\begin{table}%t2
\par
\caption {\label{table:candidates}Characteristics of the 27 microlensing candidates.
For those events that have a better fit than the point-like point-source constant speed
microlensing fit (the so-called standard fit), we also provide the standard
fit parameters.
}
%\centerline
 { %\scriptsize
\begin{tabular}{ccc cccccccc}
\hline    \hline
Candidate & Field & \multicolumn{2}{c}{$\alpha ^{\circ},~~\delta ^{\circ}~(J2000)$} & $I_C$ ($V_J-I_C$) & $t_0$ (days) & $t_{\rm E}$ (days) & $u_0$ & $\chi^2/\rm d.o.f$ & $\tau (10^{-6})$ & Note \\ 
\hline
\multicolumn{10}{c}{\boldmath $\gsct$} & \\
 {\bf GSA1}    & 200 & 277.2888	& --14.2528   & 18.3 (3.1) & 301.2 $\pm$ 0.1 &  64.0 $\pm$ 1.2 & .043 $\pm$ .0010& 299.7/435& 0.146 &  \\
% GSA8    & 200 & 18:27:13.0 & -15:01:52   & 16.4 (3.6) & 3097.3$\pm$ 1.2 &  37.7$\pm$ 1.6 & .000$\pm$*****& 778.7/540& XXXXX & (3) \\
 {\bf GSA8}    & 200 & 276.8042	& --15.0311  & 16.6 (3.7) & 996.9 $\pm$ 0.1 &  40.6 $\pm$ 1.0 & .145 $\pm$ .003& 981./533& 0.114 & (1) \\
	 & & & \multicolumn{2}{r}{Standard fit parameters:}  & 993.0 $\pm$ 0.1 &  35.2 $\pm$ 0.7 & .155 $\pm$ .002 & 1400./535& & \\
 {\bf GSA9}    & 200 & 277.1750	& --15.1644 & 18.8 (2.8) & 1760.3 $\pm$ 1.7 &  57.9 $\pm$ 3.6 & .482 $\pm$ .0158& 262.9/565& 0.142 & \\
 {\bf GSA10}   & 200 & 277.2813	& --14.8931 & 18.1 (2.3) & 1806.1 $\pm$ 0.8 &  24.6 $\pm$ 1.3 & .574 $\pm$ .0179& 237.9/596& 0.081 & \\
 {\bf GSA11}   & 201 & 278.1650	& --14.1094 & 18.8 (2.5) & 1725.3 $\pm$ 0.4 &  44.3 $\pm$ 1.4 & .187 $\pm$ .0049& 367.2/558& 0.116 & \\
 {\bf GSA12}   & 203 & 278.5875	& -13.9794 & 17.1 (1.8) & 1378.6 $\pm$ 0.2 &  50.1 $\pm$ 0.7 & .225 $\pm$ .0030&  89.3/359& 0.123 & \\
 GSA13   & 203 & 278.9404	& --14.5803 & 17.2 (1.9) & 
 313.9 $\pm$ 1.2 &  37.2 $\pm$ 2.1 & .898 $\pm$ .0153& 244.9/617& -- & \\
 GSA14   & 204 & 278.4388	& --12.8678 & 16.7 (2.2) & 1637.7 $\pm$ 3.4 &  68.4 $\pm$ 3.7 & .785 $\pm$ .0097& 421.2/392& -- & (2) \\
\hline
\multicolumn{10}{c}{\boldmath $\bsct$} & \\
 {\bf GSA15} & 301 & 281.0654	& --6.0339 & 18.3 (3.5) & 1399.8 $\pm$ 1.4 &  72.2 $\pm$ 2.8 & .337 $\pm$ .0126& 212.2/411& 0.110 & edge\\
 GSA16   & 301 & 280.7646	& --6.7583 & 16.4 (3.1) & 1997.0 $\pm$ 3.2 &  60.6 $\pm$ 4.0 & .796 $\pm$ .0141& 341.8/361& -- & \\
 {\bf GSA17}   & 302 & 281.3950	& --7.8867 & 16.4 (1.7) & 1947.2 $\pm$ 3.8 &  50.0 $\pm$ 2.4 & .532 $\pm$ .1079& 156.9/400& 0.096 & \\
 {\bf GSA18}   & 304 & 282.2879	& --7.2500 & 16.1 (2.1) & 1718.7 $\pm$ 0.1 &  55.0 $\pm$ 2.0 & .137 $\pm$ .0009& 133./514& 0.098 & (3) \\
	 & & & \multicolumn{2}{r}{Standard fit parameters:} & 1718.4 $\pm$ 0.1 &  58.0 $\pm$ 0.3 & .137 $\pm$ .0009& 155.6/516& & \\
\hline
\multicolumn{10}{c}{\boldmath $\gnor$} & \\
 {\bf GSA2}    & 400 & 242.9592	& --52.9464 & 18.6 (2.3) & 534.4 $\pm$ 0.2 & 98.3 $\pm$ 0.9 & .342 $\pm$ .002& 973.4/934 & 0.059 & (4) \\
