\begin{table}%t1
\caption{Basic parameters of the sample stars. In
Cols.~~1 and~2 we give the index number by which a star can be
identified in tables and figures throughout this work, and the name of
the star, respectively.  The classification of the sources according
to ME01 is listed in the third column.  In Col.~~5 the distances,
derived from direct (Hipparcos) parallax measurements or by
association to a star forming region (SFR, Col.~4), are given.
For the stars where the distance is determined by association with
a SFR we assume an error of~30\% in the distance.
The
spectral type according to the MK classification, the effective
temperature and the stellar luminosity are given in Cols.~~6--8, respectively.  Mass and age estimates for most stars, as
derived by comparing their positions in the HR diagram to theoretical
pre-main-sequence tracks, are given in Cols.~9 and~10.
For HD~101412 we have no reliable distance estimate, and can therefore
not determine its luminosity, mass and age.\label{tab:t2_fs:source_list}}
%\par
%\linespread{1.1}
%\selectfont
%\par
%\centerline
\begin{tabular}{rlrlllcccc}
\hline\hline
(1) & \ \ \ \ (2) & \ \ (3) & \ (4) & \ (5) & \ \ (6) \ & \ \ (7) & \ (8) & \ (9)  & (10) \\
\#  & \ \ \ \ Star&Group   &  {\it SFR}       &  $d$    &  Sp. type  &  log ${T_{\rm eff}}$ & log $L$       & Mass       &  log(age)     \\ % Remarks                   &
  &             &   &            & [pc]  &           &      [K]   &     [\lsun] & [\msun]     &      [yr]     \\ %                           &
\hline
  1 &    AB Aur       & Ia  & L519       &$  144_{\rm -   17}^{ +   22} $ & A0Ve+sh     & 3.979 &   1.67   &     2.4~$\pm$~0.2  &  6.3~$\pm$~0.2  \\ %                           &
  2 &    UX Ori       &IIa  & Orion OB1a &$  340\pm  102$              & A4IVe       & 3.925 &   1.68   &     2.5~$\pm$~0.3  &  6.3~$\pm$~0.4  \\ %                           &
%   & HD~34282       & Ib  &            &$  400\pm  120$              & A3Vne       & 3.941 &   1.27   &     2.0~$\pm$~0.3  & $>$6.5        \\ %                           &
  3 & HD~36112       & Ia  &            &$  204_{\rm -   39}^{ +   63} $ & A5IVe       & 3.911 &   1.35   &     2.0~$\pm$~0.3  &  6.5~$\pm$~0.3  \\ %                           &
  4 &    HK ORI       &IIa  & Orion OB1a &$  340\pm  102$              & A4pevar     & 3.927 &   0.87   &     1.7~$\pm$~0.3  & $>$6.8        \\ %                           &
%   & HD~36917       &IIa  & Orion OB1c &$  510\pm  153$              & A0Ve        & 3.978 &   2.13   &     3.3~$\pm$~0.3  &  5.8~$\pm$~0.4  \\ %                           &
  5 & HD~245185      & Ia  & Orion OB1a &$  340\pm  102$              & A0Ve        & 3.979 &   1.26   &     2.2~$\pm$~0.3  & $>$6.8        \\ %                           &
% 6 & HD~36910       & Ia  & Tau T4     &$   99_{\rm -   16}^{ +   24}   & F5IVe       & 3.810 &   0.01   &     1.1~$\pm$~0.3  & $>$7.0        \\ %                           &
  6 &    V380 Ori     &IIa  & Orion OB1c &$  510\pm  153$              & A1:e        & 3.965 &   1.88   &     2.8~$\pm$~0.5  &  6.2~$\pm$~0.4  \\ %                           &
  7 & HD~37357       &IIa  &            &$  240\pm   72^1$            & A2Ve        & 4.021 &   1.47   &     2.4~$\pm$~0.4  & $>$7.0        \\ % put at 240 pc (30 Lsun, from spectral type) instead of 510 (Orion OB1c) &
  8 & HD~37806       &IIa  & Orion OB1b &$  470\pm  141$              & A2Vpe       & 3.953 &   2.13   &     3.6~$\pm$~0.8  &  5.9~$\pm$~0.4  \\ %                           &
%   &   BET PIC       &  ~  &            &$   19_{\rm -    0}^{ +    0}   & A5V         & 3.914 &   0.94   &     1.7~$\pm$~0.1  &  7.3$\pm$0.1  \\ % Barrado y Navascues et a  &
%   & HD~41511       &IIa  &            &$  327_{\rm -   59}^{ +   92}   & A1Ve+M3III  & 3.965 &   3.21   &                  &               \\ % Symbiotic Star            &
%   & HD~45677       &  ~  &            & >300                        & B2III-V[e]  & 4.325 &  >2.60   &    $>$4.0        &               \\ % No dist. known            &
%   & HD~50138       &  ~  &            &$  289_{\rm -   54}^{ +   86}   & B5V[e]      & 4.188 &   2.85   &     5.0$\pm$1.0  &               \\ %                           &
%   & HD~85567       &IIa  &            & >480                        & B7-8Ve      & 4.095 &  >2.54   &    $>$4.0        &               \\ %                           &
