06h09.1m00s, 24° 21′00″
| Messier35 | |
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| Observation data (J2000 epoch) | |
| Right ascension | 06h08m 54.0s[1] |
| Declination | +24° 20′ 00″[1] |
| Distance | 2,970 ly (912 pc)[1] |
| Apparent magnitude (V) | 5.3[2] |
| Apparent dimensions (V) | 28[3] arcmins |
| Physical characteristics | |
| Mass | 1,600[4] M☉ |
| Radius | 11 ly[5] |
| Estimated age | 175 Myr[4] |
| Other designations | M35, NGC 2168,[6] Cr 82, C 0605+243 |
| Associations | |
| Constellation | Gemini |
| See also: Open cluster, List of open clusters | |
Messier 35orM35, also known as NGC 2168 or the Shoe-Buckle Cluster, is a relatively close open clusterofstars in the west of Gemini, at about the declination of the Sun when the latter is at June solstice.[a] It was discovered by Philippe Loys de Chéseaux around 1745 and independently discovered by John Bevis before 1750.[3] It is scattered over part of the sky almost the size of the full moon and is 2,970 light-years (912 parsecs) away.[1] 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 3.75 parsecs (12.2 ly) was found to be between 1600 and 3200 solar masses,[b] consistent with the mass of a realistic stellar population within the same radius.[7] Bouy et al. in 2015 found a mass of around 1,600 M☉ within the central 27.5' × 27.5′. 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] The cluster's metallicity is [Fe/H] = −0.21±0.10, 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.[8] Four probable members are chemically peculiars, while HD 41995, which in the (telescopic angular) cluster field, shows emission lines.[9]Huet 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.[10]
Stars
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