NGC 2681

Last updated
NGC 2681
NGC2681 - SDSS DR14.jpg
NGC 2681 by SDSS
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 08h 53m 32.7s [1]
Declination 51° 18′ 49″ [1]
Redshift 692 ± 11 km/s [1]
Distance 51 Mly (15,6 Mpc) [1]
Apparent magnitude  (V)11.1
Characteristics
Type (R')SAB(rs)0/a [1]
Apparent size  (V)3.6′ × 3.3′ [1]
Other designations
UGC 4645, MCG +09-15-041, PGC 24961 [1]

NGC 2681 is a lenticular galaxy in the constellation Ursa Major. The galaxy lies 50 million light years away from Earth, which means, given its apparent dimensions, that NGC 2681 is approximately 55,000 light years across. NGC 2681 has an active galactic nucleus and it is a type 3 Seyfert galaxy. Its nucleus is also a low-ionization nuclear emission-line region. [2]

NGC 2681 has possibly three bars, with a relatively large bar at the outer side. Because the galaxy is seen nearly face-on, the bar like structures cannot be projection effects. [3] From Earth based observations, in B-I images the galaxy showed neither grand design spirals nor a ring, but only two symmetrical spiral arms starting from the end of the primary bar. In Hα images some HII regions were observed in the spiral arms. [4] A dust spiral is seen in Hubble space telescope images extending to the centre. [5] The lack of stellar gradient in the central regions and the data from Faint Object Camera, Faint Object Spectrograph and International Ultraviolet Explorer indicate that the galaxy had a starburst event approximately one billion years ago, possibly after the tidal interaction with another galaxy, which involved all the galaxy. [2]

Dynamical modeling of the velocity dispersions suggests that NGC 2681 hosts a supermassive black hole whose upper mass limit was set at 6×107 M⊙. [2] As observed from Chandra X-ray Observatory, NGC 2681 displayed three stellar sources within the central kiloparsec of the galaxy. The active galactic nucleus had luminosity 1.8 × 1038 erg/s, which accounts for approximately the 20% of the total luminosity of the central kiloparsec. [6]

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">Lenticular galaxy</span> Class of galaxy between an elliptical galaxy and a spiral galaxy

A lenticular galaxy is a type of galaxy intermediate between an elliptical and a spiral galaxy in galaxy morphological classification schemes. It contains a large-scale disc but does not have large-scale spiral arms. Lenticular galaxies are disc galaxies that have used up or lost most of their interstellar matter and therefore have very little ongoing star formation. They may, however, retain significant dust in their disks. As a result, they consist mainly of aging stars. Despite the morphological differences, lenticular and elliptical galaxies share common properties like spectral features and scaling relations. Both can be considered early-type galaxies that are passively evolving, at least in the local part of the Universe. Connecting the E galaxies with the S0 galaxies are the ES galaxies with intermediate-scale discs.

<span class="mw-page-title-main">Messier 61</span> Galaxy in the constellation Virgo

Messier 61 is an intermediate barred spiral galaxy in the Virgo Cluster of galaxies. It was first discovered by Barnaba Oriani on May 5, 1779, six days before Charles Messier discovered the same galaxy. Messier had observed it on the same night as Oriani but had mistaken it for a comet. Its distance has been estimated to be 45.61 million light years from the Milky Way Galaxy. It is a member of the M61 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster.

<span class="mw-page-title-main">Galactic bulge</span> Tightly packed group of stars within a larger formation

In astronomy, a galactic bulge is a tightly packed group of stars within a larger star formation. The term almost exclusively refers to the central group of stars found in most spiral galaxies. Bulges were historically thought to be elliptical galaxies that happened to have a disk of stars around them, but high-resolution images using the Hubble Space Telescope have revealed that many bulges lie at the heart of a spiral galaxy. It is now thought that there are at least two types of bulges: bulges that are like ellipticals and bulges that are like spiral galaxies.

<span class="mw-page-title-main">Sombrero Galaxy</span> Peculiar galaxy in the constellation Virgo

The Sombrero Galaxy (also known as Messier Object 104, M104 or NGC 4594) is a peculiar galaxy of unclear classification in the constellation borders of Virgo and Corvus, being about 9.55 megaparsecs (31.1 million light-years) from the Milky Way galaxy. It is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It has a D25 isophotal diameter of approximately 29.09 kiloparsecs (94,900 light-years), making it slightly bigger in size than the Milky Way.

<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 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 1566</span> Galaxy in the constellation Dorado

NGC 1566, sometimes known as the Spanish Dancer, is an intermediate spiral galaxy in the constellation Dorado, positioned about 3.5° to the south of the star Gamma Doradus. It was discovered on May 28, 1826 by Scottish astronomer James Dunlop. At 10th magnitude, it requires a telescope to view. The distance to this galaxy remains elusive, with measurements ranging from 6 Mpc up to 21 Mpc.

