Leonard & Merritt (1989) computed the mass of M35 using a statistical technique based on proper motion velocities of its stars.

There are 305 stars that can be intrinsically shown to be extremely likely to be members,[c] and up to 4,349 averaging the 50% membership probability, from the kinematic (such as parallax and proper motion) and spectral data published before 2015.

[4] Of 418 probable members, Leiner et al. in 2015 found 64 that have variable radial velocities thus are binary star systems.

[9] Four probable members are chemically peculiars, while HD 41995, which in the (telescopic angular) cluster field, shows emission lines.

[10] Hu et al. in 2005 found 13 variable stars in the field; at least three are suspect as cluster members.