NGC 1313

Last updated
NGC 1313
Phot-43a-06.jpg
A Very Large Telescope (VLT) image of NGC 1313.
Credit: ESO.
Observation data (J2000.0 epoch)
Constellation Reticulum
Right ascension 03h 18m 15.4s [1]
Declination −66° 29′ 50″ [1]
Redshift 0.001568 [1]
Distance 12.886 Mly [1]
Characteristics
Type SB(s)d [1]
Apparent size  (V)9.1 x 7.1 arcmin [1]
Other designations
Topsy Turvy Galaxy, PGC 12286, ESO 082- G 011

NGC 1313 (also known as the Topsy Turvy Galaxy [2] ) is a field galaxy [3] and an irregular galaxy [4] discovered by the Scottish astronomer James Dunlop on 27 September 1826. [5] It has a diameter of about 50,000 light-years, or about half the size of the Milky Way. [6]

Contents

NGC 1313 lies within the Virgo Supercluster. [7]

In 2007, a rare WO star was discovered in NGC 1313, [8] currently known by its only designation of [HC2007] 31. It is of spectral type WO3. [8] The derived absolute magnitude is about -5, [8] which is very high for a single WO star. (WOs usually have absolute magnitudes of about -1 to -4) This means that the WO is likely part of a binary or a small stellar association. [8]

Supernovae

Two supernovae have been observed in NGC 2841:

Features

NGC 1313 has a strikingly uneven shape and its axis of rotation is not exactly in its centre. [13] NGC 1313 also shows strong starburst activity [14] and associated supershells. [15] NGC 1313 is dominated by scattered patches of intense star formation, which gives the galaxy a rather ragged appearance. [16] The uneven shape, the ragged appearance and the strong starburst can all be explained by a galactic collision in the past. [17] However, NGC 1313 seems to be an isolated galaxy and has no direct neighbours. Therefore, it is not clear whether it has swallowed a small companion in its past. [2]

Young, blue stars are scattered across the galaxy. [18] This is evidence of infant mortality in which the young open clusters quickly became gravitationally "unglued", scattering their resident stars into the galaxy. [19] The galaxy bears some resemblance to the Magellanic Clouds [20] and hosts two ultraluminous X-ray sources, called NGC 1313 X-1 and X-2. [21] The former is a rare intermediate-mass black hole. [22] [23]

Related Research Articles

<span class="mw-page-title-main">Messier 82</span> Starburst galaxy in the constellation Ursa Major

Messier 82 (also known as NGC 3034, Cigar Galaxy or M82) is a starburst galaxy approximately 12 million light-years away in the constellation Ursa Major. It is the second-largest member of the M81 Group, with the D25 isophotal diameter of 12.52 kiloparsecs (40,800 light-years). It is about five times more luminous than the Milky Way and its central region is about one hundred times more luminous. The starburst activity is thought to have been triggered by interaction with neighboring galaxy M81. As one of the closest starburst galaxies to Earth, M82 is the prototypical example of this galaxy type. SN 2014J, a type Ia supernova, was discovered in the galaxy on 21 January 2014. In 2014, in studying M82, scientists discovered the brightest pulsar yet known, designated M82 X-2.

<span class="mw-page-title-main">Pinwheel Galaxy</span> Galaxy in the constellation Ursa Major

The Pinwheel Galaxy is a face-on, unbarred, and counterclockwise spiral galaxy located 21 million light-years from Earth in the constellation Ursa Major. It was discovered by Pierre Méchain in 1781 and was communicated that year to Charles Messier, who verified its position for inclusion in the Messier Catalogue as one of its final entries.

<span class="mw-page-title-main">Messier 83</span> Barred spiral galaxy in the constellation Hydra

Messier 83 or M83, also known as the Southern Pinwheel Galaxy and NGC 5236, is a barred spiral galaxy approximately 15 million light-years away in the constellation borders of Hydra and Centaurus. Nicolas-Louis de Lacaille discovered M83 on 17 February 1752 at the Cape of Good Hope. Charles Messier added it to his catalogue of nebulous objects in March 1781.

<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">Messier 74</span> Face-on spiral galaxy in the constellation Pisces

Messier 74 is a large spiral galaxy in the equatorial constellation Pisces. It is about 32 million light-years away from Earth. The galaxy contains two clearly defined spiral arms and is therefore used as an archetypal example of a grand design spiral galaxy. The galaxy's low surface brightness makes it the most difficult Messier object for amateur astronomers to observe. Its relatively large angular size and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study spiral arm structure and spiral density waves. It is estimated that M74 hosts about 100 billion stars.

<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 95</span> Galaxy in the constellation Leo

Messier 95, also known as M95 or NGC 3351, is a barred spiral galaxy about 33 million light-years away in the zodiac constellation Leo. It was discovered by Pierre Méchain in 1781, and catalogued by compatriot Charles Messier four days later. In 2012 its most recent supernova was discovered.