<span class="mw-page-title-main">NGC 3169</span> Galaxy in the constellation Sextans

NGC 3169 is a spiral galaxy about 75 million light years away in the constellation Sextans. It has the morphological classification SA(s)a pec, which indicates this is a pure, unbarred spiral galaxy with tightly-wound arms and peculiar features. There is an asymmetrical spiral arm and an extended halo around the galaxy. It is a member of the NGC 3166 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 5746</span> Spiral galaxy in the constellation Virgo

NGC 5746 is a barred spiral galaxy located in the eastern part of the constellation of Virgo. It is a member of the NGC 5746 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 3642</span> Galaxy in the constellation Ursa Major

NGC 3642 is a spiral galaxy in the constellation Ursa Major. The galaxy has a low-ionization nuclear emission-line region. It is located at a distance of circa 30 million light years from Earth, which, given its apparent dimensions, means that NGC 3642 is about 50,000 light years across. The galaxy is characterised by an outer pseudoring, which was probably formed after the accretion of a gas rich dwarf 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 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 5965</span> Spiral galaxy in the constellation Draco

NGC 5965 is a spiral galaxy located in the constellation Draco. It is located at a distance of circa 150 million light years from Earth, which, given its apparent dimensions, means that NGC 5965 is about 260,000 light years across. It was discovered by William Herschel on May 5, 1788.

<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 973</span> Galaxy in the constellation Triangulum

NGC 973 is a giant 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 973 is about 230,000 light years across. It was discovered by Lewis Swift on October 30, 1885.

<span class="mw-page-title-main">NGC 4800</span> Galaxy in constellation Canes Venatici

NGC 4800 is an isolated spiral galaxy in the constellation Canes Venatici, located at a distance of 95 megalight-years from the Milky Way. It was discovered by William Herschel on April 1, 1788. The morphological classification of this galaxy is SA(rs)b, indicating a spiral galaxy with no visual bar at the nucleus (SA), an incomplete ring structure (rs), and moderately-tightly wound spiral arms (b). The galactic plane is inclined to the line of sight by an angle of 43°, and the long axis is oriented along a position angle of 25°. There is a weak bar structure at the nucleus that is visible in the infrared.

<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 7 "NASA/IPAC Extragalactic Database". Results for NGC 2681. Retrieved 2016-01-18.
  2. 1 2 3 Cappellari, Michele; Bertola, Francesco; Burstein, David; Buson, Lucio M.; Greggio, Laura; Renzini, Alvio (10 April 2001). "The Cuspy Liner Nucleus of the S0/a Galaxy NGC 2681". The Astrophysical Journal. 551 (1): 197–205. arXiv: astro-ph/0012425 . Bibcode:2001ApJ...551..197C. doi:10.1086/320054. S2CID   119357835.
  3. ↑ Erwin, Peter; Sparke, Linda S. (10 August 1999). "Triple Bars and Complex Central Structures in Disk Galaxies". The Astrophysical Journal. 521 (1): L37–L40. arXiv: astro-ph/9906262 . Bibcode:1999ApJ...521L..37E. doi:10.1086/312169. S2CID   14042533.
  4. ↑ Wozniak, H.; Friedli, D.; Martinet, L.; Martin, P.; Bratschi, P. (1 May 1995). "Disc galaxies with multiple triaxial structures. I. BVRI and Halpha surface photometry" (PDF). Astronomy and Astrophysics Supplement Series. 111: 115. Bibcode:1995A&AS..111..115W. ISSN   0365-0138.
  5. ↑ Fabricius, Maximilian H.; Saglia, Roberto P.; Fisher, David B.; Drory, Niv; Bender, Ralf; Hopp, Ulrich (1 January 2012). "Kinematic Signatures of Bulges Correlate with Bulge Morphologies and Sérsic Index". The Astrophysical Journal. 754 (1): 67. arXiv: 1204.5188 . Bibcode:2012ApJ...754...67F. doi:10.1088/0004-637X/754/1/67. ISSN   0004-637X. S2CID   118654082.
  6. ↑ Flohic, Helene M. L. G.; Eracleous, Michael; Chartas, George; Shields, Joseph C.; Moran, Edward C. (10 August 2006). "The Central Engines of 19 LINERs as Viewed by". The Astrophysical Journal. 647 (1): 140–160. arXiv: astro-ph/0604487 . Bibcode:2006ApJ...647..140F. doi:10.1086/505296. S2CID   15112150.


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.