NGC 4526

Last updated
NGC 4526
SN1994D.jpg
Supernova SN 1994D (lower left) in the outskirts of NGC 4526's central disk
Observation data (J2000 epoch)
Constellation Virgo
Right ascension 12h 34m 03.029s [1]
Declination +07° 41′ 56.90″ [1]
Redshift 0.001494±0.000027
Heliocentric radial velocity 448±8 km/s [2]
Distance 55±5  Mly  (16.9±1.6  Mpc ) [3]
52  Mly (15.8  Mpc) [4]
Apparent magnitude  (V)10.7 [2]
Characteristics
Type SAB(s)0° [5]
Apparent size  (V)7′.2 × 2′.4 [2]
Other designations
IRAS 12315+0758, NGC 4560, UGC 7718, MCG +01-32-100, PGC 41772, CGCG 042-155 [2]

NGC 4526 (also listed as NGC 4560) is a lenticular galaxy with an embedded dusty disc, located approximately 55 million light-years from the Solar System [3] in the Virgo constellation and discovered on 13 April 1784 by William Herschel. [6] Herschel observed it again on 28 December 1785, resulting in the galaxy being entered twice into the New General Catalogue. [6]

Contents

The galaxy is seen nearly edge-on. The morphological classification is SAB(s)0°, [5] which indicates a lenticular structure with a weak bar across the center and pure spiral arms without a ring. [7] It belongs to the Virgo cluster and is one of the brightest known lenticular galaxies. [5] In the galaxy's outer halo, globular cluster orbital velocities [8] indicate abnormal poverty of dark matter: only 43±18% of the mass within 5 effective radii.

The inner nucleus of this galaxy displays a rise in stellar orbital motion that indicates the presence of a central dark mass. The best fit model for the motion of molecular gas in the core region suggests there is a supermassive black hole with about 4.5+4.2
−3.0×108 (450 million) times the mass of the Sun. [9] This is the first object to have its black-hole mass estimated by measuring the rotation of gas molecules around its centre with an astronomical interferometer (in this case the Combined Array for Research in Millimeter-wave Astronomy).

Supernova SN 1969E was discovered in this galaxy in 1969, reaching a peak magnitude of 16. [10] In 1994, a type Ia supernova was discovered about two weeks before reaching peak brightness. Designated SN 1994D, it was caused by the explosion of a white dwarf star composed of carbon and oxygen. [11]

Wider Hubble Space Telescope image showing the envelope of more distant orbiting stars The whirling disc of NGC 4526.jpg
Wider Hubble Space Telescope image showing the envelope of more distant orbiting stars

See also

Related Research Articles

<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">Centaurus A</span> Radio galaxy in the constellation Centaurus

Centaurus A is a galaxy in the constellation of Centaurus. It was discovered in 1826 by Scottish astronomer James Dunlop from his home in Parramatta, in New South Wales, Australia. There is considerable debate in the literature regarding the galaxy's fundamental properties such as its Hubble type and distance. It is the closest radio galaxy to Earth, as well as the closest BL Lac object, so its active galactic nucleus has been extensively studied by professional astronomers. The galaxy is also the fifth-brightest in the sky, making it an ideal amateur astronomy target. It is only visible from the southern hemisphere and low northern latitudes.

<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">Messier 59</span> Elliptical galaxy in the constellation Virgo

Messier 59 or M59, also known as NGC 4621, is an elliptical galaxy in the equatorial constellation of Virgo. It is a member of the Virgo Cluster, with the nearest fellow member 8′ away and around 5 magnitudes fainter. The nearest cluster member of comparable brightness is the lenticular galaxy NGC 4638, which is around 17′ away. It and the angularly nearby elliptical galaxy Messier 60 were both discovered by Johann Gottfried Koehler in April 1779 when observing comet seeming close by. Charles Messier listed both in the Messier Catalogue about three days after Koehler's discovery.