<span class="mw-page-title-main">NGC 6946</span> Galaxy in the constellations Cepheus & Cygnus

NGC 6946, sometimes referred to as the Fireworks Galaxy, is a face-on intermediate spiral galaxy with a small bright nucleus, whose location in the sky straddles the boundary between the northern constellations of Cepheus and Cygnus. Its distance from Earth is about 25.2 million light-years or 7.72 megaparsecs, similar to the distance of M101 in the constellation Ursa Major. Both were once considered to be part of the Local Group, but are now known to be among the dozen bright spiral galaxies near the Milky Way but beyond the confines of the Local Group. NGC 6946 lies within the Virgo Supercluster.

<span class="mw-page-title-main">NGC 7793</span> Galaxy in the constellation Sculptor

NGC 7793 is a flocculent spiral galaxy in the southern constellation of Sculptor. It was discovered in 1826 by Scottish astronomer James Dunlop. The galaxy is located at a distance of 12.2 million light years and is receding with a heliocentric radial velocity of 227 km/s. NGC 7793 is one of the five brightest galaxies within the Sculptor Group.

<span class="mw-page-title-main">NGC 3310</span> Galaxy in the constellation Ursa Major

NGC 3310 is a grand design spiral galaxy in the constellation Ursa Major. It is a starburst galaxy and it is likely that NGC 3310 collided with one of its satellite galaxies about 100 million years ago, triggering widespread star formation. It is thought to be located approximately 46 million light-years away from the Earth, and is thought to be about 22,000 light-years wide.

<span class="mw-page-title-main">NGC 5253</span> Irregular galaxy in the M83 group of galaxies

NGC 5253 is an irregular galaxy in the constellation Centaurus. It was discovered by William Herschel on 15 March 1787.

<span class="mw-page-title-main">Ultraluminous X-ray source</span>

In astronomy and astrophysics, an ultraluminous X-ray source (ULX) is less luminous than an active galactic nucleus but more consistently luminous than any known stellar process (over 1039 erg/s, or 1032 watts), assuming that it radiates isotropically (the same in all directions). Typically there is about one ULX per galaxy in galaxies which host them, but some galaxies contain many. The Milky Way has not been shown to contain an ULX, although SS 433 is a candidate. The main interest in ULXs stems from their luminosity exceeding the Eddington luminosity of neutron stars and even stellar black holes. It is not known what powers ULXs; models include beamed emission of stellar mass objects, accreting intermediate-mass black holes, and super-Eddington emission.

<span class="mw-page-title-main">NGC 4536</span> Spiral galaxy in the constellation Virgo

NGC 4536 is an intermediate spiral galaxy in the constellation Virgo located about 10° south of the midpoint of the Virgo cluster. However, it is not considered a member of the cluster. Rather, 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. The morphological classification in the De Vaucouleurs system is SAB(rs)bc, which indicates it is a weakly barred spiral galaxy with a hint of an inner ring structure plus moderate to loosely wound arms. It does not have a classical bulge around the nucleus.

<span class="mw-page-title-main">NGC 7424</span> Galaxy in the constellation Grus

NGC 7424 is a barred spiral galaxy located 37.5 million light-years away in the southern constellation Grus. Its size makes it similar to our own galaxy, the Milky Way. It is called a "grand design" galaxy because of its well defined spiral arms. Two supernovae and two ultraluminous X-ray sources have been discovered in NGC 7424.

<span class="mw-page-title-main">NGC 266</span> Galaxy in the constellation Pisces

NGC 266 is a massive barred spiral galaxy in the constellation Pisces. NGC 266 is located at a distance of 197 megalight-years from the Milky Way. It was discovered on September 12, 1784, by William Herschel. The form of this barred galaxy is described by its morphological classification of SB(rs)ab, which indicates a quasi-ring-like structure (rs) and moderate-to-tightly wound spiral arms (ab).

<span class="mw-page-title-main">NGC 7552</span> Galaxy in the constellation Grus

NGC 7552 is a barred spiral galaxy in the constellation Grus. It is at a distance of roughly 60 million light years from Earth, which, given its apparent dimensions, means that NGC 7552 is about 75,000 light years across. It forms with three other spiral galaxies the Grus Quartet.

<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 3256</span> Peculiar galaxy in the constellation Vela

NGC 3256 is a peculiar galaxy formed from the collision of two separate galaxies in the constellation of Vela. NGC 3256 is located about 100 million light-years away and belongs to the Hydra–Centaurus Supercluster complex. NGC 3256 provides a nearby template for studying the properties of young star clusters in tidal tails. The system hides a double nucleus and a tangle of dust lanes in the central region. The telltale signs of the collision are two extended luminous tails swirling out from the galaxy. The tails are studded with a particularly high density of star clusters. NGC 3256 is the most luminous galaxy in the infrared spectrum located within z 0.01 from Earth.

<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 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.

