NGC 7679

Last updated
NGC 7679
Arp 216.png
Hubble Space Telescope (HST) image of the galaxy
Observation data (J2000 epoch)
Constellation Pisces
Right ascension 23h 28m 46.7s [1]
Declination +03° 30′ 41″ [1]
Redshift 0.017139 ± 0.000013
Helio radial velocity 5,138 ± 4 km/s [1]
Distance 191 ± 11 Mly (58.6 ± 3.3 Mpc) [1]
Apparent magnitude  (V)12.5 [2]
Characteristics
Type SB0 pec [1]
Apparent size  (V)1.3′ × 0.9′ [1]
Notable features Seyfert galaxy, starburst
Other designations
UGC 12618, Arp 216, MCG +00-59-046, CGCG 380-061, VV 329, PGC 71554, Mrk 534 [1]

NGC 7679 is a lenticular galaxy with a peculiar morphology in the constellation Pisces. It is located at a distance of circa 200 million light years from Earth, which, given its apparent dimensions, means that NGC 7679 is about 60,000 light years across. It was discovered by Heinrich d'Arrest on September 23, 1864. [3] The total infrared luminosity is 1011.05  L☉ , and thus it is categorised as a luminous infrared galaxy. [4] NGC 7679 is both a starburst galaxy and a Seyfert galaxy. [5]

Contents

Characteristics

NGC 7679 is a barred lenticular galaxy seen face on, [6] and is noted for its distorted shape. The galaxy has two plumes in opposite directions, possibly the result of tidal interaction with NGC 7682, and smooth outer arms. The inner region is of high surface brightness with many knots and a high star formation rate. [7] The star formation rate of the galaxy is estimated to be 80 M☉ per year based on the x-ray luminosity observed by XMM-Newton, [8] and on the H-alpha luminosity of 21.2 ± 0.2 M☉ per year while observations in infrared indicate a star formation of 11.35 ± 0.6 M☉ per year. [9]

There is evidence of massive starburst activity in the circumnuclear region, with 35% of the stars there being aged less than 10 million years. [10] A ring of ionised gas dominates both the optical and infrared wavelengths and is the locus of the starburst activity. [11]

Nucleus

The nucleus of NGC 7679 has been found to be active and has been categorised as a Seyfert galaxy. The most accepted theory for the energy source of Seyfert galaxies is the presence of an accretion disk around a supermassive black hole. NGC 7679 is believed to host a supermassive black hole whose mass is estimated to be 5.9×106 (106.77) M☉ based on velocity dispersion. [12]

The X-ray spectrum from BeppoSAX shows no significant absorption above 2 MeV and the iron Ka line was marginally detected. [13] However, the galaxy shows signs of obstruction in visual light, as it lacks broad emission lines. Two possible reasons are the presence of dust or the accretion disk that produces X-rays is not obstructed but the broad line region is. [14] The lack of X-ray absorption along with the presence of broad H-alpha lines but not broad H-beta mean that it cannot be easily categorised as a particular type of Seyfert galaxy. [5]

Nearby galaxies

NGC 7679 forms a pair with NGC 7682. NGC 7682 lies at a distance of 269.7 arcseconds, which corresponds to a projected distance of 97 kpc. [8] The two galaxies are connected by a hydrogen bridge, a sign of a closer encounter in the past 500 million years. [11] It is possible that the interaction of the two galaxies caused star formation in NGC 7679. [6] A fainter galaxy has been found superimposed on the eastern arm of the galaxy, but it is actually located in the background. [11]

See also

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that has a much-higher-than-normal luminosity over at least some portion of the electromagnetic spectrum with characteristics indicating that the luminosity is not produced by stars. Such excess non-stellar emission has 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">Eyes Galaxies</span> Pair of galaxies in the constellation Virgo

The Eyes Galaxies are a pair of galaxies about 52 million light-years away in the constellation Virgo. The pair are members of the string of galaxies known as Markarian's Chain.

Luminous infrared galaxies or LIRGs are galaxies with luminosities, the measurement of brightness, above 1011 L☉. They are also referred to as submillimeter galaxies (SMGs) through their normal method of detection. LIRGs are more abundant than starburst galaxies, Seyfert galaxies and quasi-stellar objects at comparable luminosity. Infrared galaxies emit more energy in the infrared than at all other wavelengths combined. A LIRG's luminosity is 100 billion times that of the Sun.

<span class="mw-page-title-main">NGC 1672</span> Galaxy in the constellation Dorado

NGC 1672 is a barred spiral galaxy located in the constellation Dorado. It was discovered by the astronomer James Dunlop on November 5, 1826. It was originally unclear whether it was a member of the Dorado Group, with some sources finding it to be a member and other sources rejecting its membership. However, recent tip of the red-giant branch (TRGB) measurements indicate that NGC 1672 is located at the same distance as other members, suggesting it is indeed a member of the Dorado Group.