<span class="mw-page-title-main">Messier 60</span> Elliptical galaxy in the constellation Virgo

Messier 60 or M60, also known as NGC 4649, is an elliptical galaxy approximately 57 million light-years away in the equatorial constellation of Virgo. Together with NGC 4647, it forms a pair known as Arp 116. Messier 60 and nearby elliptical galaxy Messier 59 were discovered by Johann Gottfried Koehler in April 1779, observing a comet in the same part of the sky. Charles Messier added both to his catalogue about three days after this.

<span class="mw-page-title-main">Messier 84</span> Galaxy in the constellation Virgo

Messier 84 or M84, also known as NGC 4374, is a giant elliptical or lenticular galaxy in the constellation Virgo. Charles Messier discovered the object in 1781 in a systematic search for "nebulous objects" in the night sky. It is the 84th object in the Messier Catalogue and in the heavily populated core of the Virgo Cluster of galaxies, part of the local supercluster.

<span class="mw-page-title-main">Messier 85</span> Elliptical galaxy in the constellation Coma Berenices

Messier 85 is a lenticular galaxy, or elliptical galaxy for other authors, in the Coma Berenices constellation. It is 60 million light-years away, and has a diameter of about 36.99 kiloparsecs across.

<span class="mw-page-title-main">Messier 89</span> Elliptical galaxy in the constellation Virgo

Messier 89 is an elliptical galaxy in the constellation Virgo. It was discovered by Charles Messier on March 18, 1781. M89 is a member of the Virgo Cluster of galaxies.

<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 5195</span> Dwarf galaxy in the constellation Canes Venatici

NGC 5195 is a dwarf galaxy that is interacting with the Whirlpool Galaxy. Both galaxies are located approximately 25 million light-years away in the constellation Canes Venatici. Together, the two galaxies are one of the most famous interacting galaxy pairs.

<span class="mw-page-title-main">NGC 1316</span> Lenticular radio galaxy in the constellation Fornax

NGC 1316 is a lenticular galaxy about 60 million light-years away in the constellation Fornax. It is a radio galaxy and at 1400 MHz is the fourth-brightest radio source in the sky.

<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">SN 1994D</span> Type Ia supernova

SN 1994D was a Type Ia supernova event in the outskirts of galaxy NGC 4526. It was offset by 9.0″ west and 7.8″ south of the galaxy center and positioned near a prominent dust lane. It was caused by the explosion of a white dwarf star composed of carbon and oxygen. This event was discovered on March 7, 1994 by R. R. Treffers and associates using the automated 30-inch telescope at Leuschner Observatory. It reached peak visual brightness two weeks later on March 22. Modelling of the light curve indicates the explosion would have been visible around March 3-4. A possible detection of helium in the spectrum was made by W. P. S. Meikle and associates in 1996. A mass of 0.014 to 0.03 M☉ in helium would be needed to produce this feature.

<span class="mw-page-title-main">NGC 4710</span> Galaxy in the constellation Coma Berenices

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. This galaxy has a B-band visual magnitude of 11.60 and an angular size of 3.0′ × 0.8′. It is located at a distance of 54.5 ± 3.6 million light-years (16.7 ± 1.1 Mpc) from the Milky Way, and is receding with a heliocentric radial velocity of 1,129 km/s. 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.

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

The Dorado Group is a loose concentration of galaxies containing both spirals and ellipticals. It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'. It lies primarily in the southern constellation Dorado and is one of the richest galaxy groups of the Southern Hemisphere. Gérard de Vaucouleurs was the first to identify it in 1975 as a large complex nebulae II in the Dorado region, designating it as G16.

<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 4036</span> Galaxy in the constellation Ursa Major

NGC 4036 is the New General Catalogue identifier for a lenticular galaxy in the northern circumpolar constellation of Ursa Major. In the Carnegie Atlas of Galaxies, it is described as being "characterized by an irregular pattern of dust lanes threaded through the disc in an 'embryonic' spiral pattern indicating a mixed S0/Sa form." It is located near the Big Dipper, a little to the north of the mid-way point between the stars Alpha Ursae Majoris and Delta Ursae Majoris. With a visual magnitude of 10.7, it can be dimly viewed using a 4 in (10 cm) aperture telescope.

