\begin{table}%t1
\par
\caption{\label{table:1}Observing log with stellar properties and integration times.}
\small%\centering
\par
\begin{tabular}{l l c c c c c c c}
\hline\hline\noalign{\smallskip}
Object ID & Name & RA\tablefootmark{a} & Dec. & Spectral type\tablefootmark{b} & Age$^{{\rm upper}}_{{\rm lower}}$ & Reference & Distance\tablefootmark{c} & Integration time\\
 &  & (h m s) & ($\degr$ $\arcmin$ $\arcsec$) &  & (Myr) &  & (pc) & (min) \\
\hline
\object{HD~105} &  & 00 05 52.54 & $-$51 45 11.0 & G0V & $30^{\rm 3500}_{27}$ & 1, 2, 27 & 40 & 104 \\
\par
\object{HD~17390} &  & 02 46 45.10 & $-$21 38 22.3 & F3IV/V & $300^{\rm 800}_{?}$ & 3, 4 & 45 & 24 \\
\par
\object{HD~21997} &  & 03 31 53.65 & $-$25 36 50.9 & A3IV/V & $50^{\rm 150}_{200}$ & 5, 3, 6 & 74 & 52 \\
\par
\object{HD~25457} &  & 04 02 36.74 & $-$00 16 08.1 & F5V\tablefootmark{d} & $50^{\rm 150}_{30}$ & 7 & 19 & 97 \\
\par
\object{HD~30447} &  & 04 46 49.53 & $-$26 18 08.8 & F3V & $20^{\rm 100}_{10}$ & 6, 8 & 78 & 65 \\
\par
\object{HD~31392} &  & 04 54 04.21 & $-$35 24 16.3 & K0V & $1300^{\rm 4000}_{400}$ & 9 & 26 & 53 \\
\par
\object{HD~32297} &  & 05 02 27.44 & +07 27 39.7 & A0V & $30^{\rm 50}_{20}$ & 10 & 112 & 39 \\
\par
\object{HD~61005} &  & 07 35 47.46 & $-$32 12 14.0 & G8V & $180^{\rm 320}_{100}$ & 11 & 35 & 53 \\
\par
\object{HD~78702} &  & 09 09 04.21 & $-$18 19 42.8 & A0/A1V & $220^{\rm 320}_{80}$ & 6 & 80 & 91 \\
\par
\object{HD~95086} &  & 10 57 03.02 & $-$68 40 02.4 & A8III & $20^{\rm 50}_{15}$ & 12, 13, 14 & 92 & 32 \\
\par
\object{HD~98800} & TV~Crt & 11 22 05.29 & $-$24 46 39.8 & K5V+K7V+M1V+?\tablefootmark{e} & $10^{\rm 20}_{3}$ & 15 & 47 & 62 \\
\par
\object{HD~109573} & HR~4796 & 12 36 01.03 & $-$39 52 10.22 & A0V+M2.5\tablefootmark{f} & $10^{\rm 20}_{4}$ & 16, 17, 18 & 67 & 185 \\
\par
\object{HD~131835} &  & 14 56 54.47 & $-$35 41 43.6 & A2IV & $14^{\rm 18}_{10}$ & 8, 6 & 111 & 145 \\
\par
\object{HD~139664} &  & 15 41 11.38 & $-$44 39 40.3 & F4V & $200^{\rm 300}_{150}$ & 7 & 18 & 170 \\
\par
\object{HD~141569} &  & 15 49 57.75 & $-$03 55 16.4 & A0Ve+M2+M4\tablefootmark{g} & $5^{\rm 8}_{2}$ & 19, 26 & 99 & 206 \\
\par
\object{HD~152404} & AK~Sco & 16 54 44.85 & $-$36 53 18.6 & F5V+F5V\tablefootmark{h} & $17^{\rm 18}_{16}$ & 20 & 145 & 127 \\
\par
\object{HD~161868} & $\gamma$~Oph & 17 47 53.56 & +02 42 26.2 & A0V & $180^{\rm 190}_{170}$ & 16, 17 & 29 & 218 \\
\par
\object{HD~164249} &  & 18 03 03.41 & $-$51 38 56.4 & F5V & $12^{\rm 20}_{8}$ & 21 & 47 & 166 \\
\par
\object{HD~170773} &  & 18 33 00.92 & $-$39 53 31.3 & F5V & $200^{\rm 300}_{150}$ & 3, 5 & 36 & 311 \\
