This cluster has an angular diameter of 10′[8] and a core radius of 3.2′.[9] It has a mass of roughly 746 M☉ and a linear tidal radius of 10.6 ± 1.6 parsecs (34.6 ± 5.2 ly).[3] Based upon photometry, the age of the cluster has been estimated by Wu et al. (2009) as 25.1 Myr[1] and 26.3+3.2 −5.2 Myr by Bell et al. (2013). The luminosity of the stars that have not yet depleted their lithium implies an age of 22±4 Myr, in good agreement with these older estimates.[9]
M36 includes ten stars with a visual magnitude brighter than 10,[9] and 178 down to magnitude 14.[8] 38 members display an infrared excess, with one being particularly high.[10] There is one candidate B-typevariable star, of 9th magnitude.[11]
A 2020 study of the variable stars in the cluster estimated a new closer distance of 3,800 light years from Earth.[12]
The YSO Holoea in M36 and the outflow at different wavelengths.
A young stellar object with an outflow, associated with the infrared source IRAS 05327+3404 was discovered in optical observations of M36. The outflow is nicknamed "Holoea", Hawaiian for "flowing gas". Despite appearing close to M36 it is probably not a part of M36 .It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.[13]
^Frommert, Hartmut; Kronberg, Christine (August 25, 2007), "Messier 36", The Messier Catalog, Students for the Exploration and Development of Space (SEDS), retrieved 2018-11-24.
^ abSanner, J.; et al. (May 2000), "Photometric and kinematic studies of open star clusters. II. NGC 1960 (M 36) and NGC 2194", Astronomy and Astrophysics, 357: 471–483, arXiv:astro-ph/0003327, Bibcode:2000A&A...357..471S.
^Delgado, A. J.; et al. (October 1984), "Search for B-Type Variable Stars in Open Clusters", Information Bulletin on Variable Stars, 2603: 1, Bibcode:1984IBVS.2603....1D.