  9 & HD~95881       &IIa  & Sco OB2-4? &$  118\pm   35$              & A2III/IVe   & 3.954 &   0.88   &     1.7~$\pm$~0.2  & $>$6.5        \\ %                           &
  10& HD~97048       & Ib  & Ced 111    &$  175_{\rm -   20}^{ +   26} $ & B9.5Ve+sh   & 4.000 &   1.64   &     2.5~$\pm$~0.2  & $>$6.3        \\ %                           &
%   & HD~98922       &IIa  &            & >540                        & B9Ve        & 4.021 &  >2.96   &    $>$5.0        &               \\ % No dist. known            &
  11& HD~100453      & Ib  &            &$  111_{\rm -    8}^{ +   10} $ & A9Ve        & 3.869 &   0.90   &     1.7~$\pm$~0.2  &  7.0~$\pm$~0.1  \\ %                           &
  12& HD~100546      & Ia  & Sco OB2-4? &$  103_{\rm -    6}^{ +    6} $ & B9Vne       & 4.021 &   1.51   &     2.4~$\pm$~0.1  & $>$7.0        \\ %                           &
  13& HD~101412      &IIa  &            &                             & B9.5V       &       &          &                  &               \\ % No dist. known            &
  14& HD~104237      &IIa  & Cha III    &$  116_{\rm -    6}^{ +    7} $ & A4IVe+sh    & 3.925 &   1.54   &     2.3~$\pm$~0.1  &  6.3~$\pm$~0.1  \\ %                           &
%   & HR 4796         &  ~  &            &$   67_{\rm -    3}^{ +    3} $ & A0V         & 3.979 &   1.39   &     2.2$\pm$0.1  &  7.0$\pm$0.2  \\ %                           &
  15& HD~135344      & Ib  & Sco OB2-3  &$  140\pm   42$              & F4Ve        & 3.819 &   0.91   &     1.6~$\pm$~0.2  &  6.9~$\pm$~0.3  \\ %                           &
  16& HD~139614      & Ia  & Sco OB2-3  &$  140\pm   42$              & A7Ve        & 3.895 &   0.91   &     1.7~$\pm$~0.3  & $>$7.0        \\ %                           &
%   & HD~140863      &  ~  &            &                             & A0III/IV    & 3.998 &          &                  &               \\ % No. dist. known           &
%   & HD~141569      &  ~  & (L169)     &$   99_{\rm -    7}^{ +    8} $ & A0Ve        & 3.979 &   1.28   &     2.3~$\pm$~0.1  & $>$7.0        \\ %                           &
  17& HD~142666      &IIa  & Sco OB2-2  &$  145\pm   43$              & A8Ve        & 3.880 &   1.13   &     1.8~$\pm$~0.3  &  6.8~$\pm$~0.4  \\ %                           &
  18& HD~142527      & Ia  &            &$  198_{\rm -   37}^{ +   60} $ & F7IIIe      & 3.796 &   1.46   &     2.5~$\pm$~0.3  &  6.0~$\pm$~0.4  \\ % put at 200 (hipparcos) instead of 145 (association with Sco OB2-2) &
% % & HD~143006      & Ia  & Sco OB2-2  &$  145\pm   43$              & G5Ve        & 3.750 &   0.23   &     1.2$\pm$0.2  &  7.2$\pm$0.2  \\ %                           &
  19& HD~144432      &IIa  & Sco OB2-2  &$  145\pm   43$              & A9IVev      & 3.866 &   1.01   &     1.8~$\pm$~0.2  &  7.0~$\pm$~0.3  \\ % Perez et~al. 2004         &
  20& HD~144668      &IIa  & Lupus 3    &$  207_{\rm -   31}^{ +   45} $ & A5-7III/IVe & 3.899 &   1.94   &     3.2~$\pm$~0.5  &  5.7~$\pm$~0.3  \\ %                           &
  21& HD~150193      &IIa  & Sco OB2-2  &$  150_{\rm -   30}^{ +   50} $ & A2IVe       & 3.953 &   1.38   &     2.3~$\pm$~0.2  & $>$6.3        \\ %                           &
%   & CD-42 11721     &  ~  &            &$  400\pm  120$              & B0IVep      & 4.470 &   3.94   &     12 $\pm$3    & $>$5.0        \\ %                           &
%   &   51 OPH        &IIa  &            &$  130_{\rm -   13}^{ +   16} $ & B9.5Vne     & 4.000 &   2.39   &                  &               \\ % Evolved Star?             &
  22& HD~163296      &IIa  &            &$  122_{\rm -   13}^{ +   16} $ & A3Ve        & 3.941 &   1.38   &     2.0~$\pm$~0.2  &  6.7~$\pm$~0.4  \\ %                           &
  23& HD~169142      & Ib  & Sco OB2-1  &$  145\pm   43$              & A5Ve        & 3.914 &   1.16   &     2.0~$\pm$~0.3  &  6.9~$\pm$~0.3  \\ %                           &
%   &    R CRA        &  ~  & NGC 6729   &$  130\pm   39$              & A1-F7Ve     & 3.86: &   0.19   &     1.2$\pm$0.5  & $>$7.0        \\ %                           &
%   &    T CRA        & Ia  & NGC 6729   &$  130\pm   39$              & F0e         & 3.857 &  -0.18   &     0.8$\pm$0.5  & $>$7.0        \\ %                           &
  24& HD~179218      & Ia  & (L693)     &$  243_{\rm -   43}^{ +   68} $ & B9e         & 4.021 &   2.00   &     2.9~$\pm$~0.5  &  6.1~$\pm$~0.4  \\                          
\hline
\end{tabular}
\par
$^1$ We adopted a distance of 240 pc so that the luminosity of this star matches its spectral type.
\end{table}