Coma Cluster

Short description: Cluster of galaxies in the constellation Coma Berenices

Not to be confused with Coma Star Cluster.

Coma Cluster

File:290px
Observation data (Epoch J2000)
Constellation(s)| Coma Berenices
Right ascension|  12h 59m 48.7s[1]
Declination| +27° 58′ 50″[1]
Brightest member| NGC 4874 and NGC 4889
Number of galaxies| > 1000[2][3]
Richness class| 2[4]
Bautz–Morgan classification| II[4]
Velocity dispersion| 1,000 km/s[5]
Redshift| 0.0231 (6 925 km/s)[1]
Distance
(co-moving)| 102.975 Mpc (336 Mly) for h−10.705[1]
ICM temperature| 8–9 keV[6]
Binding mass| ~7×1014[7] M☉
X-ray flux| (319.20 ± 2.6%)×10−12 erg s−1 cm−2[1] (0.1–2.4 keV)[1]
Other designations
Abell 1656[1]
See also: Galaxy group, Galaxy cluster, List of galaxy groups and clusters

The Coma Cluster (Abell 1656) is a large cluster of galaxies that contains over 1,000 identified galaxies.[2][3] Along with the Leo Cluster (Abell 1367), it is one of the two major clusters comprising the Coma Supercluster.[8] It is located in and takes its name from the constellation Coma Berenices. It is one of the first galaxy clusters that was remarked upon in the astronomy literature, being visually noted by William Herschel in 1785[9][10] and photographically surveyed by Max Wolf in 1901.[11][12]

The cluster's mean distance from Earth is 99 Mpc (321 million light years).[3][13][14] Its ten brightest spiral galaxies have apparent magnitudes of 12–14 that are observable with amateur telescopes larger than 20 cm.[15] The central region is dominated by two supergiant elliptical galaxies: NGC 4874 and NGC 4889.[16] The cluster is within a few degrees of the north galactic pole on the sky. Most of the galaxies that inhabit the central portion of the Coma Cluster are ellipticals. Both dwarf and giant ellipticals are found in abundance in the Coma Cluster.[17]

## Contents

* 1 Cluster members
* 2 Dark matter
* 3 X-ray source
* 4 Gallery
* 5 See also
* 6 References
* 7 External links

## Cluster members

Tails in spiral galaxy D100, found in the Coma Cluster, are created by ram-pressure stripping.[18][19]

As is usual for clusters of this richness, the galaxies are overwhelmingly elliptical and S0 galaxies, with only a few spirals of younger age, and many of them probably near the outskirts of the cluster. Some of the galaxies in the Coma Cluster have also been identified as ultra diffuse galaxies.

The full extent of the cluster was not understood until it was more thoroughly studied in the 1950s by astronomers at Mount Palomar Observatory, although many of the individual galaxies in the cluster had been identified previously.[20][21][22]

## Dark matter

The Coma Cluster is one of the first places where observed gravitational anomalies were considered to be indicative of unobserved mass. In 1933 Fritz Zwicky showed that the galaxies of the Coma Cluster were moving too fast for the cluster to be bound together by the visible matter of its galaxies. Though the idea of dark matter would not be accepted for another fifty years, Zwicky wrote that the galaxies must be held together by "dunkle Materie" (dark matter).[23][24]

About 90% of the mass of the Coma cluster is believed to be in the form of dark matter.

## X-ray source

An extended X-ray source centered at 1300+28 in the direction of the Coma cluster of galaxies was reported before August 1966.[25] This X-ray observation was performed by balloon, but the source was not detected in the sounding rocket flight launched by the X-ray astronomy group at the Naval Research Laboratory on November 25, 1964.[26] A strong X-ray source was observed by the X-ray observatory satellite Uhuru close to the center of the Coma cluster and this source was suggested to be designated Coma X-1.[27]

The Coma cluster contains about 800 galaxies within a 100 × 100 arc-min area of the celestial sphere. The source near the center at RA (1950) 12h56m ± 2m Dec 28°6' ± 12' has a luminosity Lx = 2.6 × 1044 ergs/s.[27] As the source is extended, with a size of about 45', this argues against the possibility that a single galaxy is responsible for the emission.[27] The Uhuru observations indicated a source strength of no greater than ~10−3 photons cm−2s−1keV−1 at 25 keV,[27] which disagrees with the earlier observations[25] claiming a source strength of ~10−2 photons cm−2s−1keV−1 at 25 keV, and a size of 5°.

