NGC 2911

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NGC 2911
NGC2911 - SDSS DR14.jpg
NGC 2911 by Sloan Digital Sky Survey
Observation data (J2000 epoch)
Constellation Leo
Right ascension 09h 33m 46.1s [1]
Declination +10° 09′ 09″ [1]
Redshift 0.010777 ± 0.000007 [1]
Heliocentric radial velocity 3,231 ± 2 km/s [1]
Distance 145 Mly (48.5 Mpc) [1]
Apparent magnitude  (V)11.5 [2]
Characteristics
Type SA(s)0:pec [1]
Apparent size  (V)4.1′ × 3.2′ [1]
Other designations
UGC 5092, Arp 232, MCG +02-25-003, PGC 27159 [1]

NGC 2911 is a peculiar lenticular galaxy in the constellation Leo. The galaxy lies about 145 million light years away from Earth, which means, given its apparent dimensions, that NGC 2911 is approximately 165,000 light years across. It was discovered by William Herschel on March 11, 1784. [3]

Contents

The galaxy features dust lanes. [4] The kinematic axis of the molecular gas of the galaxy isn't aligned with the stellar one, indicating it is of external origin. [5] The nucleus of the galaxy has been found to be active and it is categorised as a type 2 LINER. [6] The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. The supermassive black hole in the nucleus of NGC 5953 is estimated to have a mass of 2.7×108  M☉ based on stellar velocity dispersion. [7] A one-sided jet measuring about half parsec in length is visible in radiowaves. [8] [9]

NGC 2911 is the foremost member of a galaxy group known as NGC 2911 group or LGG 177. Other members of the group include the galaxies NGC 2912, NGC 2913, NGC 2914, and NGC 2939. [10] NGC 2912 lies at a distance of 1.3 arcminutes while NGC 2914 lies at a distance of 4.8 arcminutes. [4] [11] NGC 2919 appears next to the group but it isn't a member of it. A bit further away from the NGC 2911 group lies NGC 2872 and its group, the UGC 5189 group and the CGCG 063-066 group. [12]

See also

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 this luminosity is not produced by the 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">Messier 87</span> Elliptical galaxy in the Virgo Galaxy Cluster

Messier 87 is a supergiant elliptical galaxy in the constellation Virgo that contains several trillion stars. One of the largest and most massive galaxies in the local universe, it has a large population of globular clusters—about 15,000 compared with the 150–200 orbiting the Milky Way—and a jet of energetic plasma that originates at the core and extends at least 1,500 parsecs, traveling at a relativistic speed. It is one of the brightest radio sources in the sky and a popular target for both amateur and professional astronomers.

<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.

<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">Low-ionization nuclear emission-line region</span> Type of galactic nucleus

A low-ionization nuclear emission-line region (LINER) is a type of galactic nucleus that is defined by its spectral line emission. The spectra typically include line emission from weakly ionized or neutral atoms, such as O, O+, N+, and S+. Conversely, the spectral line emission from strongly ionized atoms, such as O++, Ne++, and He+, is relatively weak. The class of galactic nuclei was first identified by Timothy Heckman in the third of a series of papers on the spectra of galactic nuclei that were published in 1980.

<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 3367</span> Spiral galaxy in the constellation Leo

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 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 5982</span> Galaxy in the constellation Draco

NGC 5982 is an elliptical galaxy located in the constellation Draco. It is located at a distance of circa 130 million light years from Earth, which, given its apparent dimensions, means that NGC 5982 is about 100,000 light years across. It was discovered by William Herschel on May 25, 1788.

<span class="mw-page-title-main">NGC 7674</span> Galaxy located in the constellation Pegasus

NGC 7674 is a spiral galaxy located in the constellation Pegasus. It is located at a distance of about 350 million light years from Earth, which, given its apparent dimensions, means that NGC 7674 is about 125,000 light years across. It was discovered by John Herschel on August 16, 1830.

<span class="mw-page-title-main">NGC 3489</span> Galaxy in the constellation Leo

NGC 3489 is a lenticular galaxy located in the constellation Leo. It is located at a distance of about 30 million light years from Earth, which, given its apparent dimensions, means that NGC 3489 is about 30,000 light years across. It was discovered by William Herschel on April 8, 1784. NGC 3489 is a member of the Leo Group.

<span class="mw-page-title-main">NGC 5846</span> Galaxy in the constellation Virgo

NGC 5846 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered by William Herschel on February 24, 1786. It lies near 110 Virginis and is part of the Herschel 400 Catalogue. It is a member of the NGC 5846 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">IC 1459</span> Elliptical galaxy in the constellation of Grus

IC 1459 is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light-years across. It was discovered by Edward Emerson Barnard in 1892.

