Messier 82

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Messier 82
M82 HST ACS 2006-14-a-large web.jpg
A mosaic image taken by the Hubble Space Telescope of Messier 82, combining exposures taken with four colored filters that capture starlight from visible and infrared wavelengths as well as the light from the glowing hydrogen filaments
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 09h 55m 52.2s [1]
Declination +69° 40′ 47″ [1]
Redshift 203±4 km/s [1]
Distance 11.4–12.4 Mly (3.5–3.8 Mpc) [2]
Apparent magnitude  (V)8.41 [3] [4]
Characteristics
Type I0 [1]
Size12.52 kiloparsecs (40,800 light-years)
(diameter; 25.0 mag/arcsec2 B-band isophote) [1] [5]
Apparent size  (V)11.2′ × 4.3′ [1]
Notable featuresEdge-on starburst galaxy
Other designations
NGC 3034, UGC 5322, Arp 337, Cigar Galaxy, PGC 28655, 3C 231 [1]
M82 Galaxy
PIA23010-M82-CigarGalaxy-20190305.jpg
M82 magnetic field
M82 Chandra HST Spitzer.jpg
Composite image – HST (vis); Spitzer (ir); Chandra (x-ray)
M82(2).jpg
Chandra X-ray observatory image of the galaxy
Hubble views new supernova in Messier 82.jpg
Hubble views new supernova in Messier 82 [6]
M 82 supernova.jpg
M82 – December 2013; supernova – January 2014 (bottom)
M82 Bin1 No Logo Resample.jpg
Messier 82 photographed by amateur astrophotographer Radu Marinescu using a 10" Newtonian telescope, with a high emphasis on the Hydrogen-alpha star-burst areas.

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 ). [1] [5] It is about five times more luminous than the Milky Way and its central region is about one hundred times more luminous. [7] 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. [7] [lower-alpha 1] SN 2014J, a type Ia supernova, was discovered in the galaxy on 21 January 2014. [8] [9] [10] In 2014, in studying M82, scientists discovered the brightest pulsar yet known, designated M82 X-2. [11] [12] [13]

Contents

In November 2023, a gamma-ray burst was observed in M82, which was determined to have come from a magnetar, the first such event detected outside the Milky Way (and only the fourth such event ever detected). [14] [15]

Discovery

M82, with M81, was discovered by Johann Elert Bode in 1774; he described it as a "nebulous patch", this one about 3⁄4 degree away from the other, "very pale and of elongated shape". In 1779, Pierre Méchain independently rediscovered both objects and reported them to Charles Messier, who added them to his catalog. [16]

Structure

M82 was believed to be an irregular galaxy. In 2005, however, two symmetric spiral arms were discovered in near-infrared (NIR) images of M82. The arms were detected by subtracting an axisymmetric exponential disk from the NIR images. Even though the arms were detected in NIR images, they are bluer than the disk. The arms had been missed due to M82's high disk surface brightness, the nearly edge-on view of this galaxy (~80°), [7] and obscuration by a complex network of dusty filaments in its optical images. These arms emanate from the ends of the NIR bar and can be followed for the length of 3 disc scales. Assuming that the northern part of M82 is nearer to us, as most of the literature does, the observed sense of rotation implies trailing arms. [17]

Starburst region

In 2005, the Hubble Space Telescope revealed 197 young massive clusters in the starburst core. [7] The average mass of these clusters is around 200,000 solar masses, hence the starburst core is a very energetic and high-density environment. [7] Throughout the galaxy's center, young stars are being born 10 times faster than they are inside the entire Milky Way Galaxy. [18]

In the core of M82, the active starburst region spans a diameter of 500 pc. Four high surface brightness regions or clumps (designated A, C, D, and E) are detectable in this region at visible wavelengths. [7] These clumps correspond to known sources at X-ray, infrared, and radio frequencies. [7] Consequently, they are thought to be the least obscured starburst clusters from our vantage point. [7] M82's unique bipolar outflow (or 'superwind') appears to be concentrated on clumps A and C, and is fueled by energy released by supernovae within the clumps which occur at a rate of about one every ten years. [7]