## Gallery

* Thousands of globular clusters lying at the core of a galaxy cluster[28]

* A large portion of the Coma Cluster seen by Hubble's Advanced Camera for Surveys

* Hubble close-up on the Coma Cluster[29]

* A face-on view of a spiral galaxy (NGC 4911) located deep within the Coma Cluster

* Map of the central part of the Coma Cluster.

## See also

* List of Abell clusters
* List of galaxy groups and clusters
* Eridanus Cluster
* Fornax Cluster – another nearby cluster of galaxies
* Norma Cluster
* Virgo Cluster – another nearby cluster of galaxies
* X-1 X-ray source

## References

1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "NASA/IPAC Extragalactic Database". Results for Abell 1656. http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Abell+1656&extend=no.
2. ↑ 2.0 2.1 "Chandra/Field Guide to X-ray Sources". Coma Cluster. http://chandra.harvard.edu/xray_sources/coma/.
3. ↑ 3.0 3.1 3.2 "NASA / Focus on the Coma Cluster". http://imagine.gsfc.nasa.gov/docs/features/objects/coma.html.
4. ↑ 4.0 4.1 Abell, George O.; Corwin, Harold G. Jr.; Olowin, Ronald P. (May 1989). "A catalog of rich clusters of galaxies". Astrophysical Journal Supplement Series 70 (May 1989): 1–138. doi:10.1086/191333. ISSN 0067-0049. Bibcode: 1989ApJS...70....1A.
5. ↑ Struble, Mitchell F.; Rood, Herbert J. (November 1999). "A Compilation of Redshifts and Velocity Dispersions for ACO Clusters". The Astrophysical Journal Supplement Series (Chicago, Illinois, USA: The University of Chicago Press) 125 (1): 35–71. doi:10.1086/313274. Bibcode: 1999ApJS..125...35S.
6. ↑ Section 4 of Sato, Takuya; Matsushita, Kyoko; Ota, Naomi; Sato, Kosuke; Nakazawa, Kazuhiro; Sarazin, Craig L. (November 2011). "Suzaku Observations of Iron K-Lines from the Intracluster Medium of the Coma Cluster". Publications of the Astronomical Society of Japan 63 (SP3): S991–S1007. doi:10.1093/pasj/63.sp3.s991. Bibcode: 2011PASJ...63S.991S. http://pasj.asj.or.jp/v63/sp3/63s345/63s345.pdf. Retrieved March 12, 2012.
7. ↑ Gavazzi, R.; Adami, C.; Durret, F.; Cuillandre, J.-C.; Ilbert, O.; Mazure, A.; Pelló, R.; Ulmer, M.P. (May 2009). "A weak lensing study of the Coma cluster". Astronomy and Astrophysics 498 (2): L33–L36. doi:10.1051/0004-6361/200911841. Bibcode: 2009A&A...498L..33G.
8. ↑ "The Coma Supercluster". http://www.atlasoftheuniverse.com/superc/com.html.
9. ↑ "From Messier to Abell: 200 Years of Science with Galaxy Clusters - A.Biviano". https://ned.ipac.caltech.edu/level5/Biviano2/Biviano2_1.html.
10. ↑ Herschel, William (1785). "On the Construction of the Heavens." (in en). Philosophical Transactions of the Royal Society of London. Series I 75: 213–266. Bibcode: 1785RSPT...75..213H. https://ui.adsabs.harvard.edu/abs/1785RSPT...75..213H/abstract.
11. ↑ Wolf, Max (1901). "Ein merkwürdiger Haufen von Nebelflecken" (in de). Astronomische Nachrichten 155 (6–8): 127–128. doi:10.1002/asna.19011550608. Bibcode: 1901AN....155..127W. https://ui.adsabs.harvard.edu/abs/1901AN....155..127W/abstract.
12. ↑ Wolf, Max (1902). "Die Nebelflecken am Pol der Milchstrasse" (in de). Publikationen des Astrophysikalischen Instituts Koenigstuhl-Heidelberg 1: 125–176. Bibcode: 1902PAIKH...1..125W. https://ui.adsabs.harvard.edu/abs/1902PAIKH...1..125W/abstract.
13. ↑ "2MASS Atlas Image Gallery: Galaxy Groups and Clusters". Infrared Processing and Analysis Center. http://www.ipac.caltech.edu/2mass/gallery/images_galcl.html.
14. ↑ Colless, M (2001). "Coma Cluster". in P Murdin. Encyclopedia of Astronomy and Astrophysics. Bristol Institute of Physics publishing. http://eaa.iop.org/abstract/0333750888/2600. Retrieved 2006-10-08.
