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NGC 3311

Topic: Astronomy

 From HandWiki - Reading time: 7 min
Short description: Galaxy in the constellation Hydra
NGC 3311
Color cutout hst 06554 03 wfpc2 f814w f555w pc sci NGC 3311.jpg
HST image of NGC 3311
Observation data (J2000 epoch)
ConstellationHydra
Right ascension 10h 36m 42.8s[1]
Declination−27° 31′ 42″[1]
Redshift0.012759[1]
Helio radial velocity3825 km/s[1]
Distance190 Mly (57 Mpc)[1]
Group or clusterHydra Cluster
Apparent magnitude (V)12.65[1]
Characteristics
TypecD2, E+2[1]
Number of starsmore than 1 trillion[2]
Size~230,000 ly (70 kpc) (estimated)[1]
Apparent size (V)3.5 x 2.9[1]
Notable featuresMassive globular cluster population
Other designations
ESO 501-38, AM 1034-271, MCG -4-25-36, PGC 31478[1]

NGC 3311 is a super-giant[2] elliptical galaxy[3] (a type-cD galaxy)[4][3] located about 190 million light-years away[5] in the constellation Hydra.[6] The galaxy was discovered by astronomer John Herschel on March 30, 1835.[7][8] NGC 3311 is the brightest[9][10] member of the Hydra Cluster[11] and forms a pair with NGC 3309 which along with NGC 3311, dominate the central region of the Hydra Cluster.[12]

NGC 3311 is surrounded by a rich and extensive globular cluster system[13] rivaling that of Messier 87 in the Virgo Cluster.[4]

Physical characteristics

The central region of NGC 3311 is obscured by a dust cloud[14] with an estimated diameter of 1,700 ly (0.53 kpc).[15] It has an amorphous and complex structure and its small size and disturbed morphology suggests that the cloud originated from a merger event with another galaxy that occurred within the past 10 million years. Oddly though, there are no shells or isophote distortions in the outer regions of NGC 3311 that would have been the result of such a recent merger. Other scenarios for the origin of the dust cloud are by a cooling flow or by galactic wind failure.

The total estimated mass of the dust cloud is 4,600 solar masses (4.6×104 M☉).[14]

In NGC 3311, it has been detected that there is an excess blue population in the central region of the galaxy. The spectrum of the galaxy appears to resemble that of an H II region. This suggests that the excess blue population represents an ongoing formation of young bright stars.[16]

Outer halo

The outer halo of NGC 3311 appears to have formed from the accretion[17] and mergers of massive satellite galaxies in vicinity of the galaxy.[18] The halo is made up of intra-cluster stars with a dominant part of these stars coming from the outskirts of bright early-type galaxies and the rest originating from dwarf galaxies.[19] However, the build-up of its extended halo is still ongoing due to the infall of a group of 14 dwarf galaxies including the galaxies HCC 026 and HCC 007 that are currently being tidally disputed and adding their stars to the outer halo.[18][17][20][9] In contrast, the inner galaxy formed from the mergers of gas-rich lumps reminiscent of the first phase of galaxy formation.[18]

Stellar populations

The stars in the central region of NGC 3311 and in the halo are very old, with ages of over 10 Gyrs. However the stars in the central galaxy have a higher metallicity than the halo suggesting the stars in the stars in the central galaxy formed in a rapid but short period of star formation that occurred early on though a gas-rich dissipative collapse while the stars in halo formed in smaller accreted satellite galaxies with more extended star formation.[21]

Off-centered envelope

NGC 3311 contains an off centered-envelope that was first detected by Arnaboldi et al. The off centered-envelope has a higher metallicity than the outer halo[20] and is located close to the infalling group of dwarf galaxies.[18][20]

The envelope appears to have been offset from the center of NGC 3311 by a tidal interaction with the dark matter halos of the infalling group of dwarf galaxies or halo associated with NGC 3309. This tidal interaction would have also stripped gas and dust from the outer halo of NGC 3311.[18]

Intracluster planetary nebulae

Around 60 intracluster planetary nebulae have been detected surrounding NGC 3311.[22]

Supermassive black hole

NGC 3311 is host to a supermassive black hole with an estimated mass of 126 million solar masses (1.26 × 108 M☉).[23]

