NGC 4710

Last updated • 2 min readFrom Wikipedia, The Free Encyclopedia
NGC 4710
NGC 4710 (captured by the Hubble Space Telescope).jpg
Hubble Space Telescope image of NGC 4710
Observation data (J2000 epoch)
Constellation Coma Berenices
Right ascension 12h 49m 38.958s [1]
Declination +15° 09′ 55.76″ [1]
Redshift 0.00397±0.00011 [2]
Heliocentric radial velocity 1,129 km/s [3]
Distance 54.5 ± 3.6  Mly (16.7 ± 1.1  Mpc) [4]
Apparent magnitude  (V)11.9 [5]
Apparent magnitude  (B)11.60 [3]
Characteristics
Type S0a-S0/Sa [3]
Apparent size  (V)3.0′ × 0.8′ [3]
Other designations
NGC 4710, UGC 7980, PGC 43375 [6] [5]

NGC 4710 is an edge-on lenticular galaxy in the northern constellation of Coma Berenices. It was discovered on March 21, 1784 by German-British astronomer William Herschel. [7] This galaxy has a B-band visual magnitude of 11.60 and an angular size of 3.0′ × 0.8′. [3] It is located at a distance of 54.5 ± 3.6 million light-years (16.7 ± 1.1  Mpc ) from the Milky Way, [4] and is receding with a heliocentric radial velocity of 1,129 km/s. [3] This is a member of the Virgo Cluster, with a projected offset of ~6° from the cluster center and a cluster crossing time of around two billion years. [8]

Contents

The morphological classification of NGC 4710 is S0 or SA(r)0, [9] which indicates this is an unbarred lenticular galaxy [8] (SA) with an inner ring structure (r). It is inclined at an angle of 86° to the plane of the sky, with the major axis aligned along a position angle of 207°. [10] NGC 4710 has a relatively high gas abundance with a dusty nucleus. The stellar velocity distribution is characteristic of galaxies with a small bulge. Like the Milky Way, it has an X-shaped bulge which is a probable bar structure; hence it is likely a barred lenticular. [9] [11] The star formation rate is 0.11±0.02  M☉ ·yr−1. [10] NGC 4710 possesses both thin and thick discs. [12]

Further reading

Related Research Articles

<span class="mw-page-title-main">Elliptical galaxy</span> Spherical or ovoid mass of stars

An elliptical galaxy is a type of galaxy with an approximately ellipsoidal shape and a smooth, nearly featureless image. They are one of the four main classes of galaxy described by Edwin Hubble in his Hubble sequence and 1936 work The Realm of the Nebulae, along with spiral and lenticular galaxies. Elliptical (E) galaxies are, together with lenticular galaxies (S0) with their large-scale disks, and ES galaxies with their intermediate scale disks, a subset of the "early-type" galaxy population.

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

The Virgo Cluster is a large cluster of galaxies whose center is 53.8 ± 0.3 Mly away in the constellation Virgo. Comprising approximately 1,300 member galaxies, the cluster forms the heart of the larger Virgo Supercluster, of which the Local Group is a member. The Local Group actually experiences the mass of the Virgo Supercluster as the Virgocentric flow. It is estimated that the Virgo Cluster's mass is 1.2×1015M☉ out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.

<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">Sombrero Galaxy</span> Galaxy in the constellation Virgo

The Sombrero Galaxy is a peculiar galaxy of unclear classification in the constellation borders of Virgo and Corvus, being about 9.55 megaparsecs 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 an isophotal diameter of approximately 29.09 to 32.32 kiloparsecs, making it slightly bigger in size than the Milky Way.

<span class="mw-page-title-main">NGC 404</span> Galaxy in the constellation Andromeda

NGC 404 is a field galaxy located about 10 million light years away in the constellation Andromeda. It was discovered by William Herschel in 1784, and is visible through small telescopes. NGC 404 lies just beyond the Local Group and does not appear gravitationally bound to it. It is located within 7 arc-minutes of second magnitude star Mirach, making it a difficult target to observe or photograph and granting it the nickname "Mirach's Ghost".

