NGC 4036

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NGC 4036
Hazy dust in Ursa Major NGC 4036.jpg
Image of NGC 4036 taken by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 12h 01m 26.891s [1]
Declination +61° 53′ 44.52″ [1]
Redshift 0.004817 [2]
Heliocentric radial velocity 1,445 [2] km/s
Distance 62.1  Mly (19.04  Mpc) [3]
Group or cluster LGG 266 [4]
Absolute magnitude  (V)10.66 [4]
Characteristics
Type S0− [3]
Apparent size  (V)2.703′ × 1.027′ [1]
Other designations
2MASX J12012689+6153445, IRAS 11588+6210, LEDA 37930, UGC 7005, UZC J120126.7+615345, Z 292-59 [5]

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." [4] 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. [6]

Contents

The visual dimensions of this galaxy are 2.703 × 1.027 [1] arc minutes, with the major axis having a position angle of 85°. [4] The galaxy is being viewed nearly edge-on, with an inclination of 18° to the line of sight from the Earth. [7] It is moving away from us with a heliocentric radial velocity of 1,445 [2] km/s. The estimated visual luminosity of the galaxy is 4.2×1010  L⊙, or 42 billion times the brightness of the Sun. Photographs show a tightly wound spiral pattern in the galactic disk, with three dust lanes—the southern side of the galaxy appears dimmer due to the dust configuration. [7] The mass of the free gas and dust in the galaxy is about 1.7×109  M⊙ and 4.4×105 M⊙, respectively, with around 7×104 M⊙ of the gas being in an ionized state. [4]

This is a type of active galaxy known as a LINER, which means that it shows emission lines of ionized gas in the region of its nucleus. Chemically, the stars at the center of the nucleus have a higher metallicity than in the neighboring regions. It appears that there is a tilted disk of stars orbiting the nucleus within a radius of 820 ly (250 pc). The galactic bulge itself appears triaxial with the ionized gas concentrated near the center of this bulge region. [8] Images of the galaxy with the Hubble Space Telescope show a wispy disk of dust on all sides of the nucleus, with what appears to be the tendrilous remains of an ionization cone leading away 4 arc seconds to the northeast. Such features are common in Seyfert galaxies. [7]

On July 23, 2007, Type Ia supernova SN 2007gi was discovered by Koichi Itagaki near the central bulge of this galaxy. [9] It reached peak magnitude around August 14, then steadily declined in brightness thereafter. Materials identified in the spectrum included silicon, calcium, and sulfur moving outward at velocities of around 15,500 km/s. This is a 50% higher velocity than what is normally observed with supernovae of this type. [10]

NGC 4036 is a member of the LGG 266 galaxy group, along with NGC 4041, IC 758, UGC 7009, and UGC 7019. It is located just 17 arc minutes from NGC 4041, and the two form a pair with a projected separation of around 470 kly (143 kpc). [4]

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">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 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 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 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">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">NGC 1553</span> Galaxy in the constellation Dorado

NGC 1553 is a prototypical lenticular galaxy in the constellation Dorado. It is the second brightest member of the Dorado Group of galaxies. British astronomer John Herschel discovered NGC 1553 on December 5, 1834 using an 18.7 inch reflector.

<span class="mw-page-title-main">NGC 2775</span> Galaxy in the constellation Cancer

NGC 2775, also known as Caldwell 48, is a spiral galaxy in the constellation Cancer. It is 67 million light-years away from the Milky Way. It was discovered by William Herschel in 1783. NGC 2775 belongs to the Antlia-Hydra Cluster of galaxies and is the most prominent member of the NGC 2775 Group, a small galaxy group in the Virgo Super-cluster, along with the Local Group. Other members of the NGC 2775 Group include NGC 2777 and UGC 4781.

<span class="mw-page-title-main">NGC 613</span> Galaxy in the constellation of Sculptor

NGC 613 is a barred spiral galaxy located 67 million light years away in the southern constellation of Sculptor. This galaxy was discovered in 1798 by German-English astronomer William Herschel, then re-discovered and catalogued by Scottish astronomer James Dunlop. It was first photographed in 1912, which revealed the spiral form of the nebula. During the twentieth century, radio telescope observations showed that a linear feature in the nucleus was a relatively strong source of radio emission.