Dark matter halo

NGC 3311 appears to have a cored dark matter halo.[24]

Radio source

NGC 3311 has a weak radio source with a total 6-cm flux density of 0.3 mJy.[13][16]

Although NGC 3311 has a weak radio source, it is bright in X-rays.[25]

Globular clusters

NGC 3311 has one of the largest globular cluster systems known in the local universe. With an estimated population of about 16,500 ± 2,000 globular clusters, NGC 3311's globular cluster system rivals that of Messier 87's, which has about 13,000 globular clusters.[4] NGC 3309, another nearby giant elliptical has an unusually low number of globular clusters. This suggests that NGC 3311 stripped part of NGC 3309's globular clusters, with some of its globular clusters becoming members of NGC 3311's system.[24]

NGC 3311's globular cluster system was initially detected in 1976[26] and was found by Harris et al. in 1983 to contain a massive globular cluster system similar to Messier 87.[27]

An analysis by Secker et al. in 1995 using Washington photometry from the Cerro Tololo Inter-American Observatory concluded that NGC 3311 had the most metal-rich globular cluster system known, with a complete absence of populations of metal-poor and intermediate-metallicity globular clusters.[28] However, Brodie et al. and Wehner et al. determined that the globular cluster system shows a bimodal color distribution with equal numbers of metal-rich and metal-poor clusters.[29][4]

