Wikipedia

Messier 85

Messier 85 (also known as M85 or NGC 4382 or PGC 40515 or ISD 0135852) is a lenticular galaxy, or elliptical galaxy for other authors,[4] in the Coma Berenices constellation. It is 60 million light-years away, and has a diameter of about 36.99 kiloparsecs (120,600 light-years) across.[1][5]

Messier 85
Galaxy Messier 85 by Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationComa Berenices
Right ascension12h 25m 24.0s[1]
Declination+18° 11′ 28″[1]
Redshift729 ± 2 km/s[1]
Distance60 ± 4 Mly (18.5 ± 1.2 Mpc)[2]
Apparent magnitude (V)9.1[3]
Characteristics
TypeSA(s)0+ pec[1]/E2[4]
Size36.99 kiloparsecs (120,600 light-years)[1][5]
(diameter; 2MASS total aperture)
Apparent size (V)7′.1 × 5′.5[1]
Other designations
NGC 4382, UGC 7508, PGC 40515[1]

Pierre Méchain discovered M85 in 1781. It is within the outskirts of the Virgo cluster, and is relatively isolated.[6]

Properties

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M85 is extremely poor in neutral hydrogen[7] and has a very complex outer structure with shells and ripples that are thought to have been caused by a merger with another galaxy that took place between 4 and 7 billion years ago,[7] as well as a relatively young (<3 billion years old) stellar population on its centermost region, some of it in a ring, that may have been created by a late starburst.[8] Like other massive, early-type galaxies, it has different populations of globular clusters. Aside from the typical "red" and "blue" populations, there is also a population with intermediate colors and an even redder population.[6] It is likely transitioning from being a lenticular galaxy into an elliptical galaxy.[6]

While indirect methods imply that Messier 85 should contain a central supermassive black hole of around 100 million solar masses,[9] velocity dispersion observations imply that the galaxy may entirely lack a central massive black hole.[10]

M85 is interacting with the nearby spiral galaxy NGC 4394, and a small elliptical galaxy called MCG 3-32-38.[11]

Compared to other early-type galaxies, M85 emits a relatively smaller proportion of X-rays.[6]

Novae and Supernovae

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  • SN 1960R (type Ia, mag. 13.5), was discovered by H. S. Gates on 20 December 1960,[12] and independently discovered by Leonida Rosino on 18 January 1961.[13]
  • M85 has been the host of the first luminous red nova identified as such. On 7 January 7 the Lick Observatory Supernova Search (LOSS) discovered M85 OT2006-1 on the outskirts of the galaxy.[14]
  • SN 2020nlb (type Ia, mag. 17.436) was discovered by the ATLAS telescope in Hawaii on 25 June 2020.[15][16] This supernova got as bright as magnitude 12.[17]
 
Location of M85

See also

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References

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  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for Messier 85. Retrieved 18 November 2006.
  2. ^ J. L. Tonry; A.Dressler; J. P. Blakeslee; E. A. Ajhar; et al. (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". Astrophysical Journal. 546 (2): 681–693. arXiv:astro-ph/0011223. Bibcode:2001ApJ...546..681T. doi:10.1086/318301. S2CID 17628238.
  3. ^ "Messier 85". SEDS Messier Catalog. Retrieved 30 April 2022.
  4. ^ a b Kormendy, John; Fisher, David B.; Cornell, Mark E.; Bender, Ralf (2009). "Structure and Formation of Elliptical and Spheroidal Galaxies". Astrophysical Journal Supplement. 182 (1): 216–309. arXiv:0810.1681. Bibcode:2009ApJS..182..216K. doi:10.1088/0067-0049/182/1/216. S2CID 119273143.
  5. ^ a b Jarrett, T. H.; Chester, T.; Cutri, R.; Schneider, S. E.; Huchra, J. P. (2003). "The 2MASS Large Galaxy Atlas". The Astronomical Journal. 125 (2): 525. Bibcode:2003AJ....125..525J. doi:10.1086/345794.
  6. ^ a b c d Escudero, Carlos G.; Cortesi, Arianna; Faifer, Favio R.; Sesto, Leandro A.; Smith Castelli, Analía V.; Johnston, Evelyn J.; Reynaldi, Victoria; Chies-Santos, Ana L.; Salinas, Ricardo; Menéndez-Delmestre, Karín; Gonçalves, Thiago S.; Grossi, Marco; Mendes De Oliveira, Claudia (2022). "The complex globular cluster system of the S0 galaxy NGC 4382 in the outskirts of the Virgo Cluster". Monthly Notices of the Royal Astronomical Society. 511 (1): 393–412. arXiv:2201.01759. Bibcode:2022MNRAS.511..393E. doi:10.1093/mnras/stac021.
  7. ^ a b Hibbard, J. E.; Sansom, A. E. (2003). "A Search for H I in Five Elliptical Galaxies with Fine Structure". The Astronomical Journal. 125 (2): 667–683. arXiv:astro-ph/0211003. Bibcode:2003AJ....125..667H. doi:10.1086/345822. S2CID 14748737.
  8. ^ Fisher, David; Franx, Marijn; Illingworth, Garth (1996). "Line Strengths and Line-Strength Gradients in S0 Galaxies". Astrophysical Journal. 459 (1): 110. Bibcode:1996ApJ...459..110F. doi:10.1086/176873.
  9. ^ Kormendy, John; Bender, Ralf (2009). "Correlations between Supermassive Black Holes, Velocity Dispersions, and Mass Deficits in Elliptical Galaxies with Cores". Astrophysical Journal Letters. 691 (2): L142–L146. arXiv:0901.3778. Bibcode:2009ApJ...691L.142K. doi:10.1088/0004-637X/691/2/L142. S2CID 18919128.
  10. ^ Gultekin, Kayhan; Richstone, Douglas O.; et al. (2011). "Is There a Black Hole in NGC 4382?". Astrophysical Journal. 741 (1): L142–L146. arXiv:1108.1808. Bibcode:2011ApJ...741...38G. doi:10.1088/0004-637X/741/1/38. S2CID 411264.
  11. ^ "M85, Lenticular Galaxy". Messier's Nebulae and Star Clusters. Retrieved 29 March 2009.
  12. ^ Bishop, David. "Other Supernovae images, entry for SN 1960R". Rochester Astronomy. Retrieved 30 November 2024.
  13. ^ Thernoe, K. A. (23 January 1961). "Circular No. 1750". Central Bureau for Astronomical Telegrams. Observatory Copenhagen. Retrieved 30 November 2024.
  14. ^ Kulkarni, S. R.; Ofek, E. O.; Rau, A.; Cenko, S. B.; et al. (2007). "An unusually brilliant transient in the galaxy M85". Nature. 447 (7143): 458–460. arXiv:0705.3668. Bibcode:2007Natur.447..458K. doi:10.1038/nature05822. PMID 17522679. S2CID 4300285.
  15. ^ "SN 2020nlb". Transient Name Server. IAU. Retrieved 30 November 2024.
  16. ^ "AstroNote 2020-126". ATLAS20qoq (AT2020nlb): discovery of a candidate SN in MESSIER 85 (17 Mpc). Retrieved 26 June 2020.
  17. ^ Bishop, David. "Supernova 2020nlb in M85". Rochester Astronomy. Retrieved 30 November 2024.
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