NGC 5419

NGC 5419
The elliptical galaxy NGC 5419.
Observation data (J2000 epoch)
ConstellationCentaurus
Right ascension14h 03m 38.7349s[1]
Declination−33° 58′ 41.809″[1]
Redshift0.013763[1]
Heliocentric radial velocity4126 ± 15 km/s[1]
Distance210.5 ± 14.8 Mly (64.53 ± 4.54 Mpc)[1]
Group or clusterNGC 5488 Group (LGG 369)
Apparent magnitude (V)10.8[1]
Characteristics
TypeE[1]
Size~428,600 ly (131.42 kpc) (estimated)[1]
Apparent size (V)4.1' x 3.3'[1]
Other designations
2MASX J14033877-3358422, MCG -06-31-019, PGC 50100, ESO 384- G 039[1]

NGC 5419 is a large elliptical galaxy in the constellation of Centaurus. Its velocity with respect to the cosmic microwave background is 4,375 ± 23 km/s, which corresponds to a Hubble distance of 64.5 ± 4.5 Mpc (∼210 million light-years).[1] It was discovered by British astronomer John Herschel on 1 May 1834.[2]

NGC 5419 is the brightest cluster galaxy of the galaxy cluster, Abell S0753.[3] It contains a large core with a radius span of 1.58 arcsec (≈55 pc). In addition, it has a double nucleus, indicating the presence of two supermassive black holes in the center with a separation gap of only ≈70 pc.[4][5][6]

Supernovae

Two supernovae have been observed in NGC 5419:

NGC 5488 Group

According to A.M. Garcia, the galaxy NGC 5419 is part of the NGC 5488 group (also known as LGG 369). This group of galaxies has 14 members: NGC 5397, NGC 5488, IC 4366 and nine galaxies from the ESO catalog.[9]

See also

References

  1. ^ a b c d e f g h i j k "Results for object NGC 5419". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 28 July 2024.
  2. ^ Seligman, Courtney. "New General Catalogue Objects: NGC 5419". Celestial Atlas. Retrieved 13 December 2024.
  3. ^ Coziol, R.; Andernach, H.; Caretta, C. A.; Alamo-Martínez, K. A.; Tago, E. (2009-06-01). "The Dynamical State of Brightest Cluster Galaxies and The Formation of Clusters". The Astronomical Journal. 137 (6): 4795–4809. arXiv:0903.2360. Bibcode:2009AJ....137.4795C. doi:10.1088/0004-6256/137/6/4795. ISSN 0004-6256.
  4. ^ Mazzalay, Ximena; Thomas, Jens; Saglia, Roberto P.; Wegner, Gary A.; Bender, Ralf; Erwin, Peter; Fabricius, Maximilian H.; Rusli, Stephanie P. (2016-11-01). "The supermassive black hole and double nucleus of the core elliptical NGC 5419". Monthly Notices of the Royal Astronomical Society. 462 (3): 2847–2860. arXiv:1607.06466. Bibcode:2016MNRAS.462.2847M. doi:10.1093/mnras/stw1802. ISSN 0035-8711.
  5. ^ Neureiter, Bianca; Thomas, Jens; Rantala, Antti; Naab, Thorsten; Mehrgan, Kianusch; Saglia, Roberto; de Nicola, Stefano; Bender, Ralf (2023-06-01). "The isotropic center of NGC 5419 -- A core in formation?". The Astrophysical Journal. 950 (1): 15. arXiv:2305.03078. Bibcode:2023ApJ...950...15N. doi:10.3847/1538-4357/accffa. ISSN 0004-637X.
  6. ^ Arzoumanian, Zaven; Baker, Paul T.; Brazier, Adam; Brook, Paul R.; Burke-Spolaor, Sarah; Becsy, Bence; Charisi, Maria; Chatterjee, Shami; Cordes, James M.; Cornish, Neil J.; Crawford, Fronefield; Cromartie, H. Thankful; Decesar, Megan E.; Demorest, Paul B.; Dolch, Timothy (2021-06-01). "The NANOGrav 11 yr Data Set: Limits on Supermassive Black Hole Binaries in Galaxies within 500 Mpc". The Astrophysical Journal. 914 (2): 121. arXiv:2101.02716. Bibcode:2021ApJ...914..121A. doi:10.3847/1538-4357/abfcd3. ISSN 0004-637X.
  7. ^ "SN 2018zz". Transient Name Server. IAU. Retrieved 13 December 2024.
  8. ^ "SN 2020alh". Transient Name Server. IAU. Retrieved 13 December 2024.
  9. ^ Garcia, A. M. (1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47. Bibcode:1993A&AS..100...47G.