<span class="mw-page-title-main">NGC 5866</span> Galaxy in the constellation Draco

NGC 5866 is a lenticular galaxy in the constellation Draco. NGC 5866 was most likely discovered by Pierre Méchain or Charles Messier in 1781, and independently found by William Herschel in 1788. Measured orbital velocities of its globular cluster system imply that dark matter makes up only 34%±45% of the mass within 5 effective radii, a notable paucity.

<span class="mw-page-title-main">Dwarf galaxy</span> Small galaxy composed of up to several billion stars

A dwarf galaxy is a small galaxy composed of about 1000 up to several billion stars, as compared to the Milky Way's 200–400 billion stars. The Large Magellanic Cloud, which closely orbits the Milky Way and contains over 30 billion stars, is sometimes classified as a dwarf galaxy; others consider it a full-fledged galaxy. Dwarf galaxies' formation and activity are thought to be heavily influenced by interactions with larger galaxies. Astronomers identify numerous types of dwarf galaxies, based on their shape and composition.

<span class="mw-page-title-main">Messier 86</span> Elliptical galaxy in the constellation Virgo

Messier 86 is an elliptical or lenticular galaxy in the constellation Virgo. It was discovered by Charles Messier in 1781. M86 lies in the heart of the Virgo Cluster of galaxies and forms a most conspicuous group with another large galaxy known as Messier 84. It displays the highest blue shift of all Messier objects, as it is, net of its other vectors of travel, approaching the Milky Way at 244 km/s. This is due to both galaxies falling roughly towards the center of the Virgo cluster from opposing ends.

<span class="mw-page-title-main">NGC 3115</span> Galaxy in the constellation Sextans

NGC 3115 is a field lenticular (S0) galaxy in the constellation Sextans. The galaxy was discovered by William Herschel on February 22, 1787. At about 32 million light-years away from Earth, it is several times bigger than the Milky Way. It is a lenticular (S0) galaxy because it contains a disk and a central bulge of stars, but without a detectable spiral pattern. NGC 3115 is seen almost exactly edge-on, but was nevertheless mis-classified as elliptical. There is some speculation that NGC 3115, in its youth, was a quasar.

<span class="mw-page-title-main">NGC 4526</span> Lenticular galaxy in the constellation Virgo

NGC 4526 is a lenticular galaxy with an embedded dusty disc, located approximately 55 million light-years from the Solar System in the Virgo constellation and discovered on 13 April 1784 by William Herschel.

<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.

<span class="mw-page-title-main">NGC 3607</span> Galaxy in the constellation Leo

NGC 3607 is a small but fairly bright lenticular galaxy in the equatorial constellation of Leo, about 2.5° south of the prominent star Delta Leonis. The galaxy was discovered March 14, 1784 by William Herschel. Dreyer described it as "very bright, large, round, very much brighter middle, 2nd of 3". It is located at a distance of 73 million light years and is receding with a radial velocity of 930 km/s. The galaxy lies southwest of NGC 3626 at an angular separation of ~50′. It occupies the center of the Leo II Group of galaxies, forming one of its two brightest members – the other being NGC 3608. It is a member of the NGC 3607 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 4550</span> Galaxy in the constellation Virgo

NGC 4550 is a barred lenticular galaxy located in the constellation of Virgo that can be seen with amateur telescopes. It lies at a distance of 50 million light-years from the Milky Way and is a member of the Virgo Cluster.

<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 4111</span> Galaxy in constellation Canes Venatici

NGC 4111 is a lenticular galaxy in the constellation Canes Venatici. It is located at a distance of circa 50 million light-years from Earth, which, given its apparent dimensions, means that NGC 4111 is about 55,000 light-years across. It was discovered by William Herschel in 1788. NGC 4111 possesses both thin and thick discs.

<span class="mw-page-title-main">NGC 1380</span> Galaxy in the constellation Fornax

NGC 1380 is a lenticular galaxy located in the constellation Fornax. It is located at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 1380 is about 85,000 light years across. It was discovered by James Dunlop on September 2, 1826. It is a member of the Fornax Cluster.

