Messier 35 | |
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Observation data ( J2000 epoch) | |
Right ascension | 06h 08m 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 |
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. [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] 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. [10]
Messier 35 | |
---|---|
![]() | |
Observation data ( J2000 epoch) | |
Right ascension | 06h 08m 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 |
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. [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] 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. [10]