<span class="mw-page-title-main">NGC 4102</span> Galaxy in the constellation Ursa Major

NGC 4102 is an intermediate barred spiral galaxy located in the northern constellation of Ursa Major. It is visible in a small telescope and has an apparent visual magnitude of 11.2. The galaxy was discovered April 12, 1789 by William Herschel. J. L. E. Dreyer described it as "bright, pretty small, round, brighter middle and bright nucleus". This galaxy is located at a distance of 60 million light years and is receding with a heliocentric radial velocity of 837 km/s. It is a member of the Ursa Major group of galaxies.

<span class="mw-page-title-main">NGC 1614</span> Galaxy in the constellation Eridanus

NGC 1614 is the New General Catalogue identifier for a spiral galaxy in the equatorial constellation of Eridanus. It was discovered on December 29, 1885 by American astronomer Lewis Swift, who described it in a shorthand notation as: pretty faint, small, round, a little brighter middle. The nebula was then catalogued by Danish-Irish astronomer J. L. E. Drayer in 1888. When direct photography became available, it was noted that this galaxy displayed some conspicuous peculiarities. American astronomer Halton Arp included it in his 1966 Atlas of Peculiar Galaxies. In 1971, Swiss astronomer Fritz Zwicky described it as a "blue post-eruptive galaxy, compact patchy core, spiral plumes, long blue jet SSW".

<span class="mw-page-title-main">NGC 2992</span> Seyfert galaxy in the constellation Hydra

NGC 2992 is a Seyfert galaxy located 103 million light years distant in the equatorial constellation of Hydra. It was discovered in 1785 by Anglo-German astronomer William Herschel.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<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 4939</span> Spiral galaxy in the constellation Virgo

NGC 4939 is a spiral galaxy located in the constellation Virgo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 4939 is about 190,000 light years across. It was discovered by William Herschel on March 25, 1786.

<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 985</span> Ring galaxy in the constellation Cetus

NGC 985 is a ring galaxy in the constellation of Cetus. It is located about 550 million light years away from Earth, which means, given its apparent dimensions, that NGC 985 is approximately 160,000 light years across. It was discovered by Francis Leavenworth in 1886. It is a type 1 Seyfert galaxy.

<span class="mw-page-title-main">NGC 6951</span> Galaxy in the constellation Cepheus

NGC 6951 is a barred spiral galaxy located in the constellation Cepheus. It is located at a distance of about 75 million light-years from Earth, which, given its apparent dimensions, means that NGC 6951 is about 100,000 light-years across. It was discovered by Jérôme Eugène Coggia in 1877 and independently by Lewis Swift in 1878.

<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 2273</span> Galaxy in the constellation Lynx

NGC 2273 is a barred spiral galaxy located in the constellation Lynx. It is located at a distance of circa 95 million light years from Earth, which, given its apparent dimensions, means that NGC 2273 is about 100,000 light years across. It was discovered by Nils Dunér on September 15, 1867.

<span class="mw-page-title-main">NGC 7592</span> Interacting galaxy system in the constellation Aquarius

NGC 7592 is an interacting galaxy system located 300 million light years away in the constellation Aquarius. It was discovered by William Herschel on September 20, 1784. The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy. One of the galaxies hosts a type 2 Seyfert nucleus.

<span class="mw-page-title-main">NGC 2617</span> Galaxy in the constellation Hydra

NGC 2617 is a Seyfert galaxy in the equatorial constellation of Hydra. It was discovered on February 12, 1885, by French astronomer Édouard Stephan. In 1888, Danish astronomer J. L. E. Dreyer described it as "extremely faint, very small, 2 very faint stars involved". It is located at an estimated distance of 202 million light years. In the infrared, the galaxy has an angular size of 0.693 by 0.652 arcminutes.

<span class="mw-page-title-main">NGC 7172</span> Galaxy in the constellation of Piscis Austrinus

NGC 7172 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 110 million light years from Earth, which, given its apparent dimensions, means that NGC 7172 is about 100,000 light years across. It was discovered by John Herschel on September 23, 1834.

<span class="mw-page-title-main">NGC 4253</span> Galaxy in the constellation of Coma Berenices

NGC 4253 is a barred spiral galaxy located in the constellation Coma Berenices. It is located at a distance of about 185 million light years from Earth, which, given its apparent dimensions, means that NGC 4253 is about 65,000 light years across. It was discovered by William Herschel on February 3, 1788. It is a Seyfert galaxy.

