The systematic differences Astrolabe-FK5 of type and are derived from an analysis of the zenith distance residuals according to the star azimuth. The stars are separated into azimuth intervals which correspond to zones of 17 degrees wide in declination with an overlap of 8.5 degrees approximately. For the stars in each interval, the average mean zenith distance residual R.M. and the mean declination are computed. If A is the mean azimuth of the stars in the interval, R.M.(E) and R.M.(W), the mean residuals for azimuth intervals at the east and west respectively, and if is the adopted latitude of the astrolabe, it can be shown (Guinot 1955; Noël & Débarbat 1990) that for each pair of azimuth intervals (east and west) one has:
where A and S are the averages of the azimuth and paralactic angle respectively of the stars in the azimuth intervals. The results obtained with expressions (1) and (2) are given in Table 1 (click here), and in Fig. 1 they are plotted with similar results obtained with the automatic meridian circle of the U.S. Naval Observatory Station at Black Bierch, New Zealand (Corbin 1991). In Table 1 (click here), is the mean declination of the stars comprised in each declination zone designated by NN, and and are the number of stars at the corresponding east and west azimuth intervals respectively, involved in the computation of the systematic differences Astrolabe-FK5. According to the principles of the method of equal altitudes (Débarbat & Guinot 1970), systematic differences in declination are given only for those zones where the absolute value of the cosine of the paralactic angle is greater than 0.3. The systematic differences in right ascension as well as their mean errors given in Table 1 (click here) and Fig. 1 (click here) are multiplied by .
Figure 1: Systematic differences in right ascension as a function of declination: Instrument-FK5