Summary. 



1. The distribution of the ordinary clusters in space was studied supposing 

 the distance of a cluster to be inversely proportional to its apparent diameter. The 

 investigation was confined to those clusters which have been observed by Melotte 

 on the Franklin-Adams plates, these observations having the advantage of embracing 

 the whole heaven and moreover of giving apparent diameters on a uniform scale. 



The position of the clusters projected on three perpendicular Galactic planes 

 is shown on plates II and III. We find the distribution of the clusters to be in 

 the main identical to that of the J5 stars before discussed. Especially we find the 

 centre of the clusters to be situated in the same direction from the sun as the 

 centre of the 5-stars (in the coustallatiou Carina) thus stating the result found in 

 Meddel. Ser. II, N:o 14. 



It is under such circumstances natural to suppose the centres of the .B-stars 

 and of the clusters to coincide, which puts us in the position to determine the scale 

 (s) in the distribution of the clusters. Determining s from the distance of the centre 

 we find tliat the clusters have the same dispersion perpendicular to tlie galaxy as 

 the j5-stars, whereas the dispersion in the plane of tlie Galaxy is twice as great for 

 the clusters as for the 7i-stars. Tiie clusters are spread in the galactic plane to as 

 distance of 200 siriometers and perhaps somewhat more. 



2. The distribution of the globular clusters in space was, in like maimer, 

 based on their apparent diameters. Here a homogeneous and almost complete 

 material is collected by Bailey and published in H. A. 76. The distribution of the 

 globulars are essentially different from that of ordinary clusters. The centre of the 

 ystem of the globular clusters lies not in the direction of the centre of the Galaxy, 

 as determind from i^-stars and ordinary clusters, but perpendicular to it and 

 approximately in the galactic plane. The system of the globulars seems to have the 

 form of a prolate spheroid, having the axis of rotation in the plane of the Galaxy. 

 The greater axis (= the axis of rotation) is twice as long as the smaller axis. 



The scale is here more difficult to determine than for the ordinary clusters. 

 Many reasons speaking, however, for the galactic nature of the globulars — for 

 instance the similar distribution of the planetary nebulae shown on plate IV — it 

 may be assumed that the centre of the system of globulars lies in the XF-plane 



