The Alpha Persei Cluster, also known as Melotte 20 or Collinder 39, is an open cluster of stars in the northern constellation of Perseus. To the naked eye, the cluster consists of several blue-hued spectral type B stars. The most luminous member is the ~2nd magnitude yellow supergiant Mirfak, also known as Alpha Persei. Bright members also include Delta, Sigma, Psi, 29, 30, 34, and 48 Persei. The Hipparcos satellite and infrared color-magnitude diagram fitting have been used to establish a distance to the cluster of ~560 light-years (172 pc).[6][7] The distance established via the independent analyses agree, thereby making the cluster an important rung on the cosmic distance ladder. As seen from the Earth, the extinction of the cluster due to interstellar dust is around 0.30.[8]
| Alpha Persei Cluster | |
|---|---|
| Observation data (2000.0 epoch) | |
| Right ascension | 03h 26m 42.0s[1] |
| Declination | +48° 48′ 00″[1] |
| Distance | 570 ly[1] (175 pc[1]) |
| Apparent magnitude (V) | 1.2 |
| Apparent dimensions (V) | 6.1°[1] |
| Physical characteristics | |
| Estimated age | 50–70 Mya[2][3] |
| Other designations | Per OB3,[4] Cr 39, Mel 20, OCl 392.0[5] |
| Associations | |
| Constellation | Perseus |
The cluster is centered to the northeast of Alpha Persei.[8] It has a core radius of 11.4 ± 1.4 ly, a half-mass radius of 18 ly,[8] and a tidal radius of 70.6 ± 8.5 ly,[1] with 517 members being identified within the latter.[8] The cluster shows solid evidence of having undergone mass segregation, with the mean stellar mass decreasing toward the edge.[9] The age of this cluster is about 50–70 million years.[2][3] Cluster member stars show a near-solar metallicity, meaning the abundance of elements with atomic numbers higher than 2 are similar to those in the Sun.[8] The cluster shows evidence of tidal tails, which are most likely of galactic origin.[10]
The cluster field displays evidence of a much larger, background star stream. This feature is quite a bit older than the cluster, with an estimated age of 5 ± 1 Gyr. The center of the stream lies 290 ly from the cluster and it has an overall thickness of 590 ly along the line of sight. This is most likely the remains of an old, massive cluster that now has a combined mass of ~6000 M☉.[10]
Members
editThe following prominent stars are considered members of the cluster with high likelihood:
| Designation | Spectral type |
Visual magnitude |
|---|---|---|
| α Per (33 Per)[11] | F5Ib | 1.81 |
| δ Per (39 Per) | B5III | 3.01 |
| ε Per (45 Per) | B1V | 2.88 |
| ψ Per[11] | B5Ve | 4.31 |
| HD 21278[12][13] | B5V | 4.99 |
| 31 Per[11] | B5V | 5.05 |
| 29 Per[11][13] | B3V | 5.16 |
| 30 Per[13] | B8V | 5.49 |
| 34 Per | B3V | 4.67 |
| 48 Per | B3Ve | 4.03 |
| HD 21699 | B8 III | 5.49 |
| HD 21071[13] | B7V | 6.09 |
See also
editReferences
edit- ^ a b c d e f Kharchenko, N. V.; et al. (2013), "Global survey of star clusters in the Milky Way. II. The catalogue of basic parameters", Astronomy and Astrophysics, 558: 8, arXiv:1308.5822, Bibcode:2013A&A...558A..53K, doi:10.1051/0004-6361/201322302, S2CID 118548517, A53.
- ^ a b Prosser, Charles F.; et al. (October 1996). "ROSAT Pointed Observations of the Alpha Persei Cluster". Astronomical Journal. 112: 1570. Bibcode:1996AJ....112.1570P. doi:10.1086/118124.
- ^ a b Paunzen, E.; Mermilliod, J.-C. "WEBDA: Alpha Persei". Universität Wien. Retrieved 2020-10-17.
- ^ Coyne, G. V.; et al. (March 1979), "Wavelength dependence of polarization. XXXIII - The Alpha Persei star cluster", Astronomical Journal, 84: 356–369, Bibcode:1979AJ.....84..356C, doi:10.1086/112431
- ^ "Cl Melotte 20". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-10-17.
{{cite web}}: CS1 maint: postscript (link) - ^ van Leeuwen, F. (2009). "Parallaxes and proper motions for 20 open clusters as based on the new Hipparcos catalogue". Astronomy & Astrophysics. 497 (1): 209–242. arXiv:0902.1039. Bibcode:2009A&A...497..209V. doi:10.1051/0004-6361/200811382. S2CID 16420237.
- ^ Majaess, D.; et al. (2011). "Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars". Journal of the American Association of Variable Star Observers. 39 (2): 219. arXiv:1102.1705. Bibcode:2011JAVSO..39..219M.
- ^ a b c d e Lodieu, N.; et al. (August 2019). "A 5D view of the α Per, Pleiades, and Praesepe clusters". Astronomy & Astrophysics. 628: 26. arXiv:1906.03924. Bibcode:2019A&A...628A..66L. doi:10.1051/0004-6361/201935533. S2CID 182952614. A66.
- ^ Sheikhi, Najmeh; et al. (March 2016). "The binary fraction and mass segregation in Alpha Persei open cluster". Monthly Notices of the Royal Astronomical Society. 457 (1): 1028–1036. arXiv:1601.02186. Bibcode:2016MNRAS.457.1028S. doi:10.1093/mnras/stw059.
- ^ a b Nikiforova, Victoria V.; et al. (September 2020). "The Relation of the Alpha Persei Star Cluster with the Nearby Stellar Stream". The Astronomical Journal. 160 (3): 11. arXiv:2007.11211. Bibcode:2020AJ....160..142N. doi:10.3847/1538-3881/aba753. S2CID 220686998. 142.
- ^ a b c d Zuckerman, B.; et al. (June 2012). "Stellar Membership and Dusty Debris Disks in the α Persei Cluster". The Astrophysical Journal. 752 (1): 12. arXiv:1204.3950. Bibcode:2012ApJ...752...58Z. doi:10.1088/0004-637X/752/1/58. S2CID 119207634. 58.
- ^ Morrell, Nidia; Abt, Helmut A. (July 10, 1992), "Spectroscopic binaries in the Alpha Persei cluster", Astrophysical Journal, Part 1, 393 (2): 666–673, Bibcode:1992ApJ...393..666M, doi:10.1086/171534.
- ^ a b c d Hoogerwerf, Ronnie (March 2000), "OB association members in the ACT and TRC catalogues", Monthly Notices of the Royal Astronomical Society, 313 (1): 43–65, Bibcode:2000MNRAS.313...43H, doi:10.1046/j.1365-8711.2000.03192.x
External links
edit- Frommert, Hartmut; Kronberg, Christine (March 8, 1998). "Alpha Persei Moving Cluster, Mel 20". The Messier Catalogue. SEDS. Retrieved 2020-10-18.
- Käld, Janne. "The Alpha Persei Cluster (Mel 20)". Astronomical Photographs. Archived from the original on 2017-04-08. Retrieved 2020-10-18.