15. ↑ Singapore Science Centre. "ScienceNet – Astronomy & Space Science – Observatories/ Telescopes – Question No. 13490". http://www.science.edu.sg/ssc/detailed.jsp?artid=1950&type=6&root=6&parent=6&cat=66.
16. ↑ Conselice, Christopher J., Gallagher, John S., III (1998). "Galaxy aggregates in the Coma cluster". Monthly Notices of the Royal Astronomical Society 297 (2): L34–L38. doi:10.1046/j.1365-8711.1998.01717.x. Bibcode: 1998MNRAS.297L..34C.
17. ↑ Newswise: Hubble's Sweeping View of the Coma Cluster of Galaxies Retrieved on June 11, 2008.
18. ↑ "Wading through water" (in en). https://www.spacetelescope.org/images/potw1904a/.
19. ↑ Cramer, William J. (Jan 2019). "Spectacular Hubble Space Telescope Observations of the Coma Galaxy D100 and Star Formation in Its Ram Pressure–stripped Tail". The Astrophysical Journal 870 (2): 2. doi:10.3847/1538-4357/aaefff. Bibcode: 2019ApJ...870...63C.
20. ↑ Zwicky, Fritz (October 1937). "On the Masses of Nebulae and of Clusters of Nebulae". Astrophysical Journal 86 (3): 217–246. doi:10.1086/143864. Bibcode: 1937ApJ....86..217Z.
21. ↑ Shapley, Harlow (July 1934). "A Photometric Investigation of Wolf's Cluster of Nebulae in Coma". Harvard College Observatory Bulletin (Cambridge, MA, USA) 896: 3–12. Bibcode: 1934BHarO.896....3S.
22. ↑ Wallenquist, Å. (1933). "On the space distribution of the nebulae in the Coma Cluster". Annalen V.d. Bosscha-Sterrenwacht (Miscellaneous Papers (Observatorium Bosscha)) (France: Bandoeng : Gebrs. Kleijne) 4 (6): 73–77. Bibcode: 1933AnBos...4...73W.
23. ↑ Zwicky, F. (1933). "Die Rotverschiebung von extragalaktischen Nebeln" (in German). Helvetica Physica Acta 6: 110–127. Bibcode: 1933AcHPh...6..110Z. https://articles.adsabs.harvard.edu//full/1933AcHPh...6..110Z/0000110.000.html. From p 125: "Um, wie beobachtet, einen mittleren Dopplereffekt von 1000 km/sek oder mehr zu erhalten, müsste also die mittlere Dichte im Comasystem mindestens 400 mal grösser sein als die auf Grund von Beobachtungen an leuchtender Materie abgeleitete. Falls sich dies bewahrheiten sollte, würde sich also das überraschende Resultat ergeben, dass dunkle Materie in sehr viel grösserer Dichte vorhanden ist als leuchtende Materie." (In order to obtain an average Doppler effect of 1000 km/s or more, as observed, the average density in the Coma system would thus have to be at least 400 times greater than that derived on the basis of observations of luminous matter. If this were to be verified, the surprising result would then follow that dark matter is present in very much greater density than luminous matter.)
24. ↑ de Swart, J. G.; Bertone, G.; van Dongen, J. (2017). "How dark matter came to matter". Nature Astronomy 1 (59): 0059. doi:10.1038/s41550-017-0059. Bibcode: 2017NatAs...1E..59D.
25. ↑ 25.0 25.1 "Extended source of energetic cosmic X rays". Phys. Rev. Lett. 17 (8): 447–50. 1966. doi:10.1103/PhysRevLett.17.447. Bibcode: 1966PhRvL..17..447B.
26. ↑ "X-rays from the Coma cluster of galaxies". Astrophysical Journal 147 (1): 399–401. January 1967. doi:10.1086/149022. Bibcode: 1967ApJ...147..368..
27. ↑ 27.0 27.1 27.2 27.3 "A strong X-ray source in the Coma cluster observed by Uhuru". Astrophysical Journal 167 (8): L81–4. Aug 1971. doi:10.1086/180765. Bibcode: 1971ApJ...167L..81G.
28. ↑ "Clusters within clusters". https://www.spacetelescope.org/images/potw1849a/.
29. ↑ "Hubble close-up on the Coma Cluster". ESA/Hubble Picture of the Week. http://www.spacetelescope.org/images/potw1402a/.

