\begin{table}%t1
  \caption{\label{table:targets}Stellar parameters and known fluxes of our target sample.}
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  {\begin{tabular}{lccccrcrcrcccrr}
    \hline
    \hline\\[-3mm]
    Object     &  Class      &  Spectral type &  $T_{{\rm adopted}}$
               &  (log $g$)$_{{\rm adopted}}$&  $V$
               &  $F_{{\rm 12~\mu m}}$  
               &                Age           &  Ref.  & $d$       &  Ref.  
               &  $A_v$      &  Ref.          &  Sep.              &  Ref. \\
\par
               &             &                &  [K]
               &                              &  [mag]
               &  [Jy]                        
               &                [Myr]         &        &  [pc]     &       
               &  [mag]      &                &  [$''$]            &       \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    HD 3003    &  Vega       &  A0V           &  11~000
               &  4.5                         &  5.07
               &  0.48                        
               &      $\rm 50  _{- ...}^{+ 197}$  &  (1)   &  47       &  (9)  
               &  ...        &                &  0.1 (?)           &  (26) \\
\par
    HD 34~700 A &  TTS        &  G0IVe         &  6000
               &  4.5                         &  9.15
               &  0.60                        
               &                ...           &        &  ...      &  (10)  
               &  0.68       &  (19)          & SB~/~5.2~/~9.2 &  (27) \\
\par
    HD 80~951 A &  Vega       &  A1V           &  9500
               &  4.5                         &  6.00
               &  0.44
               &  ...                         &        &  220      &  (9)
               &  ...        &                &0.3~/~7.1~/~48.2&  (26) \\
\par
    HD 109~085  &  Vega       &  F2V           &  7000
               &  4.5                         &  4.31
               &  2.18                        
               &      $\rm 1000_{- 300}^{+ 300}$ &  (2)   &  18       &  (11)   
               &  0.12       &  (20)          &  ...               &       \\
\par
    HD 123~356 AB &  Vega     &  G1V~/~M?    &  6000 / 4000
               &  4.5                         &  10.0 / 12.2
               &  1.36                      
               &                ...           &        &  ...      &  (12)
               &  0.16       &  (20)          &  2.5               &  (28) \\
\par
    HD 143~006  &  TTS        &  G5Ve          &  5750
               &  4.5                         &  10.21
               &  0.86                        
               &                $\sim$1       &  (3)   &  82       &  (13) 
               &  0.62       &  (21)          &  ...               &       \\
\par
    HD 155~555 ABC &  TTS     & G5IV~/~K0IV-V~/~M4.5           &  5750 / ...
               &  4.5                         &  6.88 / 13.0
               &  0.69
               &        $\rm 12_{- 4}^{+ 8}$     &  (4)   &  32       &  (9)
               &  ...        &                &  SB~/~33.0       &  (26) \\
\par
    HD 181~296 A &  Vega      &  A0Vn          &  9500
               &  4.5                         &  5.03
               &  0.54
               &        $\rm 12_{- 4}^{+ 8}$     &  (4)   &  48       &  (9)
               &  0.12       &  (20)          &  4.1               &  (29) \\
\par
    HD 190~073  &  HAeBe      &  A2IIIpe       &  9500
               &  4.5                         &  7.82
               &  7.16                        
               &      $\rm 1.2_{- 0.6}^{+ 0.6}$  &  (5)   & $>$290   &  (14) 
               &  0.19       &  (19)          &  ...               &       \\
\par
    HD 319~139  &  TTS        &  K5Ve / K7Ve   &  4250
               &  4.5                         &  10.44
               &  0.45
               &       $\rm 5.5_{- 1.5}^{+ 1.5}$ &  (6)   &  83       &  (15)
               &  $\leq$0.12&  (22)          &  SB                &  (30) \\
\par
    CD-43 344  &  TTS (?)    &  M2            &  4500
               &  4.5                         &  9.42
               &  3.73                     
               &                ...           &        &  ...      &  (10)   
               &  0.0        &  (20)          &  ...               &       \\
\par
    FU Ori A   &  FUOR       &  G0II          &  ...
