6 Results

From the observations of program 1 used from 03 Nov. 1995 to 25 June 1997, we get corrections in both coordinates for 200 stars. Coverage of declination is about 65 degrees (from $9\hbox{$.\!\!^\circ$}5$ to $74\hbox{$.\!\!^\circ$}5$) with no gap. The results are given in the appendix, in the order of declinations from $9^\circ$ to $75^\circ$.One sees from the list that the formal errors $E_{\triangle \alpha}$vary with $\sin A$. The formal errors $E_{\triangle \delta}$vary with $\delta(\cos Q)$. When $\delta = 63^\circ$,$\cos Q$ reachs its minimum (0.5) and the $E_{\triangle \delta}$reach maximum. For $E_{\triangle \alpha} \cos \delta$, $93\%$ are better than $\pm4$ ms, $85\%$better than $\pm 3$ ms, and their mean value is $\pm 2.3$ ms. For $E_{\triangle \delta}$, $86\%$ are better than $\pm 0.040''$, $51\%$ better than $\pm 0.030''$, and their mean value is $\pm 0.031''$. If we had observed more nights in the summer of 1996, we would have got better precisions for some stars in both $\triangle \alpha$and $\triangle \delta$. One can see from Table 5 that the precisions of group corrections for numbers 9 and 10 are about 2 times worse than the others, which makes mean residuals M for some stars in the groups 9 and 10 less precise.

  

Table 5: Group corrections