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NGC 3312

Coordinates: Sky map 10h 37m 02.5s, −27° 33′ 54″
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NGC 3312
legacy surveys image of NGC 3312
Observation data (J2000 epoch)
ConstellationHydra
Right ascension10h 37m 02.5s[1]
Declination−27° 33′ 54″[1]
Redshift0.009627[1]
Heliocentric radial velocity2886 km/s[1]
Distance194 Mly (59.4 Mpc)[1]
Group or clusterHydra Cluster
Apparent magnitude (V)12.68[1]
Characteristics
TypeSA(s)b pec?, Jellyfish, LINER[1]
Size~52 kpc (170,000 ly) (estimated)[2]
Apparent size (V)3.3 x 1.3[1]
Other designations
IC 629, ESO 501-43, AM 1034-271, IRAS 10346-2718, MCG -4-25-39, PGC 31513[1]

NGC 3312 is a large[3] and highly inclined[4] spiral galaxy[5] located about 194 million light-years away[6] in the constellation Hydra.[7] The galaxy was discovered by astronomer John Herschel on March 26, 1835. It was later rediscovered by astronomer Guillaume Bigourdan on February 26, 1887. NGC 3312 was later listed and equated with IC 629 because the two objects share essentially the same celestial coordinates.[8][9] NGC 3312 is the largest spiral galaxy[3] in the Hydra Cluster[3][10] and is also classified as a LINER galaxy.[11][4]

Physical characteristics

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NGC 3312 appears to be highly distorted with sharp dust lanes. There are sharp filamentary extensions to the north and an internal ringlike structure in the galaxy. The interstellar matter in the galaxy also appears highly disturbed. These features caused astronomer De Vaucouleurs to suggest that NGC 3312 was distorted by the giant elliptical galaxies NGC 3309 and NGC 3311 which are the dominant ellipticals in the Hydra Cluster. However, NGC 3309 and NGC 3311 are too distant and their relative velocity differences too large for either elliptical to cause the filamentary extensions observed in NGC 3312. It is more likely that NGC 3312 is interacting with the intracluster medium causing ram-pressure stripping which is stripping the interstellar medium of the galaxy. This may have caused the filamentary extensions observed in NGC 3312 as evidenced by the location of the galaxy near the cluster core.[12] As a result, this galaxy can be considered part of a rare class of galaxies, known as jellyfish galaxies.

Star formation

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Although NGC 3312's morphological structure resembles that of anemic galaxies, its mean surface-brightness profile hints that star formation may be quite active. The northwest filamentary extension from NGC 3312 has high surface brightness and has the knotted texture characteristic of active star-forming regions in spiral arms. Also, the internal dust lane of NGC 3312 is ringed with bright condensations.[12]

Radio source

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NGC 3312 contains an unresolved strong radio source in its core with a strength of 27 mJy and radio emission in the disk with a strength of 24 mJy mostly being confined to the spiral arms of the galaxy or regions of star formation.[13]

See also

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References

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  1. ^ a b c d e f g h i "NASA/IPAC Extragalactic Database". Results for NGC 3312. Retrieved 2018-05-29.
  2. ^ König, Michael; Binnewies, Stefan (2017-09-07). The Cambridge Photographic Atlas of Galaxies. Cambridge University Press. ISBN 978-1-107-18948-5.
  3. ^ a b c Huchtmeier, W. K. (July 1990). "Detection of CO emission in Hydra 1 cluster galaxies". NASA Conference Publication. 3084: 386–388. Bibcode:1990NASCP3084..386H.
  4. ^ a b "Sasmirala object pages". dc.zah.uni-heidelberg.de. Retrieved 2018-05-31.
  5. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2018-05-31.
  6. ^ "NED Query Results for NGC 3312". ned.ipac.caltech.edu. Retrieved 2018-05-31.
  7. ^ "Revised NGC Data for NGC 3312". spider.seds.org. Retrieved 2018-05-31.
  8. ^ Gottlieb, Steve. "Astronomy-Mall: Adventures In Deep Space NGC objects 3001–3999". Astronomy-Mall. Retrieved 2018-04-27.
  9. ^ "New General Catalog Objects: NGC 3300 – 3349". cseligman.com. Retrieved 2018-05-04.
  10. ^ 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.
  11. ^ "NGC 3312". Retrieved 2018-05-31.
  12. ^ a b Gallagher, J. S. (July 15, 1978). "Possible optical evidence for ram-pressure-sweeping in the Hydra I cluster of galaxies". The Astrophysical Journal. 223: 386–390. Bibcode:1978ApJ...223..386G. doi:10.1086/156273. ISSN 0004-637X.
  13. ^ 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?". The Astronomical Journal. 103: 399. Bibcode:1992AJ....103..399M. doi:10.1086/116068. ISSN 0004-6256.
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