NGC 7319

Last updated
NGC 7319
NGC 7319.jpg
NGC 7319 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Pegasus
Right ascension 22h 36m 03.56s [1]
Declination +33° 58′ 32.7″ [1]
Redshift 0.022 [1]
Heliocentric radial velocity 6,740 km/s [2]
Distance 311  Mly (95.3  Mpc) [1]
Apparent magnitude  (V)14.1 [3]
Characteristics
Type SB(s)bc pec [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] 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. [6] A pair of long, parallel tidal tails extend southward from NGC 7319 in the direction of NGC 7320c, and is undergoing star formation. [7]

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. [7] The core appears faint in the ultraviolet band, indicating heavy extinction within the active galactic nucleus. [7] There is a three component radio source with an overall size of 5.5 kly that is straddling the nucleus. [8] 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]

One supernova has been observed in NGC 7319: On 19 August 1971, Leonida Rosino discovered SN 1971P (type unknown, mag. 16.8). [9]

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that the luminosity is not produced by stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

<span class="mw-page-title-main">Seyfert galaxy</span> Class of active galaxies with very bright nuclei

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.

<span class="mw-page-title-main">Black Eye Galaxy</span> Spiral galaxy in the constellation Coma Berenices

The Black Eye Galaxy is a relatively isolated spiral galaxy 17 million light-years away in the mildly northern constellation of Coma Berenices. It was discovered by Edward Pigott in March 1779, and independently by Johann Elert Bode in April of the same year, as well as by Charles Messier the next year. A dark band of absorbing dust partially in front of its bright nucleus gave rise to its nicknames of the "Black Eye", "Evil Eye", or "Sleeping Beauty" galaxy. M64 is well known among amateur astronomers due to its form in small telescopes and visibility across inhabited latitudes.

<span class="mw-page-title-main">Messier 77</span> Barred spiral galaxy in the constellation Cetus

Messier 77 (M77), also known as NGC 1068 or the Squid Galaxy, is a barred spiral galaxy in the constellation Cetus. It is about 47 million light-years (14 Mpc) away from Earth. Messier 77 was discovered by Pierre Méchain in 1780, who originally described it as a nebula. Méchain then communicated his discovery to Charles Messier, who subsequently listed the object in his catalog. Both Messier and William Herschel described this galaxy as a star cluster. Today, however, the object is known to be a galaxy.

<span class="mw-page-title-main">NGC 4395</span> Galaxy in the constellation Canes Venatici

NGC 4395 is a nearby low surface brightness spiral galaxy located about 14 million light-years from Earth in the constellation Canes Venatici. The nucleus of NGC 4395 is active and the galaxy is classified as a Seyfert Type I known for its very low-mass supermassive black hole. It is one of the lowest

<span class="mw-page-title-main">NGC 3227</span> Galaxy in the constellation Leo

NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 3226</span> Dwarf elliptical galaxy in the constellation Leo

NGC 3226 is a dwarf elliptical galaxy that is interacting with the spiral galaxy NGC 3227. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 3486</span> Galaxy in the constellation Leo Minor

NGC 3486 is an intermediate barred spiral galaxy located about 27.4 million light years away in the constellation of Leo Minor. It has a morphological classification of SAB(r)c, which indicates it is a weakly barred spiral with an inner ring and loosely wound arms. This is a borderline, low-luminosity Seyfert galaxy with an active nucleus. However, no radio or X-ray emission has been detected from the core, and it may only have a small supermassive black hole with less than a million times the mass of the Sun.

<span class="mw-page-title-main">NGC 520</span> Pair of colliding spiral galaxies in the constellation Pisces

NGC 520 is a pair of colliding spiral galaxies about 105 million light-years away in the constellation Pisces. They were discovered by astronomer William Herschel on 13 December 1784.

<span class="mw-page-title-main">NGC 5548</span> Type I Seyfert galaxy in the constellation Boötes

NGC 5548 is a Type I Seyfert galaxy with a bright, active nucleus. This activity is caused by matter flowing onto a 65 million solar mass (M☉) supermassive black hole at the core. Morphologically, this is an unbarred lenticular galaxy with tightly-wound spiral arms, while shell and tidal tail features suggest that it has undergone a cosmologically-recent merger or interaction event. NGC 5548 is approximately 245 million light years away and appears in the constellation Boötes. The apparent visual magnitude of NGC 5548 is approximately 13.3 in the V band.