<span class="mw-page-title-main">NGC 4278</span> Galaxy in the constellation Coma Berenices

NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.

<span class="mw-page-title-main">NGC 5363</span> Galaxy in the constellation Virgo

NGC 5363 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of circa 65 million light years from Earth, which, given its apparent dimensions, means that NGC 5363 is about 100,000 light years across. It was discovered by William Herschel on January 19, 1784. It is a member of the NGC 5364 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 765</span> Galaxy in the constellation Aries

NGC 765 is an intermediate spiral galaxy located in the constellation Aries. It is located at a distance of circa 220 million light years from Earth, which, given its apparent dimensions, means that NGC 765 is about 195,000 light years across. It was discovered by Albert Marth on October 8, 1864. The galaxy has an extensive hydrogen (HI) disk with low surface brightness, whose diameter is estimated to be 240 kpc.

<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 931</span> Galaxy in the constellation Triangulum

NGC 931 is a spiral galaxy located in the constellation Triangulum. It is located at a distance of circa 200 million light-years from Earth, which, given its apparent dimensions, means that NGC 931 is about 200,000 light years across. It was discovered by Heinrich d'Arrest on September 26, 1865. It is classified as a Seyfert galaxy.

<span class="mw-page-title-main">NGC 5135</span> Galaxy in the constellation Hydra

NGC 5135 is a barred spiral galaxy located in the constellation Hydra. It is located at a distance of about 200 million light years from Earth. It was discovered by John Herschel on May 8, 1834. It is a Seyfert galaxy.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 2911. Retrieved 2024-03-26.
  2. ↑ "Revised NGC Data for NGC 2911". spider.seds.org. Retrieved 30 March 2024.
  3. ↑ Seligman, Courtney. "NGC 2911 (= PGC 27159 = Arp 232)". Celestial Atlas. Retrieved 19 November 2018.
  4. 1 2 Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  5. ↑ Müller-Sánchez, F.; Prieto, M. A.; Mezcua, M.; Davies, R. I.; Malkan, M. A.; Elitzur, M. (20 January 2013). "The Central Molecular Gas Structure in Liners with Low-Luminosity Active Galactic Nuclei: Evidence for Gradual Disappearance of the Torus". The Astrophysical Journal. 763 (1): L1. arXiv: 1212.1162 . Bibcode:2013ApJ...763L...1M. doi:10.1088/2041-8205/763/1/L1.
  6. ↑ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W. (October 1997). "A Search for Dwarf Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". The Astrophysical Journal Supplement Series. 112 (2): 315–390. arXiv: astro-ph/9704107 . Bibcode:1997ApJS..112..315H. doi:10.1086/313041.
  7. ↑ Walsh, Jonelle L.; Barth, Aaron J.; Ho, Luis C.; Filippenko, Alexei V.; Rix, Hans-Walter; Shields, Joseph C.; Sarzi, Marc; Sargent, Wallace L. W. (1 October 2008). "HUBBLE SPACE TELESCOPE SPECTROSCOPIC OBSERVATIONS OF THE NARROW-LINE REGION IN NEARBY LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI". The Astronomical Journal. 136 (4): 1677–1702. arXiv: 0808.0914 . Bibcode:2008AJ....136.1677W. doi:10.1088/0004-6256/136/4/1677.
  8. ↑ Cheng, X.-P.; An, T. (20 August 2018). "Parsec-scale Radio Structure of 14 Fanaroff–Riley Type 0 Radio Galaxies". The Astrophysical Journal. 863 (2): 155. arXiv: 1807.02505 . Bibcode:2018ApJ...863..155C. doi: 10.3847/1538-4357/aad22c .
  9. ↑ Mezcua, M.; Prieto, M. A. (20 May 2014). "Evidence of Parsec-Scale Jets in Low-Luminosity Active Galactic Nuclei". The Astrophysical Journal. 787 (1): 62. arXiv: 1403.6675 . Bibcode:2014ApJ...787...62M. doi:10.1088/0004-637X/787/1/62.
  10. ↑ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN   0365-0138.
  11. ↑ de Vaucouleurs, G.; de Vaucouleurs, A.; Corwin, J. R. (1 January 1976). "Second reference catalogue of bright galaxies". Second Reference Catalogue of Bright Galaxies. 1976. Bibcode:1976RC2...C......0D.
  12. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi: 10.1111/j.1365-2966.2010.18071.x . S2CID   119194025.
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