## External links

* The Coma Cluster of Galaxies – Astronomy Picture of the Day, NASA, 2000 August 6
* The clickable Coma galaxy cluster
* The dynamical state of the Coma cluster with XMM-Newton
* Very Small Array observations of the Sunyaev-Zel'dovich effect in nearby galaxy clusters
* Hubble Space Telescope Treasury Survey of the Coma Cluster
*   * The Coma Cluster on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images

Coordinates:  12h 59m 49s, +27° 58′ 50″

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* t
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Astronomical catalogs

Abell|

* Astronomy:Abell 1651
* Astronomy:Abell 1652
* Astronomy:Abell 1653
* Astronomy:Abell 1654
* Astronomy:Abell 1655
* Abell 1656
* Astronomy:Abell 1657
* Astronomy:Abell 1658
* Astronomy:Abell 1659
* Astronomy:Abell 1660
* Astronomy:Abell 1661

* v
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Coma Berenices constellation

Stars
(list)|

| Bayer|

* α (Diadem)
* β
* γ

|

Flamsteed|

* 1
* 2
* 3
* 4
* 5
* 6
* 7
* 8
* 9
* 10
* 11
* 12
* 13
* 14
* 16
* 17
* 18
* 20
* 21
* 22
* 23
* 24
* 25
* 26
* 27
* 28
* 29
* 30
* 31
* 32
* 33
* 35
* 36
* 37
* 38
* 39
* 41

Variable|

* U
* RW
* RZ
* SS
* ST
* UX
* AL
* CC
* EK
* FK
* FM
* FS (40)
* GM
* GO
* GP
* HH
* IL
* IN
* KR
* LM
* LW

HR|

* 4633
* 4642
* 4668
* 4673
* 4676
* 4680
* 4693
* 4694
* 4698
* 4705
* 4719
* 4725
* 4793
* 4812
* 4873
* 4886
* 4926
* 4956
* 4962
* 4984
* 4992
* 5007
* 5010
* 5057
* 5102

HD|

* 107146
* 107415
* 108863
* 108874
* 112060
* 112127
* 114762
* 115404
* 116029

Other|

* BD +25 2511
* Feige 66
* GD 153
* HZ 21
* HZ 43
* PSR B1237+25
* RBS 1223
* WISE 1217+1626

Star
clusters|

| Open|

* Coma Star Cluster

|

Globular|

* Messier 53
* NGC 4147
* NGC 5053

Nebulae|

| Planetary|

* H 4-1
* LoTr 5

|

Galaxies|

| Messier|

* 64 (Black Eye Galaxy)
* 85
* 88
* 91
* 98
* 99
* 100

|

NGC|

* 4015
* 4016
* 4017
* 4018
* 4021
* 4022
* 4023
* 4028
* 4032
* 4037
* 4040
* 4042
* 4048
* 4049
* 4053
* 4056
* 4060
* 4061
* 4064
* 4065
* 4066
* 4069
* 4070
* 4072
* 4074
* 4076
* 4080
* 4084
* 4086
* 4089
* 4090
* 4091
* 4092
* 4093
* 4095
* 4098
* 4101
* 4104
* 4110
* 4122
* 4126
* 4131
* 4132
* 4134
* 4136
* 4146
* 4150
* 4152
* 4155
* 4158
* 4162
* 4166
* 4169
* 4173
* 4174
* 4175
* 4185
* 4186
* 4189
* 4192A
* 4196
* 4203
* 4204
* 4208
* 4211
* 4211B
* 4212
* 4213
* 4222
* 4237
* 4239
* 4245
* 4251
* 4253
* 4262
* 4272
* 4274
* 4275
* 4278
* 4283
* 4286
* 4293
* 4295
* 4298
* 4302
* 4308
* 4310
* 4312
* 4314
* 4323
* 4328
* 4336
* 4340
* 4344
* 4350
* 4359
* 4375
* 4377
* 4379
* 4383
* 4393
* 4394
* 4396
* 4405
* 4408
* 4414
* 4419
* 4421
* 4446
* 4447
* 4448
* 4450
* 4455
* 4459
* 4468
* 4473
* 4474
* 4475
* 4477
* 4479
* 4489
* 4494
* 4495
* 4498
* 4502
* 4506
* 4514
* 4515
* 4516
* 4523
* 4525
* 4529
* 4539
* 4540
* 4555
* 4556
* 4558
* 4559
* 4561
* 4562
* 4563
* 4565
* 4571
* 4585
* 4595
* 4611
* 4613
* 4614
* 4615
* 4633
* 4634
* 4635
* 4651
* 4659
* 4670
* 4673
* 4676 (Mice Galaxies)
* 4685
* 4689
* 4692
* 4710
* 4712
* 4715
* 4721
* 4725
* 4728
* 4728B
* 4728C
* 4735
* 4738
* 4745
* 4745B
* 4747
* 4752
* 4758
* 4787
* 4788
* 4789
* 4789A
* 4793
* 4798
* 4807
* 4807A
* 4816
* 4817
* 4819
* 4821
* 4827
* 4828
* 4839
* 4840
* 4841
* 4842
* 4848
* 4849
* 4850
* 4851
* 4853
* 4854
* 4858
* 4859
* 4860
* 4864
* 4865
* 4867
* 4869
* 4871
* 4872
* 4873
* 4874
* 4875
* 4876
* 4881
* 4882
* 4883
* 4889
* 4892
* 4894
* 4895
* 4895A
* 4896
* 4898
* 4906
* 4907
* 4908
* 4911
* 4911A
* 4919
* 4921
* 4922
* 4923
* 4926
* 4926A
* 4926B
* 4927
* 4929
* 4931
* 4934
* 4935
* 4943
* 4944
* 4949
* 4952
* 4957
* 4961
* 4966
* 4971
* 4978
* 4979
* 4983
* 5000
* 5004A
* 5004C
* 5012
* 5012A
* 5016
* 5032
* 5032B
* 5041
* 5052
* 5056
* 5057
* 5065
* 5081
* 5089
* 5092
* 5116
* 5151
* 5158
* 5172
* 5180
* 5190
* 5217

