R. J. Trumplerclassified the cluster appearance as II2r, indicating a rich cluster with little central concentration and a medium range in the brightness of the stars.[8] This was later revised to I2r, denoting a dense core.[6] The cluster has a core radius of 2.97 ± 0.46 ly (0.91 ± 0.14 pc) and atidal radius of 42.7 ± 7.2 ly (13.1 ± 2.2 pc).[4] It has an estimated age of 158.5 million years[1] and a mass of1,200 M☉.[4]
^Akbulut, B.; Ak, S.; Yontan, T.; Bilir, S.; Ak, T.; Banks, T.; Kaan Ulgen, E.; Paunzen, E. (2021). "A study of the Czernik 2 and NGC 7654 open clusters using CCD UBV photometric and Gaia EDR3 data".Astrophysics and Space Science.366 (7).arXiv:2107.03462.doi:10.1007/s10509-021-03975-x.S2CID235765696.
^Bond, Howard E. (August 1973), "Be Stars in the Galactic Cluster M 52",Publications of the Astronomical Society of the Pacific,85 (506): 405,Bibcode:1973PASP...85..405B,doi:10.1086/129477.
