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NGC 3862

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NGC3862
SDSSimage of NGC 3862. The small galaxy at the top of the image isIC 2955.
Observation data (J2000epoch)
ConstellationLeo
Right ascension11h45m05.0s[1]
Declination19° 36′ 23″[1]
Redshift0.021718 ± 0.000019[1]
Heliocentric radial velocity6511 ± 6km/s[1]
Distance304Mly(93.3Mpc)
GrouporclusterLeo Cluster
Apparent magnitude(V)13.67[1]
Characteristics
TypeE[1]
Size~152,000ly(46.6kpc) (estimated)[1]
Apparent size(V)1.5 x 1.5[1]
Notable featurescontains asupermassive black holepowering a jet ofplasmathat is moving at 98 percent of thespeed of light
Other designations
UGC06723,PGC036606,MCG+03-30-095, CGCG 097-127, 3C 264, 4C +19.40, PKS 1142+19[1]

NGC 3862is anelliptical galaxylocated 300 millionlight-yearsaway[2]in theconstellationLeo.[3]Discovered by astronomerWilliam Herschelon April 27, 1785,[4]NGC 3862 is an outlying member of theLeo Cluster.[5]

The galaxy is classified as aFR I radio galaxy[6]and as aHead-tail radio galaxy.[7][8]It hosts asupermassive black holethat is blasting a jet ofplasmathat is moving at 98 percent of thespeed of lightand is one of the few jets that can be seen invisible light.[9]

Onesupernovahas been observed in NGC 3862: SN 2023bqk (type Ia-pec,mag. 18.3).[10]

Jet

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Observations made by Bridle et al. in 1981 using maps made with theVLArevealed ajet-like structureemerging from the nucleus of NGC 3862.[7]In late January 1992, theHubble Space Telescopeobserved NGC 3862 with theFaint Object Spectrographand confirmed the presence of an optical jet in the nucleus of NGC 3862.[11][3]

A sequence ofHubble Space Telescopeimages taken between 1994 and 2014 showing the jet in NGC 3862.

The optical jet, which has a measured length of 2,800ly(860pc), appears to expand slowly and dims in peak and integrated brightness within the interior of the apparent ring of dust.[12]Within distances of about 260–360ly(80–110pc), the jet appears narrow and well-collimated.[13][14]At a distance of 330ly(100pc) the jet starts to abruptly expand and becomes turbulent. At this distance, filaments and pronounced kinks can be observed which suggests that the jet is oscillating or evolving a helical structure.[14]After crossing the ring at a distance of around 980–1,300ly(300–400pc), the jet widens dramatically, changes direction, and dims more rapidly both in peak and integrated brightness and becomes more diffuse in appearance. This suggests that the jet is interacting with the dust ring and becomes less collimated.[12]However, Perlman et al. suggests that the disk and the jet occupy physically distinct regions of the galaxy and therefore are not interacting.[15]

The total amount of energy produced by the jet is estimated to be around 3.71 × 1042ergs.[16]

Knots

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The jet of NGC 3862 contains four[17][15]faint knots of material designated in increasing order from the nucleus: Knot A, B, C and D.[15]The knots exhibit a structure similar to that of a string of pearls.[9]

Radio morphology

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NGC 3862 contains aHead-tailradio morphology[5][18][19]with two tails[20][21]that extend 520,000ly(160kpc).[7][18]This morphology appears to be the result of the galaxy interacting with theintracluster medium(ICM).[22]

Nucleus

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The central region of NGC 3862 appears host a nearly face-on disk of dust[23][24][12][25]with a diameter of 2,200ly(675pc).[26]However, as the jet of galaxy has been suggested to lie at angle of 50°[15][12]toEarth's line of sight, the dust disk must bepuffed up[12][23]in order for the jet to have been disturbed by the disk.[12]The emission ofCOin the nucleus exhibits a double-horned line profile which suggests that the dust disk is rotating. The inferred distribution of theCOis consistent with the observed dust disk and the presence of the molecular gas suggests that the gas originated from either amergerwith two gas-rich galaxies a few billion years ago or from cannibalism of smaller gas-rich galaxies.[27]

Hutchings et al. proposed instead that the apparent disk represents an evacuated region cleared of dust by some nuclear related process or by the jet itself[28][23]as indicated by the color of the region inside the ring being similar to the color of the galaxy spectrum.[28]Lara et al. also suggested this as the jet appears to widen within the apparent ring which would be consistent with an explanation of a favored expansion of the jet due to the lower density medium within the evacuated region or bubble.[13]

Supermassive black hole

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NGC 3862 contains asupermassive black holewith an estimated mass of4.7×108M☉.[29][8]

The black hole is responsible for producing the jet ofplasmathat is moving at nearly the speed of light.[9]

Companion galaxies

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NGC 3862 has anelliptical[30]or alenticularcompanion galaxyknown asIC 2955.It lies about 72,000ly(22kpc) from NGC 3862.[24]

