Messier 52
| Messier52 | |
|---|---|
 Open cluster Messier 52 in Cassiopeia | |
| Observation data (J2000epoch) | |
| Right ascension | 23h24m48.0s[1] |
| Declination | +61° 35′ 36″[1] |
| Distance | 4.6kly(1.4kpc)[1] |
| Apparent magnitude(V) | 7.3[2] |
| Apparent dimensions (V) | 13.0′[3] |
| Physical characteristics | |
| Mass | 1,200M☉[4]M☉ |
| Radius | 9.5 ly[3] |
| Estimated age | 158.5 Myr[1] |
| Other designations | NGC7654,Cr455, C 2322+613, OCl 260[5] |
| Associations | |
| Constellation | Cassiopeia |
Messier 52orM52,also known asNGC 7654or theScorpion Cluster,is anopen clusterofstarsin the highly northernconstellationofCassiopeia.It was discovered byCharles Messierin 1774.[3][a]It can be seen fromEarthundera good night skywithbinoculars.The brightness of the cluster is influenced byextinction,which is stronger in the southern half.[6]Itsmetallicityis somewhat below that of theSun,and is estimated to be [Fe/H] = −0.05 ± 0.01.[7]
R. J. Trumplerclassifiedthe cluster appearance as II2r, indicating a rich cluster with little central concentration and a medium range in the brightness of the stars.[8]This was later revised to I2r, denoting a dense core.[6]The cluster has a core radius of 2.97 ± 0.46 ly (0.91 ± 0.14 pc) and atidal radiusof 42.7 ± 7.2 ly (13.1 ± 2.2 pc).[4]It has an estimated age of 158.5 million years[1]and a mass of1,200M☉.[4]
The magnitude 8.3 supergiant star BD +60°2532 is a probable member of the cluster,[4]so too 18 candidateslowly pulsating B stars,one being aDelta (δ) Scuti variable,and three candidateGamma Doradus (γ Dor) variables.[9]There may also be threeBe stars.[10]The core of the cluster shows a lack of interstellar matter, which may be due tosupernovaeexplosion(s) early in the cluster's history.[6]
See also
[edit]References and footnotes
[edit]- ^abcdeWu, Zhen-Yu; et al. (November 2009), "The orbits of open clusters in the Galaxy",Monthly Notices of the Royal Astronomical Society,399(4): 2146–2164,arXiv:0909.3737,Bibcode:2009MNRAS.399.2146W,doi:10.1111/j.1365-2966.2009.15416.x,S2CID6066790.
- ^"Messier 52".SEDS Messier Catalog.Archived fromthe originalon 1 July 2022.Retrieved29 April2022.
- ^abcAdam, Len (2018),Imaging the Messier Objects Remotely from Your Laptop,The Patrick Moore Practical Astronomy Series, Springer, p. 241,Bibcode:2018imor.book.....A,ISBN978-3319653853
- ^abcdBonatto, C.; Bica, E. (September 2006), "Methods for improving open cluster fundamental parameters applied to M 52 and NGC 3960",Astronomy and Astrophysics,455(3): 931–942,arXiv:astro-ph/0608022,Bibcode:2006A&A...455..931B,doi:10.1051/0004-6361:20065315,S2CID16118935
- ^"M 52".SIMBAD.Centre de données astronomiques de Strasbourg.RetrievedNovember 28,2018.
- ^abcPandey, A. K.; et al. (August 2001), "NGC 7654: An interesting cluster to study star formation history",Astronomy and Astrophysics,374(2): 504–522,Bibcode:2001A&A...374..504P,doi:10.1051/0004-6361:20010642.
- ^Akbulut, B.; Ak, S.; Yontan, T.; Bilir, S.; Ak, T.; Banks, T.; Kaan Ulgen, E.; Paunzen, E. (2021). "A study of the Czernik 2 and NGC 7654 open clusters using CCD UBV photometric and Gaia EDR3 data".Astrophysics and Space Science.366(7).arXiv:2107.03462.doi:10.1007/s10509-021-03975-x.S2CID235765696.
- ^Trumpler, Robert Julius (1930), "Preliminary results on the distances, dimensions and space distribution of open star clusters",Lick Observatory Bulletin,420:154–188,Bibcode:1930LicOB..14..154T,doi:10.5479/ADS/bib/1930LicOB.14.154T.
- ^Luo, Y. P.; et al. (February 2012), "Discovery of 14 New Slowly Pulsating B Stars in the Open Cluster NGC 7654",The Astrophysical Journal Letters,746(1): 5,Bibcode:2012ApJ...746L...7L,doi:10.1088/2041-8205/746/1/L7,L7.
- ^Bond, Howard E. (August 1973), "Be Stars in the Galactic Cluster M 52",Publications of the Astronomical Society of the Pacific,85(506): 405,Bibcode:1973PASP...85..405B,doi:10.1086/129477.
- ^September 7
External links
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Media related toMessier 52at Wikimedia Commons- Messier 52, SEDS Messier pages
- Messier 52 onWikiSky:DSS2,SDSS,GALEX,IRAS,Hydrogen α,X-Ray,Astrophoto,Sky Map,Articles and images
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