The Chandra X-ray Observatory detected fluctuating X-ray emissions about 600 light-years from the center of M82. Astronomers have postulated that this comes from the first known intermediate-mass black hole, of roughly 200 to 5000 solar masses. [19] M82, like most galaxies, hosts a supermassive black hole at its center. [20] This one has mass of approximately 3 × 107 solar masses, as measured from stellar dynamics. [20]

Unknown object

In April 2010, radio astronomers working at the Jodrell Bank Observatory of the University of Manchester in the UK reported an object in M82 that had started sending out radio waves, and whose emission did not look like anything seen anywhere in the universe before. [21]

There have been several theories about the nature of this object, but currently no theory entirely fits the observed data. [21] It has been suggested that the object could be an unusual "micro quasar", having very high radio luminosity yet low X-ray luminosity, and being fairly stable, it could be an analogue of the low X-ray luminosity galactic microquasar SS 433. [22] However, all known microquasars produce large quantities of X-rays, whereas the object's X-ray flux is below the measurement threshold. [21] The object is located at several arcseconds from the center of M82 which makes it unlikely to be associated with a supermassive black hole. It has an apparent superluminal motion of four times the speed of light relative to the galaxy center. [23] [24] Apparent superluminal motion is consistent with relativistic jets in massive black holes and does not indicate that the source itself is moving above lightspeed. [23]

Starbursts

M82 is being physically affected by its larger neighbor, the spiral M81. Tidal forces caused by gravity have deformed M82, a process that started about 100 million years ago. This interaction has caused star formation to increase tenfold compared to "normal" galaxies.

M82 has undergone at least one tidal encounter with M81 resulting in a large amount of gas being funneled into the galaxy's core over the last 200 Myr. [7] The most recent such encounter is thought to have happened around 2–5×108 years ago and resulted in a concentrated starburst together with a corresponding marked peak in the cluster age distribution. [7] This starburst ran for up to ~50 Myr at a rate of ~10 M⊙ per year. [7] Two subsequent starbursts followed, the last (~4–6 Myr ago) of which may have formed the core clusters, both super star clusters (SSCs) and their lighter counterparts. [7]

Stars in M82's disk seem to have been formed in a burst 500 million years ago, leaving its disk littered with hundreds of clusters with properties similar to globular clusters (but younger), and stopped 100 million years ago with no star formation taking place in this galaxy outside the central starburst and, at low levels since 1 billion years ago, on its halo. A suggestion to explain those features is that M82 was previously a low surface brightness galaxy where star formation was triggered due to interactions with its giant neighbor. [25] Ignoring any difference in their respective distances from the Earth, the centers of M81 and M82 are visually separated by about 130,000 light-years. [26] The actual separation is 300+300
−200 kly. [27] [2]

Supernovae

As a starburst galaxy, Messier 82 is prone to frequent supernova, caused by the collapse of young, massive stars. The first (although false) supernova candidate reported was SN 1986D, initially believed to be a supernova inside the galaxy until it was found to be a variable short-wavelength infrared source instead. [28]

The first confirmed supernova recorded in the galaxy was SN 2004am, discovered in March 2004 from images taken in November 2003 by the Lick Observatory Supernova Search. It was later determined to be a Type II supernova. [29] In 2008, a radio transient was detected in the galaxy, designated SN 2008iz and thought to be a possible radio-only supernova, being too obscured in visible light by dust and gas clouds to be detectable. [30] A similar radio-only transient was reported in 2009, although never received a formal designation and was similarly unconfirmed. [28]

Prior to accurate and thorough supernova surveys, many other supernovae likely occurred in previous decades. The European VLBI Network studied a number of potential supernova remnants in the galaxy in the 1980s and 90s. One supernova remnant displayed clear expansion between 1986 and 1997 that suggested it originally went supernova in the early 1960s, and two other remnants show possible expansion that could indicate an age almost as young, but could not be confirmed at the time. [31]

