Table 1: Comparative photometry relative to the star S1. Relative photometric uncertainties in the last significant digit are listed in parentheses after their respective values. The last column gives the reduced $\chi ^2$ of the fit to a constant flux value. Seeing corresponds to the full width at half-maximum of point sources in the image. The data were obtained with DFOSC on the Danish 1.5 m telescope except that marked with a $\dagger $, where StanCam on the NOT was used.
  Days since XRF (3.92 Dec. 2003, UT)  
  1.36 2.29 6.43 8.28 9.33 32.19$^\dagger$ 45.34 63.45 100.12  
Exp. (s): $4\times600$ $3\times600$ $3\times600$ $5\times420$ $3\times600$ $6\times 300$ $5\times600$ $4\times600$ $5\times600$  
Seeing: 1.09 $^{\prime\prime}$ 1.03 $^{\prime\prime}$ 0.95 $^{\prime\prime}$ 0.87 $^{\prime\prime}$ 0.85 $^{\prime\prime}$ 0.83 $^{\prime\prime}$ 0.98 $^{\prime\prime}$ 1.05 $^{\prime\prime}$ 1.00 $^{\prime\prime}$  
Object Relative photometry $\chi^2_\nu$
S2 1.000(5) 0.997(5) 1.013(6) 1.009(4) 1.004(5) 0.994(7) 1.004(3) 1.01(1) 0.992(5) 1.71
S3 1.396(6) 1.386(7) 1.388(8) 1.378(6) 1.378(6) 1.390(9) 1.407(4) 1.42(1) 1.391(6) 3.29
S4 1.923(9) 1.96(1) 1.92(1) 1.921(8) 1.93(1) 1.94(1) 1.929(6) 1.91(2) 1.90(1) 3.15
S5 2.36(1) 2.37(2) 2.41(2) 2.39(1) 2.39(1) 2.35(2) 2.371(9) 2.37(3) 2.40(2) 1.50
HG 031203 2.47(1) 2.48(2) 2.37(2) 2.38(1) 2.34(1) 2.33(2) 2.41(1) 2.52(4) 2.49(2) 15.26


Source LaTeX | All tables | In the text