Several star clumps are detected inside the low-density extended corona of the open cluster M 67 with the help of the method ``the distances to nearest neighbour analysis'', elaborated earlier for analysis of galaxy distributions. The groups include from 5 to 11 stars and have mean sizes from 0.5 to 1.2 pc. We check the reality of their existence by statistical estimates based on kinematical data analysis. It is shown that at least one clump is not a random star density fluctuation. The question of the origin of these substructures remains open.
Astronomy and Astrophysics
- Pub Date:
- June 1998
- STARS: FORMATION;
- OPEN CLUSTERS AND ASSOCIATIONS: INDIVIDUAL: M 67