DEPARTMENT OF MERIDIAN ASTROMETRY. I4I 



Since the date of my last report the Prehminary General Catalogue of 

 6,188 stars has been completed, and the printer's copy has recently been sent 

 to the Carnegie Institution. The completion of this work has been delayed 

 through a variety of causes connected with the large scheme of observations 

 and reductions carried on throughout the year, together with other extensive 

 pieces of computation growing out of results derivable from the new Cata- 

 logue, and also with the preparation of the program of observation for the 

 Southern Observatory. 



Among these a careful discussion of the solar motion is a prominent fea- 

 ture. This has been completed so far as the determination of the solar apex 

 is concerned. The definitive result of this, for 1875, so far as the present ma- 

 terial is concerned, is: 



R. A., 270° 31'; Decl., +34° 17' 



The results in detail for four pairs of zones, symmetrical with the equator, 



are: 



A D 



to ±10° 270°. +34°.5 



±10 to ±30 270 .8 +31 .0 



±30 to ±50 273 .8 +38 .3 



±50 to ±90 272 .8 +30 .0 



Restricting the computations to stars of the sixth magnitude and brighter, 

 we have 



A=26g° 52' D=+34° 39' 



For stars having motions larger than 20" per century the result is 

 A=272° 29' D=+34° 28' 



These results of the partial areas seem to be so accordant that it is difficult 

 to suspect that there are anomalous deviations from the law of random mo- 

 tions in various parts of the sky or at different distances from the sun. 



Results derived from the material distributed in zones parallel with the Gal- 

 axy are equally accordant with these, but show that the mean distances of the 

 stars near the plane of the Galaxy are greater than those of the stars near the 

 poles. But in this part of the discussion peculiarities of motion have been de- 

 veloped that require further study. 



The material of observation is now being prepared for a further discussion 

 by methods other than those employed in obtaining the results presented in 

 the foregoing, and by methods calculated to throw light on the relation of the 

 stellar-motions to the system of the Galaxy. Of this part of the work it 

 would be premature to speak at present. 



During the discussion for the solar motion, of which the main results are 

 presented in the foregoing, a special research was made that led to the fol- 

 lowing results, stated in summary : 