<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 4203</span> Galaxy in the constellation Coma Berenices

NGC 4203 is the New General Catalogue identifier for a lenticular galaxy in the northern constellation of Coma Berenices. It was discovered on March 20, 1787 by English astronomer William Herschel, and is situated 5.5° to the northwest of the 4th magnitude star Gamma Comae Berenices and can be viewed with a small telescope. The morphological classification of NGC 4203 is SAB0−, indicating that it has a lenticular form with tightly wound spiral arms and a weak bar structure at the nucleus.

<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.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W.; Chester, Thomas; Elias, Jonathan H.; Huchra, John P.; Liebert, James W.; Lonsdale, Carol J.; Monet, David G.; Price, Stephan; Seitzer, Patrick; Jarrett, Thomas H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Elizabeth V.; Evans, Tracey E.; Fowler, John W.; Fullmer, Linda; Hurt, Robert L.; Light, Robert M.; Kopan, Eugene L.; Marsh, Kenneth A.; McCallon, Howard L.; Tam, Robert; Van Dyk, Schuyler D.; Wheelock, Sherry L. (1 February 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. 1 2 3 4 "NASA/IPAC Extragalactic Database", Results for NGC 4526, retrieved 2006-10-18.
  3. 1 2 Tonry, J. L.; et al. (2001), "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances", Astrophysical Journal, 546 (2): 681–693, arXiv: astro-ph/0011223 , Bibcode:2001ApJ...546..681T, doi:10.1086/318301, S2CID   17628238.
  4. ↑ Hatt, Dylan; et al. (July 2018). "The Carnegie-Chicago Hubble Program. IV. The Distance to NGC 4424, NGC 4526, and NGC 4356 via the Tip of the Red Giant Branch". The Astrophysical Journal. 861 (2): 10. arXiv: 1806.02900 . Bibcode:2018ApJ...861..104H. doi: 10.3847/1538-4357/aac9cc . S2CID   119430198. 104.
  5. 1 2 3 Burstein, D. (November 1979), "Structure and origin of S0 galaxies. I - Surface photometry of S0 galaxies", Astrophysical Journal Supplement Series, 41: 435–450, Bibcode:1979ApJS...41..435B, doi: 10.1086/190625 .
  6. 1 2 Courtney Seligman. "New General Catalog Objects: NGC 4500 - 4549" . Retrieved October 17, 2021.
  7. ↑ Buta, Ronald J.; et al. (2007), Atlas of Galaxies, Cambridge University Press, pp. 13–17, ISBN   978-0521820486.
  8. ↑ Adebusola B. Alabi; Duncan A. Forbes; Aaron J. Romanowsky; Jean P. Brodie; Jay Strader; Joachim Janz; Christopher Usher; Lee R. Spitler; Sabine Bellstedt; Anna Ferre-Mateu (2016-05-20). "The SLUGGS survey: the mass distribution in early-type galaxies within five effective radii and beyond". Monthly Notices of the Royal Astronomical Society. 460 (4): 3838–3860. arXiv: 1605.06101 . Bibcode:2016MNRAS.460.3838A. doi: 10.1093/mnras/stw1213 . S2CID   55054073.
  9. ↑ Davis, Timothy A.; et al. (February 2013), "A black-hole mass measurement from molecular gas kinematics in NGC4526", Nature, 494 (7437): 328–330, arXiv: 1301.7184 , Bibcode:2013Natur.494..328D, doi:10.1038/nature11819, PMID   23364690, S2CID   205232307.
  10. ↑ Kowal, C. T.; Sargent, W. L. W. (November 1971), "Supernovae discovered since 1885", Astronomical Journal, 41: 756–764, Bibcode:1971AJ.....76..756K, doi: 10.1086/111193 .
  11. ↑ Lentz, Eric J.; et al. (August 2001), "Non-LTE Synthetic Spectral Fits to the Type Ia Supernova 1994D in NGC 4526", The Astrophysical Journal, 557 (1): 756–764, arXiv: astro-ph/0104225 , Bibcode:2001ApJ...557..266L, doi:10.1086/322239, S2CID   119535927.
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.