         & & & \multicolumn{2}{r}{Standard fit parameters:} & 533.6 $\pm$ 0.5 & 137.8 $\pm$ 2.6 & .233 $\pm$ .0029&1196.5/937& & \\
{\bf  GSA19}   & 401 & 244.1379	& --52.0272 & 15.5 (5.1) & 2367.7 $\pm$ 1.3 &  90.4 $\pm$ 3.0 & .043$\pm$ .025 &893./880& 0.063 & (5) \\
%	 & & & \multicolumn{2}{|r|}{Standard fit parameters:}& 4481.2$\pm$ 0.1 &  91.3$\pm$ 0.7 & .000$\pm$ .5356&1462.5/888& & \\
	 & & & \multicolumn{2}{r}{Standard fit parameters:}& 2373.5 $\pm$ 0.1 &  93.1 $\pm$ 0.7 & .022 $\pm$ .007&1388.5/888& & \\
% GSA20   & 402 & 16:15:06.2 & -52:58:12 & 16.3 (1.3) & 4594.6$\pm$ 0.3 &  46.3$\pm$ 0.7 & .565$\pm$ .0050& 712.4/698& XXXXX & (2) \\
 {\bf GSA20}   & 402 & 243.7758	& --52.9700 & 16.4 (1.3) & 2465.5 $\pm$ 1.0 &  40.$\pm$ 5.0 & .72 $\pm$ .02& 414./696& 0.039 & (6) \\
	 & & & \multicolumn{2}{r}{Standard fit parameters:} & 2487.1$\pm$ 0.3 &  46.3 $\pm$ 0.7 & .565$\pm$ .0050& 712.4/698& & \\
% GSA21   & 404 & 16:17:13.5 & -53:06:36 & 16.7 (2.5) & 3694.7$\pm$ 0.0 &  39.1$\pm$ 0.2 & .037$\pm$ .0007&1884.4/567& XXXXX & (3) \\
 {\bf GSA21}   & 404 & 244.3063	& --53.1100 & 16.8 (2.7) & 1587.3 $\pm$ .03 &  74. $\pm$ 3.0 & .0142 $\pm$ .0008&259./565& 0.077 & (7) \\
	 & & & \multicolumn{2}{r}{Standard fit parameters:} & 1587.2 $\pm$ .03 &  39.1 $\pm$ 0.2 & .037 $\pm$ .0007&1884.4/567& & \\
 {\bf GSA22}   & 404 & 244.4263	& --54.0508 & 18.4 (2.0) & 2182.4 $\pm$ 0.2 &  26.6 $\pm$ 1.1 & .048 $\pm$ .0180& 429.5/742& 0.031 & \\
 {\bf GSA23}   & 404 & 245.1208	& --53.9825 & 18.3 (1.7) & 1573.8 $\pm$ 3.8 &  78.5 $\pm$ 5.7 & .542 $\pm$ .0152& 522.3/784& 0.062 & corner\\
 GSA24   & 406 & 246.5442	& --54.0394 & 18.0 (1.9) & 2002.5 $\pm$ 1.4 &  55.5 $\pm$ 2.6 & .720 $\pm$ .0158& 579.4/786& -- & \\
 {\bf GSA25}   & 408 & 247.6917	& --53.9281 & 21.1 (1.4) & 850.9 $\pm$ .03 &  67.6 $\pm$ 2.9 & .003 $\pm$ .0001& 876.2/771& 0.057 & (8) \\
 {\bf GSA3}    & 409 & 244.1129	& --54.6303 & 17.7 (1.4) & 696.0 $\pm$ 2.0 &  60.4 $\pm$ 3.0 & .615 $\pm$ .0102& 606.7/1090& 0.051 & \\
 {\bf GSA26}   & 411 & 241.8729	& --55.3814 & 17.8 (2.2) & 1642.1 $\pm$ 0.3 &  23.2 $\pm$ 0.8 & .504 $\pm$ .0138& 441.5/759& 0.030 & \\
 {\bf GSA27}   & 411 & 242.4846	& --55.2292 & 18.3 (1.7) & 2193.8 $\pm$ 0.1 &   6.8 $\pm$ 0.4 & .210 $\pm$ .0068& 433.6/831& 0.022 & \\
\hline
\multicolumn{10}{c}{\boldmath $\tmus$} & \\
 {\bf GSA28}   & 501 & 202.2838	& --64.2750 & 19.3 (3.7) & 1992.2 $\pm$ 0.4 &  205. $\pm$ 20.0 & .029 $\pm$ .004& 717/499& 0.431 & (9) \\
	 & & & \multicolumn{2}{r}{Standard fit parameters:} & 1992.0 $\pm$ 0.4 &  87.3 $\pm$ 3.0 & .094 $\pm$ .0046& 868.5/500& & \\
 {\bf GSA29}   & 502 & 204.0683	& --63.7117 & 19.3 (2.5) & 1229.7 $\pm$ 0.3 &  74.2 $\pm$ 2.7 & .082 $\pm$ .0042& 161.7/354& 0.166 & \\
 {\bf GSA30}   & 505 & 199.2942	& --64.2592 & 16.5 (2.7) & 2396.9 $\pm$ 0.1 &  12.4 $\pm$ 0.2 & .062 $\pm$ .0023& 792.0/856& 0.073 & \\