Ultra-compact dwarf galaxies

A large population of about 50 ultra-compact dwarf galaxies (UDCs)[30] have been detected in the Hydra Cluster,[31][30] with most of them being dynamically associated to NGC 3311. It appears that the ultra-compact dwarf galaxies, especially the brighter and more massive ones such as HUCD1 with a mass of 5×107 and a half-light radius of 83 ly (25.4 pc) are the remnant nuclei of dwarf galaxies whose stellar envelopes were stripped off during an interaction with another galaxy or the cluster itself.[30]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 "NASA/IPAC Extragalactic Database". Results for NGC 3311. http://nedwww.ipac.caltech.edu/. 
  2. ↑ 2.0 2.1 Bely, Pierre-Yves; Christian, Carol; Roy, Jean-René (2010-03-11) (in en). A Question and Answer Guide to Astronomy. Cambridge University Press. ISBN 978-0-521-18066-5. https://books.google.com/books?id=PbLPel3zRdEC&pg=PA170. 
  3. ↑ 3.0 3.1 "Detailed Object Classifications". http://ned.ipac.caltech.edu/cgi-bin/NEDatt?objname=NGC+3311. 
  4. ↑ 4.0 4.1 4.2 4.3 Wehner, Elizabeth M. H.; Harris, William E.; Whitmore, Bradley C.; Rothberg, Barry; Woodley, Kristin A. (2008). "The Globular Cluster Systems around NGC 3311 and NGC 3309" (in en). The Astrophysical Journal 681 (2): 1233. doi:10.1086/587433. ISSN 0004-637X. Bibcode: 2008ApJ...681.1233W. http://stacks.iop.org/0004-637X/681/i=2/a=1233. 
  5. ↑ "Your NED Search Results". http://ned.ipac.caltech.edu/cgi-bin/objsearch?objname=NGC+3311&extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES. 
  6. ↑ "Revised NGC Data for NGC 3311". http://spider.seds.org/ngc/revngcic.cgi?NGC3311. 
  7. ↑ Gottlieb, Steve. "Astronomy-Mall: Adventures In Deep Space NGC objects 3001-3999". http://www.astronomy-mall.com/Adventures.In.Deep.Space/NGC%203000%20-%203999%20(11-30-17).htm. 
  8. ↑ "New General Catalog Objects: NGC 3300 - 3349" (in en-US). https://cseligman.com/text/atlas/ngc33.htm#3311. 
  9. ↑ 9.0 9.1 Barbosa, C. E.; Arnaboldi, M.; Coccato, L.; Gerhard, O.; Mendes de Oliveira, C.; Hilker, M.; Richtler, T. (January 2018). "Sloshing in its cD halo: MUSE kinematics of the central galaxy NGC 3311 in the Hydra I cluster" (in en). Astronomy & Astrophysics 609: A78. doi:10.1051/0004-6361/201731834. ISSN 0004-6361. Bibcode: 2018A&A...609A..78B. 
  10. ↑ "NGC 3311". http://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC+3311&submit=submit+id. 
  11. ↑ Richter, O.-G. (February 1989). "The Hydra I cluster of galaxies. V - A catalogue of galaxies in the cluster area". Astronomy and Astrophysics Supplement Series 77: 237–256. Bibcode: 1989A&AS...77..237R. 
  12. ↑ Kotanyi, C. (November 1990). "NGC 3309: an S-shaped radio galaxy in a nearby cluster.". Revista Mexicana de Astronomía y Astrofísica 21: 173–176. Bibcode: 1990RMxAA..21..173K. 
  13. ↑ 13.0 13.1 Lindblad, P. O.; Jorsater, S., S.; Sandqvist, Aa. (March 1985). "The nuclear radio sources in the elliptical galaxies NGC 3309 and NGC 3311 in the cluster Abell 1060". Astronomy and Astrophysics 144: 496–501. Bibcode: 1985A&A...144..496L. 
  14. ↑ 14.0 14.1 Grillmair, Carl J.; Faber, S. M.; Lauer, Tod R.; Baum, William A.; Lynds, Roger C.; O'Neil, Earl J. Jr.; Shaya, Edward J. (July 1994). "The nuclear regions of NGC 3311 and NGC 7768 imaged with the Hubble Space Telescope Planetary Camera" (in en). The Astronomical Journal 108: 102. doi:10.1086/117049. ISSN 0004-6256. Bibcode: 1994AJ....108..102G. 
  15. ↑ van Dokkum, P. G.; Franx, M. (1995-11-01). "Dust in the Cores of Early-Type Galaxies". The Astronomical Journal 110: 2027. doi:10.1086/117667. ISSN 0004-6256. Bibcode: 1995AJ....110.2027V. 
  16. ↑ 16.0 16.1 Vasterberg, A. R.; Jorsater, S.; Lindblad, P. O. (July 1991). "An optical study of the cD galaxy NGC 3311 and the giant elliptical galaxy NGC 3309 in the cluster Hydra I". Astronomy and Astrophysics 247: 335–347. Bibcode: 1991A&A...247..335V. 
  17. ↑ 17.0 17.1 Ventimiglia, G.; Arnaboldi, M.; Gerhard, O. (2011-04-01). "The unmixed kinematics and origins of diffuse stellar light in the core of the Hydra I cluster (Abell 1060)". Astronomy and Astrophysics 528: A24. doi:10.1051/0004-6361/201015982. ISSN 0004-6361. Bibcode: 2011A&A...528A..24V. 
