958 



3. Immediate results of the comparison. . 



The zone-corrections found were afterwards added to the direct Ij^ 

 obtained differences Kü — B.Z. with reversed sign. From the quantities 

 so obtained I then formed mean values in various ways. 



In the first place two groups were distinguished according to 

 magnitude (limit 8'". 50 according to Kü) : group B and group F. 



Then solutions were carried out, by which in varying degree the 

 largest P. M. are excluded : 



a. solution A', in which were only exchided all stars from zones 

 1, 2, 5, and 7 (which show great anomalies), besides those stars 

 from other zones (13 in number), which show in one of the two 

 coordinates a very great difference Kü — B.Z,, which, as a further investi- 

 gation showed, could not be explained to a large extent by P. M.; 



b. solution A, in which a small number of the largest P. M. was 

 excluded as loell, viz. all differences which deviated by more than 

 0*8 or 10"0 from a "normal" value for Kü — B.Z. derived from a 

 preliminary solution; these were 39 in number; 



c. solution E, in which 1 excluded all differences which deviated 

 by more than 0^40 or 5''0 from the normal ; there were 315 of these. 



In all these cases a deviation in one of the coordinates has 

 caused the complete exclusion of the star. 



Further I reduced all results to the system of Auwers' New 

 Fundamental Catalogue, while at the same time 1 calculated all 

 the reductions so as to be able to pass over to the system of 

 Newcomb or Boss (Prel. Gen. Cat.). 



4. Determinations of the unknown quantities. 



The mean numbers are, as formerly; represented by formulae of 

 the form 



A« =r a + ^ ^^n a -\- c cos a -\- d sin 2« -f « cos 2« + fsm 3« -j- g cos 3« 

 Afi =z a' -\- b' si7i a -\- c' cos ft -\- d' siti 2« + •?' cos 2a -\- ƒ' sin 3« -|- 9' cos 3«, 



the actual unknown quantities were deduced from the coefficients 

 of these formulae, after- corrections had again been introduced 

 depending upon the systematic connection between the distances 

 of the stars and the galactic latitude. The results obtained are 

 briefly discussed below. 



5. Results for the precession. 



a. from Right Ascensions. The six values of the precession from 

 the various solutions agree very satisfactorily, especially those 

 obtained from bright and faint stars : 



