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NGC 7319

Today we are preparing to enter the exciting world of NGC 7319. Whether it is a historical figure, a current topic, a social phenomenon or any other aspect that catches our attention, NGC 7319 undoubtedly has a significant impact on our lives. Throughout this article we will explore various perspectives, analyze relevant data and present expert opinions in order to fully understand the importance and relevance of NGC 7319 in the current context. We're excited to dive into this topic and discover everything NGC 7319 has to offer us.

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NGC 7319
NGC 7319 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationPegasus
Right ascension22h 36m 03.56s[1]
Declination+33° 58′ 32.7″[1]
Redshift0.022[1]
Heliocentric radial velocity6,740 km/s[2]
Distance311 Mly (95.3 Mpc)[1]
Apparent magnitude (V)14.1[3]
Characteristics
TypeSB(s)bc pec[3]
Size25.09 kiloparsecs (81,800 light-years) (diameter; 25.0 mag/arcsec2 B-band isophote)[3]
Apparent size (V)1′.7 × 1′.3[3]
Other designations
NGC 7319, UGC 12102, LEDA 69269, PGC 69269[4][3]

NGC 7319 is a highly distorted barred spiral galaxy that is a member of the compact Stephan's Quintet[5] group located in the constellation Pegasus, some 311 megalight-years distant from the Milky Way.[1] It was discovered on 27 September 1873 by French astronomer Édouard Stephan.[6]

The galaxy's arms, dust and gas have been highly disturbed as a result of the interaction with the other members of the Quintet. Nearly all of the neutral hydrogen has been stripped from this galaxy, most likely as a result of a collision with NGC 7320c some 100 million years ago.[7] A pair of long, parallel tidal tails extend southward from NGC 7319 in the direction of NGC 7320c, and is undergoing star formation.[8]

This is a type 2 Seyfert galaxy[1] with one of the largest circumnuclear outflows known in galaxies of this type. This outflow reaches velocities of up to 500 km/s and spans 13 kly. The star formation rate appears normal for a spiral galaxy at 1.98±0.58 M☉ yr−1, and the majority (68%) is occurring in the spiral arms.[8] The core appears faint in the ultraviolet band, indicating heavy extinction within the active galactic nucleus.[8] There is a three component radio source with an overall size of 5.5 kly that is straddling the nucleus.[9] A strong X-ray source with a high redshift has been detected at a separation of 8″ from the galactic nucleus, a quasi-stellar object.[2]

Supernova

One supernova has been observed in NGC 7319: SN 1971P (type unknown, mag. 16.8) was discovered by Leonida Rosino on 19 August 1971.[10][11]

See also

References

  1. ^ a b c d e f Koss, Michael; et al. (October 2011). "Host Galaxy Properties of the Swift Bat Ultra Hard X-Ray Selected Active Galactic Nucleus". The Astrophysical Journal. 739 (2): 20. arXiv:1107.1237. Bibcode:2011ApJ...739...57K. doi:10.1088/0004-637X/739/2/57. S2CID 118119154. 57.
  2. ^ a b Galianni, Pasquale; et al. (February 2005). "The Discovery of a High-Redshift X-Ray-Emitting QSO Very Close to the Nucleus of NGC 7319". The Astrophysical Journal. 620 (1): 88–94. arXiv:astro-ph/0409215. Bibcode:2005ApJ...620...88G. doi:10.1086/426886. S2CID 757970.
  3. ^ a b c d e "NASA/IPAC Extragalactic Database". Results for NGC 7319. Retrieved 2007-04-21.
  4. ^ "NGC 7319". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-10-08.
  5. ^ Di Mille, F.; et al. (October 2008). Funes, José G.; J., S.; Corsini, Enrico Maria (eds.). 3D Spectroscopy of the Nuclear Environment of a Selected Sample of Nearby Active Galactic Nuclei: NGC 7319. Formation and Evolution of Galaxy Disks. Proceedings of the conference held 1–5 October 2007 at the Centro Convegni Matteo Ricci, Rome, Italy. ASP Conference Series. Vol. 396. San Francisco: Astronomical Society of the Pacific. p. 61. Bibcode:2008ASPC..396...61D.
  6. ^ Seligman, Courtney. "New General Catalogue Objects: NGC 7319". Celestial Atlas. Retrieved 28 August 2024.
  7. ^ Moles, M.; et al. (August 1997). "The Dynamical Status of Stephan's Quintet". The Astrophysical Journal. 485 (2): L69 – L73. arXiv:astro-ph/9707194. Bibcode:1997ApJ...485L..69M. doi:10.1086/310817. S2CID 19033219.
  8. ^ a b c Xu, C. Kevin; et al. (January 2005). "Ultraviolet Emission and Star Formation in Stephan's Quintet". The Astrophysical Journal. 619 (1): L95 – L98. arXiv:astro-ph/0411319. Bibcode:2005ApJ...619L..95X. doi:10.1086/425130. S2CID 119371650.
  9. ^ Aoki, Kentaro; et al. (August 1999). "The Radio Emission of the Seyfert Galaxy NGC 7319". The Astrophysical Journal. 521 (2): 565–571. arXiv:astro-ph/9812365. Bibcode:1999ApJ...521..565A. doi:10.1086/307559. S2CID 8435704.
  10. ^ Rosino, L. (16 September 1971). "Possible Supernova in NGC 7319". Central Bureau for Astronomical Telegrams. 2355. Smithsonian Astrophysical Observatory, IAU: 1. Retrieved 15 August 2025.
  11. ^ "SN 1971P". Transient Name Server. IAU. Retrieved 15 August 2025.
  • Media related to NGC 7319 at Wikimedia Commons
  • NGC 7319 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images


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