NGC 4490

In this article, the topic of NGC 4490 will be addressed from a broad and complete perspective, with the aim of providing relevant information of interest to readers. Different aspects related to NGC 4490, its origin, evolution, impact and relevance today will be analyzed. In addition, different opinions and points of view on NGC 4490 will be explored, in order to enrich the debate and offer a comprehensive vision of the topic. Throughout the article, data, statistics and solid information will be presented to support each argument, in order to provide quality and reliable content for the reader interested in deepening their knowledge about NGC 4490.

NGC 4490
NGC 4490 and satellite galaxy, NGC 4485
Observation data (J2000 epoch)
ConstellationCanes Venatici
Right ascension12h 30m 36.2s[1]
Declination41° 38′ 38″[1]
Redshift565 ± 3 km/s[1]
Distance25.1 ± 5.0 Mly (7.7 ± 1.5 Mpc)[1]
Apparent magnitude (V)9.8
Characteristics
TypeSB(s)d pec [1]
Size53000 ly
Apparent size (V)6.3′ × 3.1′[1]
Other designations
Arp 269, UGC 7651, PGC 41333[1]

NGC 4490, also known as the Cocoon Galaxy, is a barred spiral galaxy in the constellation Canes Venatici. William Herschel discovered it in 1788. It is known to be of the closest interacting/merging galactic system. The galaxy lies at a distance of 25 million light years from Earth making it located in the local universe. It interacts with its smaller companion NGC 4485 and as a result is a starburst galaxy. NGC 4490 and NGC 4485 are collectively known in the Atlas of Peculiar Galaxies as Arp 269. The two galaxies have already made their closest approach and are rushing away from each other. It has been discovered that NGC 4490 has a double nucleus.[2]

NGC 4490 is located 3/4° northwest of beta Canum Venaticorum and with apparent visual magnitude 9.8, can be observed with 15x100 binoculars.[3] It is a member of the Herschel 400 Catalogue. It belongs to the Canes II Group. NGC 4490 has a system of satellite galaxies oriented roughly in a plane.[4]

Stellar stream

A stellar stream 25,000 light years long connects the two interacting galaxies. The stellar stream is made of bright knots and large gas rich pockets. Young blue hot massive stars are formed in this region.[5]

Supernovae

Two supernovae have been observed in NGC 4490:

  • Extreme tidal forces have carved out the shapes and properties of NGC 4490.
    Extreme tidal forces have carved out the shapes and properties of NGC 4490.[12]

See also

References

  1. ^ a b c d e f g "NASA/IPAC Extragalactic Database". Results for NGC 4490. Retrieved 2016-01-18.
  2. ^ Lawrence, A. L.; Kerton, C. R.; Struck, Curtis; Smith, Beverly J. (2020-02-27). "Revealing the Double Nucleus of NGC 4490". The Astrophysical Journal. 891 (1): 11. arXiv:2001.05601. Bibcode:2020ApJ...891...11L. doi:10.3847/1538-4357/ab6c6a. ISSN 1538-4357.
  3. ^ Craig Crossen, Gerald Rhemann (2012). Sky Vistas: Astronomy for Binoculars and Richest-Field Telescopes. Springer Science+Business Media. p. 233. ISBN 978-3-7091-0626-6.
  4. ^ Pawlowski, Marcel S.; Müller, Oliver; Taibi, Salvatore; Júlio, Mariana P.; Kanehisa, Kosuke Jamie; Heesters, Nick (2024). "The satellite galaxy plane of NGC 4490 in light of ΛCDM". Astronomy & Astrophysics. 688: A153. arXiv:2405.06016. Bibcode:2024A&A...688A.153P. doi:10.1051/0004-6361/202449954.
  5. ^ [email protected]. "Distant view of a galactic crash — NGC 4490 and NGC 4485 (ground-based image)". www.spacetelescope.org. Retrieved 2023-11-25.
  6. ^ Wild, P. (1982). "Probable Supernova in NGC 4490". International Astronomical Union Circular (3689): 1. Bibcode:1982IAUC.3689....1W.
  7. ^ "SN 1982F". Transient Name Server. IAU. Retrieved 5 December 2024.
  8. ^ Mostardi, R.; Li, W.; Filippenko, A. V. (2008). "Possible Supernova in NGC 4490". Central Bureau Electronic Telegrams (1280): 1. Bibcode:2008CBET.1280....1M.
  9. ^ Nakano, S. (2008). "Supernova 2008ax in NGC 4490". Central Bureau Electronic Telegrams (1286): 1. Bibcode:2008CBET.1286....1N.
  10. ^ David Bishop. "Supernova 2008ax in NGC 4490". Rochester Astronomy. Retrieved 5 December 2024.
  11. ^ "SN 2008ax". Transient Name Server. IAU. Retrieved 5 December 2024.
  12. ^ "Bursting with Starbirth". www.spacetelescope.org. Retrieved 28 September 2017.
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