\hline
\hline
\multicolumn{10}{c}{\bf{Uncertain candidate}} & \\
{\it GSAu1}   & 202 & 278.0371	& --13.2851 & 18.1 (2.9) & 1695.8$\pm$ 6.9 & 409.3 $\pm$ 20.9 & .708 $\pm$ .0155& 426.9/613& -- & \\
\hline
\end{tabular}}
\smallskip
  -- Names in bold type correspond to events selected for the optical depth
and duration analysis (with $u_0<0.7$).
\newline
-- $I_C$ ($V_J-I_C$) are the fitted unmagnified magnitudes of the lensed object
(including the contribution of a possible blend).
\newline
%Fit combine sans tenir compte du blend 
-- $t_0$ is the time of maximum magnification, given in HJD-2~450~000.
\newline
-- $t_{\rm E}$ is the Einstein disk crossing time, in days.
\newline
-- $u_0$ is the dimensionless impact parameter.
\newline
-- $\chi^2/\rm d.o.f.$ corresponds to the best microlensing fit.
\newline
-- $\tau$ is the individual contribution of each event to the optical depth
towards the corresponding target.
In the case of ``non standard'' events, we use the $t_{\rm E}$ value
obtained from the best (non standard) fit
and the efficiency evaluated at $t_{\rm E}$ of the standard fit (see text)
for the calculation of~$\tau$.
\par
{\bf Notes:}
%\newline
{\bf (1) GSA8}: Blended; $C_R=1.00\pm 0.03,\ C_B=0.68 \pm 0.02$; lensed star has $I_C^*\ (V_J^*-I_C^*)=16.6\ (4.4)$.
{\bf (2) GSA14}: light curve exhibits typical features of a binary lens system.
Given the small number of measurements with significant magnification,
no reliable analysis of the shape can be performed.
{\bf (3) GSA18}: parallax; projected Einstein radius in the solar plane $\tilde{r}_{\rm E}=12.5\pm 7.0 ~\rm AU$.
{\bf (4) GSA2}: described in Paper~I. Found
at that time as the first candidate for a binary lensed source (Xallarap).
{\bf (5) GSA19}: Xallarap and blend; the best fit is performed ignoring
the 3 most magnified measurements, that are affected by the non-linearity of the CCD.
$\ C_R=1.,\ C_B=0.160\pm 0.013$; lensed star has $I_C^*\ (V_J^*-I_C^*)=15.5\ (8.4)$.
The light curve distorsion could be due to the face-on circular orbiting of
the source around the center-of-mass of a system including
a non luminous object, with period $P_0=294.\pm 47.~\rm  days$,
and with a projected orbit radius of $\rho=ax/R_{\rm E}=0.081\pm 0.023$,
where~$a$ is the orbit radius and $x=D_{\rm lens}/D_{\rm source}$.
See also text.
{\bf (6) GSA20}: parallax; $\tilde{r}_{\rm E}=0.94\pm 0.07 ~\rm AU$.
{\bf (7) GSA21}: blended; $C_R=0.53\pm 0.02,\ C_B=0.34\pm 0.02$; lensed star has $I_C^*\ (V_J^*-I_C^*)=17.5\ (3.5)$.
{\bf (8) GSA25}: an improbable configuration, but a genuine one (very small $u_0$ on a very faint star).
{\bf (9) GSA28}: blended; $C_R=0.30\pm 0.03,\ C_B=1$; lensed star has $I_C^*\ (V_J^*-I_C^*)=20.6\ (1.5)$.
The $\chi^2/\rm d.o.f.$ of the fit is affected by
an underestimate of the errors due to bright neighboring stars.
\par
\end{table}