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Messier 35 or M35, also known as NGC 2168 or the Shoe-Buckle Cluster, is a relatively close open cluster of stars in the west of Gemini, at about the declination of the Sun when the latter is at June solstice.Template:Efn It was discovered by Philippe Loys de Chéseaux around 1745 and independently discovered by John Bevis before 1750.<ref name=Thompson2007/> It is scattered over part of the sky almost the size of the full moon and is Template:Convert away.<ref name=Wu2009a/> The compact open cluster NGC 2158 lies directly southwest of it.

Leonard & Merritt (1989) computed the mass of M35 using a statistical technique based on proper motion velocities of its stars. The mass within the central Template:Convert was found to be between 1600 and 3200 solar masses,Template:Efn consistent with the mass of a realistic stellar population within the same radius.<ref name=Leonard1989/> Bouy et al. in 2015 found a mass of around Template:Val within the central Template:Nowrap. There are 305 stars that can be intrinsically shown to be extremely likely to be members,Template:Efn 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.<ref name=Bouy2015/> The cluster's metallicity is [Fe/H] = Template:Val, where −1 would be ten times less metallic than the sun.<ref name=Bouy2015/>

Of 418 probable members, Leiner et al. in 2015 found 64 that have variable radial velocities thus are binary star systems.<ref name=Leiner2015/> Four probable members are chemically peculiars, while HD 41995, which in the (telescopic angular) cluster field, shows emission lines.<ref name=Paunzen2014/> Hu et al. in 2005 found 13 variable stars in the field; at least three are suspect as cluster members. To be a member means to have a gravitational tie or, if recently freed, having been created by the same event.<ref name=Hu2005/>

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