See also

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References

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  1. ^abcdefghi"NASA/IPAC Extragalactic Database".Results for NGC 3862.Retrieved2018-09-03.
  2. ^"Your NED Search Results".ned.ipac.caltech.edu.Retrieved2018-09-03.
  3. ^ab"High Energy Jet in Galaxy NGC 3862".sci.esa.int.ESA. 7 May 1992.Retrieved26 August2018.
  4. ^"New General Catalog Objects: NGC 3850 – 3899".cseligman.com.Retrieved2018-09-03.
  5. ^abNorthover, K. J. E. (1976-11-01)."Observations of the Radio Galaxies 3C 264 and 3C 315".Monthly Notices of the Royal Astronomical Society.177(2): 307–317.Bibcode:1976MNRAS.177..307N.doi:10.1093/mnras/177.2.307.ISSN0035-8711.
  6. ^"3CRR Atlas:3C 264: Main Page".www.jb.man.ac.uk.Retrieved2018-09-04.
  7. ^abcBridle, A. H.; Vallee, J. P. (August 1981)."High-resolution radio observations of the X-ray galaxy NGC 3862 /3C 264/ in Abell 1367".The Astronomical Journal.86:1165–1174.doi:10.1086/112995.
  8. ^abBoccardi, B.; Migliori, G.; Grandi, P.; Torresi, E.; Mertens, F.; Karamanavis, V.; Angioni, R.; Vignali, C. (2019-07-01)."The TeV-emitting radio galaxy 3C 264 - VLBI kinematics and SED modeling".Astronomy & Astrophysics.627:A89.arXiv:1905.06634.Bibcode:2019A&A...627A..89B.doi:10.1051/0004-6361/201935183.ISSN0004-6361.
  9. ^abc"HubbleSite: News – Hubble Video Shows Shock Collision Inside Black Hole Jet".hubblesite.org.Retrieved2018-09-04.
  10. ^Transient Name Server entry for SN 2023bqk.Retrieved 25 October 2023.
  11. ^Crane, P.; Peletier, R.; Baxter, D.; Sparks, W. B.; Albrecht, R.; Barbieri, C.; Blades, J. C.; Boksenberg, A.; Deharveng, J. M. (January 1993). "Discovery of an optical synchrotron jet in 3C 264".The Astrophysical Journal.402:L37–L40.Bibcode:1993ApJ...402L..37C.doi:10.1086/186694.ISSN0004-637X.
  12. ^abcdefBaum, Stefi A.; O'Dea, Christopher P.; Giovannini, Gabriele; Cotton, William B.; Koff, Sigrid de; Luigina Feretti; Golombek, Daniel; Lara, Lucas; Macchetto, Ferdinando D. (1997)."HST and Merlin Observations of 3C 264—A Laboratory for Jet Physics and Unified Schemes".The Astrophysical Journal.483(1): 178.Bibcode:1997ApJ...483..178B.doi:10.1086/304221.ISSN0004-637X.S2CID121711548.
  13. ^abLara, L.; Giovannini, G.; Cotton, W. D.; Feretti, L.; Venturi, T. (2004-02-13). "The inner kiloparsec of the jet in 3C 264".Astronomy & Astrophysics.415(3): 905–913.arXiv:astro-ph/0311077.Bibcode:2004A&A...415..905L.doi:10.1051/0004-6361:20034317.ISSN0004-6361.S2CID15112672.
  14. ^abLara, L.; Feretti, L.; Giovannini, G.; Baum, S.; Cotton, W. D.; O’Dea, C. P.; Venturi, T. (March 1, 1999)."The Radio‐Optical Jet in NGC 3862 from Parsec to Subkiloparsec Scales".The Astrophysical Journal.513(1): 197–206.arXiv:astro-ph/9810495.Bibcode:1999ApJ...513..197L.doi:10.1086/306852.ISSN0004-637X.S2CID119367414.
  15. ^abcdPerlman, E. S.; Padgett, C. A.; Georganopoulos, M.; Worrall, D. M.; Kastner, J. H.; Franz, G.; Birkinshaw, M.; F. Dulwich; O'Dea, C. P. (2010). "A Multi-Wavelength Spectral and Polarimetric Study of the Jet of 3C 264".The Astrophysical Journal.708(1): 171–187.arXiv:0911.1817.Bibcode:2010ApJ...708..171P.doi:10.1088/0004-637X/708/1/171.ISSN0004-637X.S2CID56125038.
  16. ^Sahakyan, N.; Baghmanyan, V.; Zargaryan, D. (June 2018). "Fermi-LAT observation of nonblazar AGNs".Astronomy & Astrophysics.614:A6.arXiv:1801.09381.Bibcode:2018A&A...614A...6S.doi:10.1051/0004-6361/201732304.ISSN0004-6361.S2CID119278881.
  17. ^Meyer, Eileen T.; Georganopoulos, Markos; Sparks, William B.; Perlman, Eric; van der Marel, Roeland P.; Anderson, Jay; Sohn, Sangmo Tony; Biretta, John; Norman, Colin (May 2015)."A kiloparsec-scale internal shock collision in the jet of a nearby radio galaxy".Nature.521(7553): 495–497.Bibcode:2015Natur.521..495M.doi:10.1038/nature14481.hdl:11603/19645.ISSN0028-0836.PMID26017450.S2CID4451677.