2014 supernova

On 21 January 2014 at 19.20 UT, a new distinct star was observed in M82, at apparent magnitude +11.7, by astrophysics lecturer Steve Fossey and four of his students, at the University of London Observatory. It had brightened to magnitude +10.9 two days later. Examination of earlier observations of M82 found the supernova to figure on the intervening day as well as on 15 through 20 January, brightening from magnitude +14.4 to +11.3; it could not be found, to limiting magnitude +17, from images caught of 14 January. It was initially suggested that it could become as bright as magnitude +8.5, well within the visual range of small telescopes and large binoculars, [32] but peaked at fainter +10.5 on the last day of the month. [33] Preliminary analysis classified it as "a young, reddened type Ia supernova". The International Astronomical Union (IAU) has designated it SN 2014J. [34] SN 1993J was also at relatively close distance, in M82's larger companion galaxy M81. SN 1987A in the Large Magellanic Cloud was much closer. 2014J is the closest type Ia supernova since SN 1972E. [8] [9] [10]

See also

Notes

  1. ↑ The irregular galaxy IC 10 in the Local Group is sometimes classified as a starburst galaxy, and hence is the closest such galaxy to Earth.

Related Research Articles

<span class="mw-page-title-main">M81 Group</span> Galaxy group in Ursa Major and Camelopardalis

The M81 Group is a galaxy group in the constellations Ursa Major and Camelopardalis that includes the galaxies Messier 81 and Messier 82, as well as several other galaxies with high apparent brightnesses. The approximate center of the group is located at a distance of 3.6 Mpc, making it one of the nearest groups to the Local Group. The group is estimated to have a total mass of ×1012M☉. The M81 Group, the Local Group, and other nearby groups all lie within the Virgo Supercluster.

<span class="mw-page-title-main">Messier 100</span> Galaxy in the constellation Coma Berenices

Messier 100 is a grand design intermediate spiral galaxy in the southern part of the mildly northern Coma Berenices. It is one of the brightest and largest galaxies in the Virgo Cluster and is approximately 55 million light-years from our galaxy, its diameter being 107,000 light years, and being about 60% as large. It was discovered by Pierre Méchain in 1781 and 29 days later seen again and entered by Charles Messier in his catalogue "of nebulae and star clusters". It was one of the first spiral galaxies to be discovered, and was listed as one of fourteen spiral nebulae by Lord William Parsons of Rosse in 1850. NGC 4323 and NGC 4328 are satellite galaxies of M100; the former is connected with it by a bridge of luminous matter.

<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">Starburst galaxy</span> Galaxy undergoing an exceptionally high rate of star formation

A starburst galaxy is one undergoing an exceptionally high rate of star formation, as compared to the long-term average rate of star formation in the galaxy, or the star formation rate observed in most other galaxies.

<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">Whirlpool Galaxy</span> Galaxy in the constellation Canes Venatici

The Whirlpool Galaxy, also known as Messier 51a (M51a) or NGC 5194, is an interacting grand-design spiral galaxy with a Seyfert 2 active galactic nucleus. It lies in the constellation Canes Venatici, and was the first galaxy to be classified as a spiral galaxy. It is 7.22 megaparsecs away and 23.58 kiloparsecs (76,900 ly) in diameter.

<span class="mw-page-title-main">Messier 81</span> Spiral galaxy in the constellation Ursa Major

Messier 81 (also known as NGC 3031 or Bode's Galaxy) is a grand design spiral galaxy about 12 million light-years away in the constellation Ursa Major. It has a D25 isophotal diameter of 29.44 kiloparsecs (96,000 light-years). Because of its relative proximity to the Milky Way galaxy, large size, and active galactic nucleus (which harbors a 70 million M☉ supermassive black hole), Messier 81 has been studied extensively by professional astronomers. The galaxy's large size and relatively high brightness also makes it a popular target for amateur astronomers. In late February 2022, astronomers reported that M81 may be the source of FRB 20200120E, a repeating fast radio burst.