<span class="mw-page-title-main">NGC 4041</span> Spiral galaxy in the constellation Ursa Major

NGC 4041 is the New General Catalogue identifier for a spiral galaxy in the northern circumpolar constellation of Ursa Major. It is located an estimated 70 million light years from the Sun. The morphological classification of SA(rs)bc indicates this is a spiral galaxy the lacks a bar; the 'rs' means it has a weakly-formed ring structure, and the 'bc' indicates the spiral arms are moderately to loosely wound.

<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 4178</span> Galaxy in the constellation Virgo

NGC 4178 is the New General Catalogue identifier for a barred spiral galaxy in the equatorial constellation of Virgo. It was discovered April 11, 1825 by English astronomer John Herschel. Located some 43.8 million light years away, this galaxy spans 2.3 × 0.4 arc minutes and is seen at a low angle, being inclined by 77° to the line of sight from the Earth. The morphological classification of NGC 4178 is SB(rs)dm, indicating that it has a bar feature at the core, and, per the '(rs)', has traces of a ring-like structure surrounding the bar. The 'dm' suffix indicates the spiral arms are diffuse, broken, and irregular in appearance with no bulge at the nucleus. This galaxy is a member of the Virgo Cluster, which is the richest nearby group of galaxies outside the Local Group and forms the core of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 5643</span> Galaxy in the constellation Lupus

NGC 5643 is an intermediate spiral galaxy in the constellation Lupus. Based on the tip of the red-giant branch distance indicator, it is located at a distance of about 40 million light-years. NGC 5643 has an active galactic nucleus and is a type II Seyfert galaxy.

<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 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 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 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 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 5728</span> Spiral galaxy in the constellation Libra

NGC 5728 is an active barred spiral galaxy located 146 million light years away in the southern constellation of Libra. It was discovered on May 7, 1787 by William Herschel. The designation comes from the New General Catalogue of J. L. E. Dreyer, published in 1888. It has an apparent visual magnitude of 13.40 and spans an angle of 3.4 arcminutes. The galaxy shows a red shift of 0.00935 and has a heliocentric radial velocity of 2,803 km/s. It has an estimated mass of 72 billion times the mass of the Sun and stretches around 30 kpc across.

<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 3 4 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 Kochanek, C. S.; et al. (October 2001), "The K-Band Galaxy Luminosity Function", The Astrophysical Journal, 560 (2): 566–579, arXiv: astro-ph/0011456 , Bibcode:2001ApJ...560..566K, doi:10.1086/322488, S2CID   119420446.
  3. 1 2 de Vaucouleurs G.; et al. (1994), "Third Reference Catalogue of Bright Galaxies (RC3)", The Astronomical Journal, 108: 2128, Bibcode:1994AJ....108.2128C, doi:10.1086/117225, archived from the original on 2006-09-30, retrieved 2015-11-16.{{citation}}: CS1 maint: numeric names: authors list (link)
  4. 1 2 3 4 5 6 Cinzano, P.; et al. (August 1999), "The kinematics and the origin of the ionized gas in NGC 4036", Monthly Notices of the Royal Astronomical Society, 307 (2): 433–448, arXiv: astro-ph/9903216 , Bibcode:1999MNRAS.307..433C, doi: 10.1046/j.1365-8711.1999.02617.x , S2CID   119466666.
  5. ↑ "NGC 4036". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2015-11-16.
  6. ↑ O'Meara, Steve (2007), Herschel 400 Observing Guide, Cambridge University Press, p. 102, ISBN   978-0521858939.
  7. 1 2 3 O'Meara, Stephen James (2011), Deep-Sky Companions: The Secret Deep, vol. 4, Cambridge University Press, pp. 214–215, ISBN   978-1139500074.
  8. ↑ Sil'chenko, O. K.; Vlasyuk, V. V. (January 2001), "A Chemically Decoupled Nucleus and Structure of the Nuclear Region in the S0 Galaxy NGC4036", Astronomy Letters, 27: 15–24, Bibcode:2001AstL...27...15S, doi:10.1134/1.1336857, S2CID   54607256.
  9. ↑ Harutyunyan, A.; et al. (August 2007), Green, D. W. E. (ed.), "Supernova 2007gi in NGC 4036", Central Bureau Electronic Telegrams, 1021: 1, Bibcode:2007CBET.1021....1H.
  10. ↑ Zhang, T.; et al. (January 2010), "Optical Observations of the Rapidly Expanding Type Ia Supernova 2007gi", Publications of the Astronomical Society of the Pacific, 122 (887): 1–11, arXiv: 0910.1913 , Bibcode:2010PASP..122....1Z, doi:10.1086/649851, S2CID   118517321.


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