22\% of the
    flux). $^{\star\star}$  The errors and the upper
limits refer to the statistical errors (flux rms) and do not include the calibration
uncertainty (between 11 and 16\% of
    the flux). 
Distance references: $^1$ de Zeeuw et~al.~(\cite{1999AJ....117..354D}); $^2$ Perryman et~al.~(\cite{Perrymanetal1997}); $^3$ Hillenbrand et~al.(\cite{Hillenbrandetal2008}); $^4$ Pinsonneault et~al.~(\cite{1998ApJ...504..170P}); $^5$~based on recent Pleiades distances: de Zeeuw et~al.~(\cite{1999AJ....117..354D}), Zwahlen et~al.~(\cite{2004A&A...425L..45Z}), Soderblom et~al.~(\cite{2004AAS...204.4507S}) and Pan et~al.~(\cite{2004Natur.427..326P}).}
\par
\end{table}