<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 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 99</span> Spiral galaxy in the constellation Coma Berenices

Messier 99 or M99, also known as NGC 4254 or St. Catherine's Wheel, is a grand design spiral galaxy in the northern constellation Coma Berenices approximately 15,000,000 parsecs from the Milky Way. It was discovered by Pierre Méchain on 17 March 1781. The discovery was then reported to Charles Messier, who included the object in the Messier Catalogue of comet-like objects. It was one of the first galaxies in which a spiral pattern was seen. This pattern was first identified by Lord Rosse in the spring of 1846.

<span class="mw-page-title-main">Messier 108</span> Galaxy in the constellation Ursa Major

Messier 108 is a barred spiral galaxy about 28 million light-years away from Earth in the northern constellation Ursa Major. It was discovered by Pierre Méchain in 1781 or 1782. From the Earth, this galaxy is seen almost edge-on.

<span class="mw-page-title-main">Sculptor Galaxy</span> Intermediate spiral galaxy in the constellation Sculptor

The Sculptor Galaxy is an intermediate spiral galaxy in the constellation Sculptor. The Sculptor Galaxy is a starburst galaxy, which means that it is currently undergoing a period of intense star formation.

<span class="mw-page-title-main">NGC 4639</span> Galaxy in the constellation Virgo

NGC 4639 is a barred spiral galaxy located in the equatorial constellation of Virgo. It was discovered by German-born astronomer William Herschel on April 12, 1784. John L. E. Dreyer described it as "pretty bright, small, extended, mottled but not resolved, 12th magnitude star 1 arcmin to southeast". This is a relatively nearby galaxy, lying approximately 72 million light-years away from the Milky Way. It is a companion to NGC 4654, and the two appear to have interacted roughly 500 million years ago. NGC 4639 is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4666</span> Spiral galaxy in the constellation Virgo

NGC 4666 is a spiral galaxy in the equatorial constellation of Virgo, located at a distance of approximately 55 megalight-years from the Milky Way. It was discovered by the German-born astronomer William Herschel on February 22, 1784. 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. John L. E. Dreyer described it as "bright, very large, much extended 45°±, pretty suddenly brighter middle". It is a member of an interacting system with NGC 4668 and a dwarf galaxy, and belongs to a small group that also includes NGC 4632.

<span class="mw-page-title-main">SN 2014J</span> Supernova in Messier 82

SN 2014J was a type-Ia supernova in Messier 82 discovered in mid-January 2014. It was the closest type-Ia supernova discovered for 42 years, and no subsequent supernova has been closer as of 2023. The supernova was discovered by chance during an undergraduate teaching session at the University of London Observatory. It peaked on 31 January 2014, reaching an apparent magnitude of 10.5. SN 2014J was the subject of an intense observing campaign by professional astronomers and was bright enough to be seen by amateur astronomers.

<span class="mw-page-title-main">NGC 3859</span> Spiral galaxy in the constellation Leo

NGC 3859 is a spiral galaxy located about 295 million light-years away in the constellation Leo. It was discovered by astronomer Édouard Stephan on March 23, 1884. The galaxy is a member of the Leo Cluster.

<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 6951</span> Galaxy in the constellation Cepheus

