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Home All issues Volume 500 / No 3 (June IV 2009) A&A, 500 3 (2009) 1027-1044 Full HTML
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Table 2:

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.
Candidate Field $\alpha ^{\circ},~~\delta ^{\circ}~(J2000)$ IC (VJ-IC) t0 (days) $t_{\rm E}$ (days) u0 $\chi^2/\rm d.o.f$ $\tau (10^{-6})$ Note
$\gamma \ {\rm Sct} $  
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 200 276.8042 -15.0311 16.6 (3.7) 996.9 $\pm$ 0.1 40.6 $\pm$ 1.0 .145 $\pm$ .003 981./533 0.114 (1)
      Standard fit parameters: 993.0 $\pm$ 0.1 35.2 $\pm$ 0.7 .155 $\pm$ .002 1400./535    
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  
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  
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  
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)
$\beta \ {\rm Sct} $  
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 -  
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  
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)
      Standard fit parameters: 1718.4 $\pm$ 0.1 58.0 $\pm$ 0.3 .137 $\pm$ .0009 155.6/516    
$\gamma \ {\rm Nor} $  
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)
      Standard fit parameters: 533.6 $\pm$ 0.5 137.8 $\pm$ 2.6 .233 $\pm$ .0029 1196.5/937    
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)
      Standard fit parameters: 2373.5 $\pm$ 0.1 93.1 $\pm$ 0.7 .022 $\pm$ .007 1388.5/888    
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)
      Standard fit parameters: 2487.1$\pm$ 0.3 46.3 $\pm$ 0.7 .565$\pm$ .0050 712.4/698    
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)
      Standard fit parameters: 1587.2 $\pm$ .03 39.1 $\pm$ 0.2 .037 $\pm$ .0007 1884.4/567    
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  
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 -  
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)
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  
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  
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  
$\theta \ {\rm Mus} $  
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)
      Standard fit parameters: 1992.0 $\pm$ 0.4 87.3 $\pm$ 3.0 .094 $\pm$ .0046 868.5/500    
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  
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  
Uncertain candidate  
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 -  
- Names in bold type correspond to events selected for the optical depth and duration analysis (with u0<0.7).
- IC (VJ-IC) are the fitted unmagnified magnitudes of the lensed object (including the contribution of a possible blend).
- t0 is the time of maximum magnification, given in HJD-2 450 000.
- $t_{\rm E}$ is the Einstein disk crossing time, in days.
- u0 is the dimensionless impact parameter.
- $\chi^2/\rm d.o.f.$ corresponds to the best microlensing fit.
- $\tau$ 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 $\tau$.

Notes: (1) GSA8: Blended; $C_R=1.00\pm 0.03,\ C_B=0.68 \pm 0.02$; lensed star has $I_C^*\ (V_J^*-I_C^*)=16.6\ (4.4)$. (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. (3) GSA18: parallax; projected Einstein radius in the solar plane $\tilde{r}_{\rm E}=12.5\pm 7.0 ~\rm AU$. (4) GSA2: described in Paper I. Found at that time as the first candidate for a binary lensed source (Xallarap). (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. (6) GSA20: parallax; $\tilde{r}_{\rm E}=0.94\pm 0.07 ~\rm AU$. (7) GSA21: blended; $C_R=0.53\pm 0.02,\ C_B=0.34\pm 0.02$; lensed star has $I_C^*\ (V_J^*-I_C^*)=17.5\ (3.5)$. (8) GSA25: an improbable configuration, but a genuine one (very small u0 on a very faint star). (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.


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