\begin{table}
%\centering
\par
\caption{\label{tab:lc}The most frequently observed asteroids by SDSS that have known lightcurves from the independent study elsewhere.}
\begin{tabular}{rllclc}
\hline\hline \noalign{\smallskip}
\multicolumn{2}{c}{Asteroid} & $U$ & LC & $N$ & Analysed\\
\hline
   (728) & Leonisis        &3  & 2007  &  17 (15)& yes\\
  (1534) & N\"asi          &3-- & 2007  & 15 (12)& yes\\
  (1829) & Dawson          &2  & 2002&\\
  (1829) & Dawson          &3  & 2005& 8 (7)& yes\\
  (1829) & Dawson          &3  & 2007&\\
  (2453) & Wabash          &3  & 2005  & 14 (11)& yes\\
  (2659) & Millis          &3  & 1991  & 11 (10)& yes\\
  (2903) & Zhuhai          &2  & 2000  & 10 (8)&no \\
  (4467) & Kaidanovskij    &1  & 2005  & 14 (13)& no\\
  (5288) & Nankichi        &2  & 2007  & 10 (9) &no \\
  (5448) & Siebold         &3  & 2007  & 10 (9) & no \\
  (7760) & 1990 RW$_3$        &3  & 2005  & 8 (8) & yes\\
  (8405) & Asbolus         &2  & 1996 &  \\
  (8405) & Asbolus         &3  & 1997 &  \\
  (8405) & Asbolus         &3  & 2005 & 14 (12)& yes \\
  (9368) & Esashi          &3  & 2007  &  10 (10)& yes\\
 (16706) & Svojs\'ik       &1  & 2003  & 10 (9) & no \\
 (30825) & 1990 TG$_1$        &3  & 2005  & 10 (9) & yes\\
 (35690) & 1999 CT$_{21}$       &2  & 2000  & 14 (14) &yes \\
\hline
\end{tabular}
\tablefoot{$U$ is the index of quality for rotation period determination,
LC denotes the year at which the best lightcurve was obtained,  $N$ is the number of (reliable) SDSS observations in 2005.}
\end{table}