<span class="mw-page-title-main">NGC 4298</span> Galaxy in the constellation Coma Berenices

NGC 4298 is a flocculent spiral galaxy located about 53 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4299</span> Spiral galaxy in the constellation Virgo

NGC 4299 is a featureless spiral galaxy located about 55 million light-years away in the constellation Virgo. It was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4324</span> Galaxy in the constellation of Virgo

NGC 4324 is a lenticular galaxy located about 85 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on March 4, 1862. NGC 4324 has a stellar mass of 5.62 × 1010M☉, and a baryonic mass of 5.88 × 1010M☉. The galaxy's total mass is around 5.25 × 1011M☉. NGC 4324 is notable for having a ring of star formation surrounding its nucleus. It was considered a member of the Virgo II Groups until 1999, when its distance was recalculated and it was placed in the Virgo W Group.

References

  1. 1 2 Skrutskie, Michael F.; et al. (February 1, 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi: 10.1086/498708 . ISSN   0004-6256. S2CID   18913331.
  2. ↑ Abazajian, Kevork N.; et al. (2009). "The Seventh Data Release of the Sloan Digital Sky Survey". The Astrophysical Journal Supplement Series. 182 (2): 543–558. arXiv: 0812.0649 . Bibcode:2009ApJS..182..543A. doi:10.1088/0067-0049/182/2/543. S2CID   14376651.
  3. 1 2 3 4 5 6 Boselli, A.; et al. (2014). "The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). IV. The role of the cluster environment on galaxy evolution". Astronomy & Astrophysics. 570: A69. arXiv: 1407.4986 . Bibcode:2014A&A...570A..69B. doi:10.1051/0004-6361/201424419. S2CID   119244700. A69.
  4. 1 2 Haynes, Martha P.; et al. (July 2018). "The Arecibo Legacy Fast ALFA Survey: The ALFALFA Extragalactic H I Source Catalog". The Astrophysical Journal. 861 (1): 49. arXiv: 1805.11499 . Bibcode:2018ApJ...861...49H. doi: 10.3847/1538-4357/aac956 . 49.
  5. 1 2 "NASA/IPAC Extragalactic Database". Results for NGC 4710. Retrieved 2007-04-02.
  6. ↑ "NGC 4710". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-09-22.
  7. ↑ Seligman, Courtney. "NGC Objects: NGC 4700 - 4749". Celestial Atlas. Retrieved 2024-04-10.
  8. 1 2 Wrobel, J. M.; Kenney, Jeffrey D. P. (November 1992). "Nuclear Molecular Gas in the Virgo Cluster S0 Galaxy NGC 4710". Astrophysical Journal. 399: 94. Bibcode:1992ApJ...399...94W. doi:10.1086/171905.
  9. 1 2 Gonzalez, O. A.; et al. (June 2016). "Comparing the properties of the X-shaped bulges of NGC 4710 and the Milky Way with MUSE". Astronomy & Astrophysics. 591. id. A7. arXiv: 1603.02546 . Bibcode:2016A&A...591A...7G. doi:10.1051/0004-6361/201527806.
  10. 1 2 Topal, Selçuk; et al. (December 2016). "Molecular gas kinematics and line diagnostics in early-type galaxies: NGC 4710 and NGC 5866". Monthly Notices of the Royal Astronomical Society. 463 (4): 4121–4152. arXiv: 1609.01506 . Bibcode:2016MNRAS.463.4121T. doi: 10.1093/mnras/stw2257 .{{cite journal}}: |last2= has generic name (help)
  11. ↑ Bogdan, C. Ciambur; Graham, Alister W. (June 2016). "Quantifying the (X/peanut)-shaped structure in edge-on disc galaxies: length, strength, and nested peanuts". Monthly Notices of the Royal Astronomical Society. 459 (2): 1276–1292. arXiv: 1603.00019 . Bibcode:2016MNRAS.459.1276C. doi: 10.1093/mnras/stw759 . S2CID   118991786.
  12. ↑ Kasparova, A. (2016). "The Diversity of Thick Galactic Discs". Monthly Notices of the Royal Astronomical Society: Letters . 460 (1): 89–93. arXiv: 1604.07624 . Bibcode:2016MNRAS.460L..89K. doi: 10.1093/mnrasl/slw083 . S2CID   119303521.
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.