<span class="mw-page-title-main">NGC 3259</span> Galaxy in the constellation Ursa Major

NGC 3259 is a barred spiral galaxy located approximately 90 million light-years from Earth, in the Ursa Major constellation. It has the morphological classification SAB(rs)bc, which indicates that it is a spiral galaxy with a weak bar across the nucleus (SAB), an incomplete inner ring structure circling the bar (rs), and moderate to loosely wound spiral arms (bc). This galaxy is a known source of X-ray emission and it has an active galactic nucleus of the Seyfert 2 type.

<span class="mw-page-title-main">NGC 3783</span> Galaxy in the constellation Centaurus

NGC 3783 is a barred spiral galaxy located about 135 million light years away in the constellation Centaurus. It is inclined by an angle of 23° to the line of sight from the Earth along a position angle of about 163°. The morphological classification of SBa indicates a bar structure across the center (B) and tightly-wound spiral arms (a). Although not shown by this classification, observers note the galaxy has a luminous inner ring surrounding the bar structure. The bright compact nucleus is active and categorized as a Seyfert 1 type. This nucleus is a strong source of X-ray emission and undergoes variations in emission across the electromagnetic spectrum.

<span class="mw-page-title-main">NGC 4698</span> Galaxy in the constellation Virgo

NGC 4698 is a barred spiral galaxy located around 55 million light years away from Earth in the constellation of Virgo. It belongs to the Virgo Cluster of galaxies and is positioned near the northeastern edge of this assemblage. The morphological classification of NGC 4698 in the De Vaucouleurs system is SA(s)ab, which indicates a purely spiral structure with moderate to tightly wound arms. It is inclined to the line of sight from the Earth by an angle of 53° along a position angle of 170°.

<span class="mw-page-title-main">NGC 4041</span> Spiral galaxy in the constellation Ursa Major

NGC 4041 is the New General Catalogue identifier for a spiral galaxy in the northern circumpolar constellation of Ursa Major. It is located an estimated 70 million light years from the Sun. The morphological classification of SA(rs)bc indicates this is a spiral galaxy the lacks a bar; the 'rs' means it has a weakly-formed ring structure, and the 'bc' indicates the spiral arms are moderately to loosely wound.

<span class="mw-page-title-main">NGC 4293</span> Galaxy in the constellation Coma Berenices

NGC 4293 is a lenticular galaxy in the northern constellation of Coma Berenices. It was discovered by English astronomer William Herschel on March 14, 1784, who described it as "large, extended, resolvable, 6 or 7′ long". This galaxy is positioned to the north-northwest of the star 11 Comae Berenices and is a member of the Virgo Cluster of galaxies. It is assumed to lie at the same distance as the Virgo Cluster itself: around 54 million light years away. The galaxy spans an apparent area of 5.3 × 3.1 arc minutes.

<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

NGC 7469 is an intermediate spiral galaxy in the constellation of Pegasus. NGC 7469 is located about 200 million light-years away from Earth, which means, given its apparent dimensions, that NGC 7469 is approximately 90,000 light-years across. It was discovered by William Herschel on November 12, 1784.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<span class="mw-page-title-main">NGC 1386</span> Galaxy in the constellation Eridanus

NGC 1386 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 53 million light years from Earth, which, given its apparent dimensions, means that NGC 1386 is about 50,000 light years across. It is a Seyfert galaxy, the only one in Fornax Cluster.

<span class="mw-page-title-main">NGC 1241</span> Galaxy in the constellation Eridanus

NGC 1241 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 150 million light years from Earth, which, given its apparent dimensions, means that NGC 1241 is about 140,000 light years across. It was discovered by William Herschel on January 10, 1785. It is classified as a Seyfert galaxy.

<span class="mw-page-title-main">NGC 1142</span> Interacting and distorted spiral galaxy in the constellation Cetus

NGC 1142 is a distorted spiral galaxy in the constellation of Cetus. It is located about 370 million light years away from Earth, which means, given its apparent dimensions, that NGC 1142 is approximately 170,000 light years across. It is a type 2 Seyfert galaxy. It interacts with the elliptical galaxy NGC 1141.

References

  1. 1 2 3 4 5 6 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. 1 2 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. 1 2 3 4 "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. ↑ 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.
  7. 1 2 3 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.
  8. ↑ 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.
  9. ↑ Transient Name Server entry for SN 1971P. Retrieved 25 March 2023.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.