\par
\object{HD~193307} &  & 20 21 41.03 & $-$49 59 57.9 & G0V & $5700^{\rm 6300}_{5100}$ & 22, 27 & 32 & 90 \\
\par
\object{HD~195627} &  & 20 35 34.85 & $-$60 34 54.3 & F0V & $30^{\rm 230}_{10}$ & 3, 12 & 28 & 98 \\
\par
\object{HD~207129} &  & 21 48 15.75 & $-$47 18 13.0 & G2V & $3000^{\rm 8000}_{10}$ & 5, 22, 24, 25, 27 & 16 & 354 \\
\noalign{\smallskip}\hline
\end{tabular}
\tablefoot{
\tablefoottext{a}{Positions are from the Hipparcos Catalogue \citep{Perryman1997}.}
\tablefoottext{b}{Spectral types are from \citet{Torres2006,Thoren2000,Manoj2006,Thevenin1999}.}
\tablefoottext{c}{Distances are from the Hipparcos Catalogue \citep{Perryman1997}}
\tablefoottext{d}{From \citet{Lopez2006}. Marked as T Tau-type in SIMBAD astronomical database.}
\tablefoottext{e}{Quadruple system composed of two spectroscopic binaries, Aa+b and Ba+b, separated by 0$\farcs$848 \citep{Prato2001}. IR excess originates from the Ba+b (K7+M1V binary) component (for which the coordinates are given) \citep[see][and references therein]{Laskar2009}.}
\tablefoottext{f}{Binary system with the secondary (M2.5 pre-main-sequence) star located 7$\farcs$7 to the southwest of the primary (A0V). IR excess comes from HD~109573A (also designated HR~4796A or GQ~Lup) with an imaged circumstellar ring \citep{Schneider2009}.}
\tablefoottext{g}{Primary component HD~141569A, which is possibly still in its pre-main-sequence stage, has a binary companion consisting of two M stars at $\sim8\arcsec$ separation. The double pair could be unbound and merely flying by \citep{Reche2009}.}
\tablefoottext{h}{Spectroscopic binary with high IR excess attributed to long-lived primordial, circumbinary disk \citep{Uzpen2007,Gomez2009}.}
} 
\tablebib{
(1)~\citet[][]{Hollenbach2005} and references therein; (2)~\citet{Apai2008}; (3)~\citet{Zuckerman2004b}; (4)~\citet{Zuckerman2004a};
(5)~\citet{Song2003}; (6)~\citet{Moor2006}; (7)~\citet[][]{Lopez2006} and references therein; (8)~\citet[][]{Rhee2007} and references therein;
(9)~\citet[][]{Carpenter2009} and references therein; (10)~\citet{Perryman1997}; (11)~\citet{Roccatagliata2009}; (12)~\citet{Lowrance2000};
(13)~\citet{deZeeuw1999}; (14)~\citet{Mamajek2002}; (15)~\citet{Barrado2006}; (16)~\citet{Song2001}; (17)~\citet{Rieke2005};
(18)~\citet{Stauffer1995}; (19)~\citet{Weinberger2000}; (20)~\citet[][]{Chen2005b} and references therein; (21)~\citet{Zuckerman2001a};
(22)~\citet{Mamajek2008}; (23)~\citet{Henry1996}; (24)~\citet[][]{Bryden2006} and references therein; (25)~\citet{Zuckerman2000};
(26)~\citet{Merin2004}; (27)~\citet{Valenti2005}.
}
\end{table}