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 7679. Retrieved 2020-11-03.
  2. ↑ "Revised NGC Data for NGC 7679". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 7679 (= PGC 71554)". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Sanders, D. B.; Mazzarella, J. M.; Kim, D.-C.; Surace, J. A.; Soifer, B. T. (October 2003). "The IRAS Revised Bright Galaxy Sample". The Astronomical Journal. 126 (4): 1607–1664. arXiv: astro-ph/0306263 . Bibcode:2003AJ....126.1607S. doi:10.1086/376841. S2CID   14825701.
  5. 1 2 Della Ceca, R.; Pellegrini, S.; Bassani, L.; Beckmann, V.; Cappi, M.; Palumbo, G. G. C.; Trinchieri, G.; Wolter, A. (September 2001). "Unveiling the AGN powering the "Composite" Seyfert/Star-forming galaxy NGC 7679: BeppoSAX and ASCA results". Astronomy & Astrophysics. 375 (3): 781–790. arXiv: astro-ph/0106444 . Bibcode:2001A&A...375..781D. doi: 10.1051/0004-6361:20010913 .
  6. 1 2 Yankulova, I. M.; Golev, V. K.; Jockers, K. (July 2007). "The luminous infrared composite Seyfert 2 galaxy NGC 7679 through the [O III] λ 5007 emission line". Astronomy & Astrophysics. 469 (3): 891–898. doi: 10.1051/0004-6361:20077440 .
  7. ↑ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  8. 1 2 Ricci, C.; Bauer, F. E.; Treister, E.; Schawinski, K.; Privon, G. C.; Blecha, L.; Arevalo, P.; Armus, L.; Harrison, F.; Ho, L. C.; Iwasawa, K.; Sanders, D. B.; Stern, D. (23 January 2017). "Growing supermassive black holes in the late stages of galaxy mergers are heavily obscured". Monthly Notices of the Royal Astronomical Society: stx173. doi: 10.1093/mnras/stx173 .
  9. ↑ Davies, Rebecca L.; Groves, Brent; Kewley, Lisa J.; Dopita, Michael A.; Hampton, Elise J.; Shastri, Prajval; Scharwächter, Julia; Sutherland, Ralph; Kharb, Preeti; Bhatt, Harish; Jin, Chichuan; Banfield, Julie; Zaw, Ingyin; James, Bethan; Juneau, Stéphanie; Srivastava, Shweta (21 October 2016). "Dissecting galaxies: spatial and spectral separation of emission excited by star formation and AGN activity". Monthly Notices of the Royal Astronomical Society. 462 (2): 1616–1629. doi: 10.1093/mnras/stw1754 .
  10. ↑ Gu, Q. S.; Huang, J. H.; de Diego, J. A.; Dultzin-Hacyan, D.; Lei, S. J.; Benítez, E. (August 2001). "The nuclear starburst activity in the Seyfert 2 galaxy NGC 7679". Astronomy & Astrophysics. 374 (3): 932–935. arXiv: astro-ph/0106165 . Bibcode:2001A&A...374..932G. doi: 10.1051/0004-6361:20010806 .
  11. 1 2 3 Buson, L. M.; Cappellari, M.; Corsini, E. M.; Held, E. V.; Lim, J.; Pizzella, A. (February 2006). "NGC 7679: an anomalous, composite Seyfert 1 galaxy whose X-ray luminous AGN vanishes at optical wavelengths". Astronomy & Astrophysics. 447 (2): 441–451. arXiv: astro-ph/0510034 . Bibcode:2006A&A...447..441B. doi: 10.1051/0004-6361:20053204 .
  12. ↑ Alonso-Herrero, Almudena; Pereira-Santaella, Miguel; Rieke, George H.; Diamond-Stanic, Aleksandar M.; Wang, Yiping; Hernán-Caballero, Antonio; Rigopoulou, Dimitra (19 February 2013). "Local luminous infrared galaxies. III. Co-evolution of black hole growth and star formation activity?". The Astrophysical Journal. 765 (2): 78. arXiv: 1301.4015 . Bibcode:2013ApJ...765...78A. doi:10.1088/0004-637X/765/2/78. hdl: 10261/109183 . S2CID   119215482.
  13. ↑ Dadina, M. (January 2007). "BeppoSAX observations in the 2–100 keV band of the nearby Seyfert galaxies: an atlas of spectra". Astronomy & Astrophysics. 461 (3): 1209–1252. Bibcode:2007A&A...461.1209D. doi: 10.1051/0004-6361:20065734 .
  14. ↑ Risaliti, G. (May 2002). "The BeppoSAX view of bright Compton-thin Seyfert 2 galaxies". Astronomy & Astrophysics. 386 (2): 379–398. arXiv: astro-ph/0202392 . Bibcode:2002A&A...386..379R. doi: 10.1051/0004-6361:20020170 .
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