NGC 6951 is a barred spiral galaxy located in the constellation Cepheus. It is located at a distance of about 75 million light-years from Earth, which, given its apparent dimensions, means that NGC 6951 is about 100,000 light-years across. It was discovered by Jérôme Eugène Coggia in 1877 and independently by Lewis Swift in 1878.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 3034. Retrieved 27 October 2006.
  2. 1 2 Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the local group and of the M81 group estimated from distortions in the local velocity field". Astrophysics. 49 (1): 3–18. Bibcode:2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6. S2CID   120973010.
  3. ↑ "M 82". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 14 December 2018.
  4. ↑ Armando, Gil de Paz; Boissier; Madore; Seibert; Boselli; et al. (2007). "The GALEX Ultraviolet Atlas of Nearby Galaxies". Astrophysical Journal Supplement . 173 (2): 185–255. arXiv: astro-ph/0606440 . Bibcode:2007ApJS..173..185G. doi:10.1086/516636. S2CID   119085482.
  5. 1 2 De Vaucouleurs, Gerard; De Vaucouleurs, Antoinette; Corwin, Herold G.; Buta, Ronald J.; Paturel, Georges; Fouque, Pascal (1991). Third Reference Catalogue of Bright Galaxies. Bibcode:1991rc3..book.....D.
  6. ↑ "Hubble views new supernova in Messier 82". ESA / HUBBLE. Retrieved 12 March 2014.
  7. 1 2 3 4 5 6 7 8 9 10 11 12 13 Barker, S.; de Grijs, R.; Cerviño, M. (2008). "Star cluster versus field star formation in the nucleus of the prototype starburst galaxy M 82". Astronomy and Astrophysics . 484 (3): 711–720. arXiv: 0804.1913 . Bibcode:2008A&A...484..711B. doi:10.1051/0004-6361:200809653. S2CID   18885080.
  8. 1 2 "ATel #5786: Classification of Supernova in M82 as a young, reddened Type Ia Supernova". ATel. Retrieved 14 April 2018.
  9. 1 2 "Sudden Supernova in M82 Galaxy Rips Apart The Night Sky (A Bit)". Huffington Post. 22 January 2014.
  10. 1 2 Plait, Phil (22 January 2014). "KABOOM! Nearby Galaxy M82 Hosts a New Supernova!". Slate.
  11. ↑ "Shockingly Bright Dead Star with a Pulse Is an X-ray Powerhouse". Space.com. 8 October 2014.
  12. ↑ "Researchers detect brightest pulsar ever recorded". Massachusetts Institute of Technology. 8 October 2014.
  13. ↑ "NASA's NuSTAR Telescope Discovers Shockingly Bright Dead Star". NASA. 8 October 2014.
  14. ↑ Mereghetti, Sandro; Rigoselli, Michela; Salvaterra, Ruben; Pacholski, Dominik Patryk; Rodi, James Craig; Gotz, Diego; Arrigoni, Edoardo; D'Avanzo, Paolo; Adami, Christophe; Bazzano, Angela; Bozzo, Enrico; Brivio, Riccardo; Campana, Sergio; Cappellaro, Enrico; Chenevez, Jerome; De Luise, Fiore; Ducci, Lorenzo; Esposito, Paolo; Ferrigno, Carlo; Ferro, Matteo; Israel, Gian Luca; Le Floc'h, Emeric; Martin-Carrillo, Antonio; Onori, Francesca; Rea, Nanda; Reguitti, Andrea; Savchenko, Volodymyr; Souami, Damya; Tartaglia, Leonardo; Thuillot, William; Tiengo, Andrea; Tomasella, Lina; Topinka, Martin; Turpin, Damien; Ubertini, Pietro (10 March 2024). "A magnetar giant flare in the nearby starburst galaxy M82". Astrophysics. 629 (2): 58–61. arXiv: 2312.14645 . Bibcode:2024Natur.629...58M. doi:10.1038/s41586-024-07285-4. PMID   38658757.
  15. ↑ Smith, Kiona (25 April 2024). "A Dead Star in a Nearby Galaxy Just Did Something Wild". Inverse. Retrieved 26 April 2024.
  16. ↑ "Messier 82". SEDS.
  17. ↑ Mayya, Y. D.; Carrasco, L.; Luna, A. (2005). "The Discovery of Spiral Arms in the Starburst Galaxy M82". Astrophysical Journal . 628 (1): L33–L36. arXiv: astro-ph/0506275 . Bibcode:2005ApJ...628L..33M. doi:10.1086/432644. S2CID   17576187.
