NGC 3860

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NGC 3860
SDSS NGC 3860.jpg
SDSS image of NGC 3860.
Observation data (J2000 epoch)
ConstellationLeo
Right ascension11h 44m 49.1s[1]
Declination19° 47′ 42″[1]
Redshift0.018663[1]
Helio radial velocity5595 km/s[1]
Distance340 Mly (105 Mpc)[1]
Group or clusterLeo Cluster
Apparent magnitude (V)14.22[1]
Characteristics
TypeSa[1]
Mass~3.7×1011[2] M☉
Size~133,000 ly (40.7 kpc) (estimated)[1]
Apparent size (V)1.0 x 0.5[1]
Other designations
CGCG 97-120, IRAS 11422+2003, MCG 3-30-88, PGC 36577, UGC 6718[1]

NGC 3860 is a spiral galaxy[3] located about 340 million light-years away[4] in the constellation Leo.[5] NGC 3860 was discovered by astronomer William Herschel on April 27, 1785.[6] The galaxy is a member of the Leo Cluster[7][8] and is a low-luminosity AGN (LLAGN).[9][10] Gavazzi et al. however classified NGC 3860 as a strong AGN which may have been triggered by a supermassive black hole in the center of the galaxy.[11]

H I deficiency[]

Observations of NGC 3860 show that the galaxy has lost approximately 90% of its original hydrogen content. This indicates that NGC 3860 has crossed though the core of the Leo Cluster and that ram pressure exerted by the dense intergalactic medium in the cluster stripped most of the neutral atomic hydrogen from the galaxy.[12]

The gas disk of NGC 3860 is truncated, which is an additional indicator that the galaxy is undergoing ram pressure stripping as it falls into the Leo Cluster.[13]

See also[]

References[]

  1. ^ a b c d e f g h i j "NASA/IPAC Extragalactic Database". Results for NGC 3860. Retrieved 2018-07-23.
  2. ^ Sun, M.; Murray, S. S. (2002). "Chandra View of the Dynamically Young Cluster of Galaxies A1367. I. Small-Scale Structures". The Astrophysical Journal. 576 (2): 708. arXiv:astro-ph/0206255. Bibcode:2002ApJ...576..708S. doi:10.1086/341756. ISSN 0004-637X. S2CID 11414230.
  3. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2018-07-23.
  4. ^ "NED Query Results for NGC 3860". ned.ipac.caltech.edu. Retrieved 2018-07-23.
  5. ^ "Revised NGC Data for NGC 3860". spider.seds.org. Retrieved 2018-07-23.
  6. ^ "New General Catalog Objects: NGC 3850 - 3899". cseligman.com. Retrieved 2018-07-17.
  7. ^ "NGC 3860". Retrieved 2018-07-24.
  8. ^ "Detailed Object Classifications". ned.ipac.caltech.edu. Retrieved 2018-07-24.
  9. ^ Sun, M.; Murray, S. S. (2002). "Chandra View of the Dynamically Young Cluster of Galaxies A1367. II. Point Sources". The Astrophysical Journal. 577 (1): 139–149. arXiv:astro-ph/0202431. Bibcode:2002ApJ...577..139S. doi:10.1086/342156. ISSN 0004-637X. S2CID 119421982.
  10. ^ Caglar, Turgay; Hudaverdi, Murat (2017-08-31). "XMM–Newton view of X-ray overdensities from nearby galaxy clusters: the environmental dependencies". Monthly Notices of the Royal Astronomical Society. 471 (4): 4990–5007. arXiv:1709.00117. Bibcode:2017MNRAS.471.4990C. doi:10.1093/mnras/stx1811. ISSN 0035-8711. S2CID 39126208.
  11. ^ Gavazzi, G.; Savorgnan, G.; Fumagalli, Mattia (2011-09-26). "The complete census of optically selected AGNs in the Coma supercluster: the dependence of AGN activity on the local environment". Astronomy & Astrophysics. 534: A31. arXiv:1107.3702. Bibcode:2011A&A...534A..31G. doi:10.1051/0004-6361/201117461. ISSN 0004-6361. S2CID 73621726.
  12. ^ Gavazzi, G.; Cortese, L.; Boselli, A.; Iglesias-Paramo, J.; Vílchez, J. M.; Carrasco, L. (2003). "Capturing a Star Formation Burst in Galaxies Infalling onto the Cluster A1367". The Astrophysical Journal. 597 (1): 210–217. arXiv:astro-ph/0307075. Bibcode:2003ApJ...597..210G. doi:10.1086/378264. ISSN 0004-637X.
  13. ^ Fossati, Matteo; Fumagalli, Michele; Gavazzi, Giuseppe; Consolandi, Guido; Boselli, Alessandro; Yagi, Masafumi; Sun, Ming; Wilman, David J. (2019-04-01). "MUSE sneaks a peek at extreme ram-pressure stripping events - IV. Hydrodynamic and gravitational interactions in the Blue Infalling Group". Monthly Notices of the Royal Astronomical Society. 484 (2): 2212–2228. arXiv:1901.03334. Bibcode:2019MNRAS.484.2212F. doi:10.1093/mnras/stz136. ISSN 0035-8711. S2CID 118857397.

External links[]


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