               &  4.5                         &  8.94
               &  5.95
               &                $<$0.3        &  (7)   & 450       &  (16)
               &  2.2        &  (23)          &  0.5               &  (31) \\
\par
    KK Oph A   &  HAeBe      & A6Ve           &  8750
               &  4.5                         &  9.4~--~12.9 
               &  9.87
               &         $\rm 7_{- 0.5}^{+ 1.0}$ &  (8)   & 160       &  (17)
               &  1.6        &  (24)          &  1.6               &  (32) \\
\par
    PDS 144 N  &  HAeBe      &  A2IV          &  8750
               &  4.5                         &  14.2
               &  ...
               &                ...           &        & $\sim$1000&  (18)
               &  3.0        &  (25)          &  $\sim$5.0         &  (33) \\
\par
    PDS 144 S  &  HAeBe      &  A5V           &  8750
               &  4.5                         &  13.1
               &  ...
               &                ...           &        & $\sim$1000&  (18)
               &  1.1        &  (25)          &  $\sim$5.0         &  (33) \\
  \noalign{\smallskip}
  \hline
  \end{tabular}}
\medskip
\par
           References: 
           Spectral types are obtained either from SIMBAD or one of the 
           cited papers, if a more accurate classification is available 
           in the literature. $T_{{\rm adopted}}$ and 
           (log~$g$)$_{{\rm adopted}}$ list the temperature and surface 
           gravity which we used for the Kurucz atmosphere models. 
           $V$-band magnitudes and IRAS 12~$\mu$m fluxes are 
           taken from the SIMBAD database. KK~Oph shows variability in 
           the visual. PDS~144 is not 
           resolved by IRAS; its $V$-band fluxes were given by Perrin et~al.\ (\cite{Perrin}).  Stellar ages: (1)~Song et~al.\ (\cite{Song01}), (2)~Wyatt et~al.\ (\cite{Wyatt}) and
           references therein, (3)~Dunkin et~al.\ (\cite{Dunkin}) and
           references therein, (4)~mean age of the $\beta$~Pic moving 
           group as given in Zuckerman \& Song 
           (\cite{Zuckerman01}), (5)~Catala et~al.\ (\cite{Catala}), 
           (6)~Quast et~al.\ (\cite{Quast}), (7)~e.g.\ D'Angelo et 
           al.\ (\cite{Angelo}), (8)~Carmona et~al.\ (\cite{Carmona}). 
           Errors in the age determinations are quite heterogeneous, 
           depending on the cited work. Distances are taken from 
           (9)~Hipparcos parallax, (10)~uncertain Hipparcos parallax, 
           (11)~Wyatt et~al.\ (\cite{Wyatt}), (12)~The Hipparcos parallax 
           was recently removed from SIMBAD and is likely not firm, 
           (13)~Sylvester et~al.\ (\cite{Sylvester96}), (14)~van den 
           Ancker et~al.\ (\cite{Ancker}), (15)~Quast et~al.\ (\cite{Quast}), 
           (16)~e.g.\ Wang et~al.\ (\cite{Wang}), (17)~Hillenbrand et 
           al.\ (\cite{Hillenbrand}), (18)~Perrin et~al.\ (\cite{Perrin}) 
           and references therein. Extinctions: (19)~van den Ancker 
           et~al.\ (\cite{Ancker}), (20)~Sylvester \& Mannings 
           (\cite{Sylvester00}), (21)~Malfait et~al.\ (\cite{Malfait98}), 
           (22)~Hutchinson et~al.\ (\cite{Hutchinson}), (23)~Kenyon et 
           al.\ (\cite{Kenyon88}), (24)~Carmona et 
           al.\ (\cite{Carmona}), (25)~Perrin et~al.\ (\cite{Perrin}).
           Stellar separations in multiple systems: (26)~Dommanget
           \& Nys (\cite{Dommanget}), (27)~Sterzik et~al.\ (\cite{Sterzik}),
           (28)~Worley \& Douglass (\cite{Worley}), (29)~Lowrance et
           al.\ (\cite{Lowrance}), (30)~Quast et~al.\ (\cite{Quast}),
           (31)~Wang et~al.\ (\cite{Wang}), (32)~Leinert et 
           al.\ (\cite{Leinert97}), (33)~Perrin et~al.\ (\cite{Perrin}).
           ``SB'' denotes a spectroscopic binary. Note on the multiplicity
           of HD~155~555: Although the SB components are not spatially 
           resolved, we label them as A and B, since this naming convention
           existed already in the literature.
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\end{table}