Messier 35

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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.[1] It is scattered over part of the sky almost the size of the full moon and is Script error: No such module "convert". away.[2] 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 Script error: No such module "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.[3] Bouy et al. in 2015 found a mass of around Script error: No such module "val". within the central 27.5' × 27.5. 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.[4] The cluster's metallicity is [Fe/H] = Script error: No such module "val"., where −1 would be ten times less metallic than the sun.[4]

Of 418 probable members, Leiner et al. in 2015 found 64 that have variable radial velocities thus are binary star systems.[5] Four probable members are chemically peculiars, while HD 41995, which in the (telescopic angular) cluster field, shows emission lines.[6] 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.[7]

See also

References and footnotes

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External links

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