It is a rich cluster (Trumpler class II3r), with 295 stars according to Haug (1978) and 280 according with Archinal, Hynes (2003).[5] One of its members, V Centauri, is a cepheid variable. Despite its large distance from the cluster centre, it has high likelihood of being a member of it.[6]
The tidal radius of the cluster is 6.4 - 12.4 parsecs (21 - 40 light years) and represents the average outer limit of NGC 5662, beyond which a star is unlikely to remain gravitationally bound to the cluster core.[3]
^Jones, K. G. (March 1969). "The search for the nebulae - VI". Journal of the British Astronomical Association. 79: 213–222. Bibcode:1969JBAA...79..213J.