  18. ^abLara, L.; Cotton, W. D.; Feretti, L.; Giovannini, G.; Venturi, T.; Marcaide, J. M. (1997-01-01)."VLBI Observations of a Complete Sample of Radio Galaxies. VII. Study of the FR I Sources 3C 31, 4C 35.03, and 3C 264".The Astrophysical Journal.474(1): 179–187.Bibcode:1997ApJ...474..179L.doi:10.1086/303462.ISSN0004-637X.
  19. ^Gavazzi, G.; Perola, G. C.; Jaffe, W. (1981-11-01). "Observations of the head-tail radio galaxy NGC 3862 /3C 264/ at 0.6, 1.4, and 5.0 GHz".Astronomy and Astrophysics.103:35–43.Bibcode:1981A&A...103...35G.ISSN0004-6361.
  20. ^Baum, Stefi Alison; Heckman, Timothy M.; Bridle, Alan; van Breugel, Wil J. M.; Miley, George K. (1988-12-01)."Extended optical-line-emitting gas in radio galaxies – Broad-band optical, narrow-band optical, and radio imaging of a representative sample".The Astrophysical Journal Supplement Series.68:643–714.Bibcode:1988ApJS...68..643B.doi:10.1086/191301.ISSN0067-0049.
  21. ^Parma, P.; de Ruiter, H. R.; Cameron, R. A. (1991-12-01). "Very large array observations of radio-selected dumbbell galaxies".The Astronomical Journal.102:1960–1976.Bibcode:1991AJ....102.1960P.doi:10.1086/116018.ISSN0004-6256.
  22. ^Kharb, P.; O'Dea, C. P.; Tilak, A.; Baum, S. A.; Haynes, E.; Noel-Storr, J.; Fallon, C.; Christiansen, K. (2012-07-01). "VLBA and Chandra Observations of Jets in FRI Radio Galaxies: Constraints on Jet Evolution".The Astrophysical Journal.754(1): 1.arXiv:1205.1460.Bibcode:2012ApJ...754....1K.doi:10.1088/0004-637X/754/1/1.ISSN0004-637X.S2CID118636901.
  23. ^abcMartel, André R.; Turner, Neal J.; Sparks, William B.; Baum, Stefi A. (2000)."Nuclear Gas and Dust Disks in Nearby 3CR Elliptical Galaxies".The Astrophysical Journal Supplement Series.130(2): 267.Bibcode:2000ApJS..130..267M.doi:10.1086/317356.ISSN0067-0049.
  24. ^abKleijn, Gijs A. Verdoes; Baum, Stefi A.; Zeeuw, P. Tim de; O'Dea, Chris P. (1999). "Hubble Space Telescope Observations of Nearby Radio-Loud Early-Type Galaxies".The Astronomical Journal.118(6): 2592.arXiv:astro-ph/9909256.Bibcode:1999AJ....118.2592V.doi:10.1086/301135.ISSN1538-3881.
  25. ^Quillen, A. C.; Almog, Jessica; Yukita, Mihoko (2003). "870 Micron Observations of Nearby 3CRR Radio Galaxies".The Astronomical Journal.126(6): 2677.arXiv:astro-ph/0308306.Bibcode:2003AJ....126.2677Q.doi:10.1086/379562.ISSN1538-3881.S2CID119358673.
  26. ^van Bemmel, I. M.;Morganti, R.;Oosterloo, T.; van Moorsel, G. (2012-11-29). "A relation between circumnuclear H I, dust, and optical cores in low-power radio galaxies".Astronomy & Astrophysics.548:A93.arXiv:1211.0859.Bibcode:2012A&A...548A..93V.doi:10.1051/0004-6361/201219179.ISSN0004-6361.S2CID119279384.
  27. ^Lim, Jeremy; Leon, Stephane; Combes, Françoise; Dinh-V-Trung (2000). "Molecular Gas in the Powerful Radio Galaxies 3C 31 and 3C 264: Major or Minor Mergers?".The Astrophysical Journal Letters.545(2): L93.arXiv:astro-ph/0011520.Bibcode:2000ApJ...545L..93L.doi:10.1086/317885.ISSN1538-4357.S2CID119081169.
  28. ^abHutchings, J. B.; Baum, S. A.; Weistrop, D.; Nelson, C.; Kaiser, M. E.; Gelderman, R. F. (1998). "Spatially Resolved Spectra of 3C Galaxy Nuclei".The Astronomical Journal.116(2): 634.arXiv:astro-ph/9805177.Bibcode:1998AJ....116..634H.doi:10.1086/300474.ISSN1538-3881.S2CID119106358.
  29. ^Le, Truong; Newman, William; Edge, Brinkley (2018-03-10). "Jet launching radius in low-power radio-loud AGNs in advection-dominated accretion flows".Monthly Notices of the Royal Astronomical Society.477(2): 1803–1813.arXiv:1803.03860.Bibcode:2018MNRAS.477.1803L.doi:10.1093/mnras/sty644.ISSN0035-8711.S2CID59501170.
  30. ^"Your NED Search Results".ned.ipac.caltech.edu.Retrieved2018-10-12.
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