References

  1. 1 2 3 4 5 6 "NASA/IPAC Extragalactic Database". Results for NGC 1313. Retrieved 17 May 2023.
  2. 1 2 "The Topsy-Turvy Galaxy NGC 1313". ESO. 23 November 2006.
  3. ↑ "Taking a narrow view of lopsided galaxy". Gemini Observatory. 21 May 2010. Archived from the original on 12 June 2015. Retrieved 22 February 2016.
  4. ↑ Nemiroff, R.; Bonnell, J., eds. (7 August 2009). "The Star Clusters of NGC 1313". Astronomy Picture of the Day . NASA.
  5. ↑ Courtney Seligman. "NGC 1313 (= PGC 12286)". Celestial Atlas. Archived from the original on 2015-06-12. Retrieved 2016-02-22.
  6. ↑ Nemiroff, R.; Bonnell, J., eds. (30 March 2010). "Unusual Starburst Galaxy NGC 1313". Astronomy Picture of the Day . NASA.
  7. ↑ "Nearby Groups of Galaxies". ned.ipac.caltech.edu. Retrieved 2018-05-07.
  8. 1 2 3 4 Hadfield, L. J.; Crowther, P. A. (2007-10-01). "A survey of the Wolf-Rayet population of the barred, spiral galaxy NGC 1313". Monthly Notices of the Royal Astronomical Society. 381 (1): 418–432. arXiv: 0708.2039 . Bibcode:2007MNRAS.381..418H. doi: 10.1111/j.1365-2966.2007.12284.x . ISSN   0035-8711. S2CID   3024190.
  9. ↑ Hill, P. W. (1965). "The Spectrum of the 1962 Supernova in NGC 1313". Monthly Notices of the Royal Astronomical Society. 131: 155–157. doi: 10.1093/mnras/131.1.155 .
  10. ↑ "SN 1962M". Transient Name Server. IAU . Retrieved 1 December 2024.
  11. ↑ Dopita, M. A.; Ryder, S. D. (1990). "Nova in NGC 1313". International Astronomical Union Circular. 4950: 3. Bibcode:1990IAUC.4950....3D.
  12. ↑ Ryder, Stuart; Staveley-Smith, Lister; Dopita, Michael; Petre, Robert; Colbert, Edward; Malin, David; Schlegel, Eric (1993). "SN 1978K: An Extraordinary Supernova in the Nearby Galaxy NGC 1313". The Astrophysical Journal. 416: 167. doi: 10.1086/173223 .
  13. ↑ Materne, J. (April 1979). "The structure of nearby groups of galaxies - Quantitative membership probabilities". Astronomy and Astrophysics. 74 (2): 235–243. Bibcode:1979A&A....74..235M.
  14. ↑ "VLT Image of Starburst Galaxy NGC 1313". European Southern Observatory. 23 November 2006. Retrieved 22 February 2016.
  15. ↑ Suzuki; et al. (2013). "AKARI view of star formation in NGC 1313". Astronomy & Astrophysics. 554: A8. Bibcode:2013A&A...554A...8S. doi: 10.1051/0004-6361/201220294 .
  16. ↑ "NGC 1313". Astrosurf. 22 October 2006.
  17. ↑ "Tumult in NGC 1313" (in German). Wissenschaft.de. 28 November 2006.
  18. ↑ "Hubble Sees Star Cluster "Infant Mortality"". NASA. 10 January 2007. Retrieved 23 February 2016.
  19. ↑ Anne Pellerin; Martin Meyer; Jason Harris; Daniela Calzetti (2007). "Stellar Clusters in NGC 1313: Evidence of Infant Mortality". The Astrophysical Journal. 653 (2): L87–L90. arXiv: astro-ph/0702547 . Bibcode:2007ApJ...658L..87P. doi:10.1086/515437. S2CID   5537525.
  20. ↑ Mollá, Mercedes; Roy, Jean-René (1 April 1999). "Modeling the Radial Abundance Distribution of the Transition Galaxy NGC 1313". The Astrophysical Journal. 514 (2): 781–786. arXiv: astro-ph/9903129 . Bibcode:1999ApJ...514..781M. doi:10.1086/306982. S2CID   18874798.
  21. ↑ Matteo Bachetti; et al. (2013). "The Ultraluminous X-Ray Sources NGC 1313 X-1 and X-2: A Broadband Study with NuSTAR and XMM-Newton". The Astrophysical Journal. 778 (2): 163. arXiv: 1310.0745 . Bibcode:2013ApJ...778..163B. doi:10.1088/0004-637X/778/2/163. S2CID   28161179.
  22. ↑ Dheeraj Pasham; et al. (2015). "Evidence for High-Frequency QPOs with a 3:2 Frequency Ratio from a 5000 Solar Mass Black Hole". The Astrophysical Journal. 811 (1): L11. arXiv: 1601.02628 . Bibcode:2015ApJ...811L..11P. doi:10.1088/2041-8205/811/1/L11. S2CID   33907571.
  23. ↑ "Intermediate-Mass Black Hole 5,000 Times Mass of Sun". Sci-News.com. 23 September 2015. Retrieved 23 February 2016.
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.