  18. ↑ 18.0 18.1 18.2 18.3 18.4 Barbosa, C. E.; Arnaboldi, M.; Coccato, L.; Hilker, M.; Mendes de Oliveira, C.; Richtler, T. (2016-04-26). "The Hydra I cluster core" (in en). Astronomy & Astrophysics 589: A139. doi:10.1051/0004-6361/201628137. ISSN 0004-6361. Bibcode: 2016A&A...589A.139B. 
  19. ↑ Coccato, L.; Gerhard, O.; Arnaboldi, M.; Ventimiglia, G. (2011-09-01). "Stellar population and the origin of intra-cluster stars around brightest cluster galaxies: the case of NGC 3311". Astronomy and Astrophysics 533: A138. doi:10.1051/0004-6361/201117546. ISSN 0004-6361. Bibcode: 2011A&A...533A.138C. 
  20. ↑ 20.0 20.1 20.2 Arnaboldi, M.; Ventimiglia, G.; Iodice, E.; Gerhard, O.; Coccato, L. (2012-09-01). "A tale of two tails and an off-centered envelope: diffuse light around the cD galaxy NGC 3311 in the Hydra I cluster". Astronomy and Astrophysics 545: A37. doi:10.1051/0004-6361/201116752. ISSN 0004-6361. Bibcode: 2012A&A...545A..37A. 
  21. ↑ Johnston, Evelyn J.; Merrifield, Michael; Aragón-Salamanca, Alfonso (2018-08-01). "Spectroscopic decomposition of the galaxy and halo of the cD galaxyNGC 3311". Monthly Notices of the Royal Astronomical Society 478 (3): 4255–4267. doi:10.1093/mnras/sty1342. ISSN 0035-8711. Bibcode: 2018MNRAS.478.4255J. 
  22. ↑ Ventimiglia, G.; Arnaboldi, M.; Gerhard, O. (November 2008). "Intracluster Planetary Nebulae in the Hydra I cluster" (in en). Astronomische Nachrichten 329 (9–10): 1057–1060. doi:10.1002/asna.200811090. ISSN 0004-6337. Bibcode: 2008AN....329.1057V. 
  23. ↑ Pellegrini, S. (2010-07-01). "The Nuclear X-ray Emission of Nearby Early-type Galaxies". The Astrophysical Journal 717 (2): 640–652. doi:10.1088/0004-637X/717/2/640. ISSN 0004-637X. Bibcode: 2010ApJ...717..640P. 
  24. ↑ 24.0 24.1 Richtler, T.; Salinas, R.; Misgeld, I.; Hilker, M.; Hau, G. K. T.; Romanowsky, A. J.; Schuberth, Y.; Spolaor, M. (2011-06-24). "The dark halo of the Hydra I galaxy cluster: core, cusp, cosmological?" (in en). Astronomy & Astrophysics 531: A119. doi:10.1051/0004-6361/201015948. ISSN 0004-6361. Bibcode: 2011A&A...531A.119R. 
  25. ↑ McMahon, P. M.; van Gorkom, J. H.; Richter, O.-G.; Ferguson, H. C. (February 1992). "H I imaging of NGC 3312 and NGC 3314a - A foreground group to the Hydra cluster?" (in en). The Astronomical Journal 103: 399. doi:10.1086/116068. ISSN 0004-6256. Bibcode: 1992AJ....103..399M. 
  26. ↑ Smith, M. G.; Weedman, D. W. (1976-05-01). "Globular clusters in the Hydra I cluster of galaxies.". The Astrophysical Journal 205: 709–715. doi:10.1086/154326. ISSN 0004-637X. Bibcode: 1976ApJ...205..709S. 
  27. ↑ Harris, W. E.; Smith, M. G.; Myra, E. S. (1983-09-01). "Globular cluster systems in the Hydra I elliptical galaxies. II". The Astrophysical Journal 272: 456–472. doi:10.1086/161313. ISSN 0004-637X. Bibcode: 1983ApJ...272..456H. 
  28. ↑ Secker, Jeff; Geisler, Doug; McLaughlin, Dean E.; Harris, William E. (1995-03-01). "Washington photometry of the globular cluster system around NGC 3311. 1: Analysis of the metallicities". The Astronomical Journal 109: 1019–1032. doi:10.1086/117338. ISSN 0004-6256. Bibcode: 1995AJ....109.1019S. 
  29. ↑ Brodie, J. P.; Larsen, S. S.; Kissler-Patig, M. (2000-11-01). "A New Look at Globular Cluster Colors in NGC 3311 and the Case for Exclusively Metal-rich Globular Cluster Systems". The Astrophysical Journal Letters 543 (1): L19–L22. doi:10.1086/318166. ISSN 0004-637X. Bibcode: 2000ApJ...543L..19B. 
  30. ↑ 30.0 30.1 30.2 Misgeld, I.; Mieske, S.; Hilker, M.; Richtler, T.; Georgiev, I. Y.; Schuberth, Y. (2011-07-01). "A large population of ultra-compact dwarf galaxies in the Hydra I cluster". Astronomy and Astrophysics 531: A4. doi:10.1051/0004-6361/201116728. ISSN 0004-6361. Bibcode: 2011A&A...531A...4M. 
  31. ↑ Wehner, Elizabeth M. H.; Harris, William E. (2007-10-01). "Ultracompact Dwarf Candidates in the Hydra Cluster". The Astrophysical Journal Letters 668 (1): L35–L38. doi:10.1086/522305. ISSN 0004-637X. Bibcode: 2007ApJ...668L..35W. 

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