  18. ↑ Happy Sweet Sixteen, Hubble Telescope! Newswise, Retrieved 30 July 2008.
  19. ↑ Patruno, A.; Portegies Zwart, S.; Dewi, J.; Hopman, C. (2006). "The ultraluminous X-ray source in M82: an intermediate-mass black hole with a giant companion". Monthly Notices of the Royal Astronomical Society: Letters . 370 (1): L6–L9. arXiv: astro-ph/0602230 . Bibcode:2006MNRAS.370L...6P. doi: 10.1111/j.1745-3933.2006.00176.x . S2CID   10694200.
  20. 1 2 Gaffney, N. I.; Lester, D. F. & Telesco, C. M. (1993). "The stellar velocity dispersion in the nucleus of M82". Astrophysical Journal Letters . 407: L57–L60. Bibcode:1993ApJ...407L..57G. doi:10.1086/186805.
  21. 1 2 3 "Mysterious radio waves emitted from nearby galaxy" . Retrieved 14 April 2018.
  22. ↑ Tana Joseph, Thomas Maccarone, Robert Fender: The unusual radio transient in M82: an SS 433 analogue? , 2011-07-25
  23. 1 2 Muxlow, T. W. B.; Beswick, R. J.; Garrington, S. T.; Pedlar, A.; Fenech, D. M.; Argo, M. K.; Van Eymeren, J.; Ward, M.; Zezas, A.; Brunthaler, A.; Rich, R. M.; Barlow, T. A.; Conrow, T.; Forster, K.; Friedman, P. G.; Martin, D. C.; Morrissey, P.; Neff, S. G.; Schiminovich, D.; Small, T.; Donas, J.; Heckman, T. M.; Lee, Y. -W.; Milliard, B.; Szalay, A. S.; Yi, S. (2010). "Discovery of an unusual new radio source in the star-forming galaxy M82: Faint supernova, supermassive black hole or an extragalactic microquasar?". Monthly Notices of the Royal Astronomical Society: Letters. 404 (1): L109–L113. arXiv: 1003.0994 . Bibcode:2010MNRAS.404L.109M. doi: 10.1111/j.1745-3933.2010.00845.x . S2CID   119302437.
  24. ↑ O'Brien, Tim. "Mystery object in Starburst Galaxy M82 – Jodrell Bank Centre for Astrophysics". www.jb.man.ac.uk. Retrieved 14 April 2018.
  25. ↑ Divakara Mayya, Y.; Carrasco, Luis (2009). "M82 as a Galaxy: Morphology and Stellar Content of the Disk and Halo". Revista Mexicana de Astronomía y Astrofísica, Serie de Conferencias. 37: 44–55. arXiv: 0906.0757 . Bibcode:2009arXiv0906.0757D.
  26. ↑ Declination separation of 36.87′ and Right Ascension separation of 9.5′ gives via Pythagorean theorem a visual separation of 38.07′; Average distance of 11.65 Mly × sin(38.07′) = 130,000 ly visual separation.
  27. ↑ Separation = sqrt(DM812 + DM822 – 2 DM81 DM82 Cos(38.07′)) assuming the error direction is about the same for both objects.
  28. 1 2 "Messier Object 82". www.messier.seds.org. Archived from the original on 14 July 2020. Retrieved 14 July 2020.
  29. ↑ "SN 2004am | Transient Name Server". wis-tns.weizmann.ac.il. Retrieved 14 July 2020.
  30. ↑ "SN 2008iz | Transient Name Server". wis-tns.weizmann.ac.il. Retrieved 14 July 2020.
  31. ↑ Pedlar, A.; Muxlow, T. W. B.; Garrett, M. A.; Diamond, P.; Wills, K. A.; Wilkinson, P. N.; Alef, W. (August 1999). "VLBI observations of supernova remnants in Messier 82". Monthly Notices of the Royal Astronomical Society. 307 (4): 761–768. Bibcode:1999MNRAS.307..761P. doi: 10.1046/j.1365-8711.1999.02642.x .
  32. ↑ "Astronomy Now: Bright, young supernova outburst in Messier 82, MARK ARMSTRONG, 23 January 2014". Archived from the original on 2 December 2020. Retrieved 14 April 2018.
  33. ↑ "Supernova in M82 Passes Its Peak – Sky & Telescope". 17 February 2014. Archived from the original on 14 February 2014. Retrieved 14 April 2018.
  34. ↑ "Supernova in Messier 82 discovered by UCL students". www.ucl.ac.uk. Archived from the original on 23 January 2014. Retrieved 14 April 2018.
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