Other|

* B2 1215+30
* B2 1308+326
* 3C 275.1
* 3C 287
* 4C +21.35
* Coma A
* Coma Berenices
* DDO 154
* 1ES 1218+304
* GQ Com
* IC 755 (NGC 4019)
* IC 3599
* IC 4051
* IOK-1
* LEDA 83677
* Malin 1
* ON 231 (W Com)
* PG 1211+143
* PG 1247+268
* PGC 44691
* Ton 153
* Ton 1530
* Ton 1542
* UGC 7321

Galaxy
clusters|

* Coma Cluster
* M94 Group
* NGC 4631 Group

Other|

* GRB 000418
* GRB 050509B
* GRB 080607
* GRB 090323
* GRB 090424
* iPTF14atg
* SN 1979C
* SN 1984A
* SN 1987K
* SN 2005ap
* SN 2006X
* VIRGOHI21
* XRF 050416A

* v
* t
* e

Galaxies

Morphology|

* Disc
* Lenticular
* barred
* unbarred
* Spiral
* anemic
* barred
* flocculent
* grand design
* intermediate
* Magellanic
* unbarred
* Dwarf galaxy
* elliptical
* irregular
* spheroidal
* spiral
* Elliptical galaxy
* cD
* Irregular
* barred
* Peculiar
* Ring
* Polar

Structure|

* Active galactic nucleus
* Bar
* Bulge
* Dark matter halo
* Disc
* Disc galaxy
* Halo
* corona
* Galactic center
* Galactic plane
* Galactic ridge
* Interstellar medium
* Protogalaxy
* Spiral arm
* Supermassive black hole

Active nuclei|

* Blazar
* LINER
* Markarian
* Quasar
* Radio
* X-shaped
* Relativistic jet
* Seyfert

Energetic galaxies|

* Lyman-alpha emitter
* Luminous infrared
* Starburst
* blue compact dwarf
* pea
* faint blue
* Hot dust-obscured

Low activity|

* Low surface brightness
* Ultra diffuse
* Dark galaxy

Interaction|

* Field
* Galactic tide
* Cloud
* Groups and clusters
* group
* cluster
* Brightest cluster galaxy
* fossile group
* Interacting
* merger
* Jellyfish
* Satellite
* Stellar stream
* Superclusters
* Walls
* Voids and supervoids
* void galaxy

Lists|

* Galaxies
* Galaxies named after people
* Largest
* Nearest
* Polar-ring
* Ring
* Spiral
* Groups and clusters
* Large quasar groups
* Quasars

* Superclusters
* Voids

See also|

* Extragalactic astronomy
* Galactic astronomy
* Galactic coordinate system
* Galactic empire
* Galactic habitable zone
* Galactic magnetic fields
* Galactic orientation
* Galactic quadrant
* Galaxy color–magnitude diagram
* Galaxy formation and evolution
* Galaxy rotation curve
* Illustris project
* Intergalactic dust
* Intergalactic stars
* Intergalactic travel
* Population III stars

* Book
* Category
* Portal

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