Canis Major

Canis Major

Canis Major
Canis Major
Abbreviation CMa
Genitive Canis Majoris
Pronunciation , genitive
Symbolism the greater dog
Right ascension 06h 12.5m to 07h 27.5m[1]
Declination −11.03° to −33.25°[1]
Family Orion
Quadrant SQ2
Area 380 sq. deg. (43rd)
Main stars 8
Stars with planets 7
Stars brighter than 3.00m 5
Stars within 10.00 pc (32.62 ly) 1
Brightest star Sirius (α CMa) (−1.46m)
Nearest star Sirius (α CMa)
(8.60 ly, 2.64 pc)
Messier objects 1
Meteor showers None
Visible at latitudes between +60° and −90°.
Best visible at 21:00 (9 p.m.) during the month of February.

Canis Major is a constellation in the southern celestial hemisphere. In the second century, it was included in Ptolemy's 48 constellations, and is counted among the 88 modern constellations. Its name is Latin for "greater dog" in contrast to Canis Minor, the "lesser dog"; both figures are commonly represented as following the constellation of Orion the hunter. The Milky Way passes through Canis Major and several open clusters lie within its borders.

Canis Major contains Sirius, the brightest star in the night sky, known as the 'dog star'. It is bright because of its proximity to our Solar System. In contrast, the other bright stars of the constellation are stars of great distance and high luminosity. At magnitude 1.5, Epsilon Canis Majoris (Adhara) is the second brightest star of the constellation and one of the brightest sources of ultraviolet radiation in the night sky. Next in brightness are the yellow-white supergiant Delta (Wezen) at 1.8, the blue-white giant Beta (Mirzam) at 2.0, blue-white supergiants Eta (Aludra) at 2.4 and Omicron1 at 3.0, and white spectroscopic binary Zeta (Furud), also at 3.0. The red hypergiant VY Canis Majoris is one of the largest stars known, while the neutron star RX J0720.4-3125 has a radius of a mere 5 km.


  • History and mythology 1
    • In western astronomy 1.1
    • In non-western astronomy 1.2
  • Characteristics 2
  • Notable features 3
    • Stars 3.1
    • Deep-sky objects 3.2
  • Notes 4
    • Cited texts 4.1
  • External links 5

History and mythology

In western astronomy

In ancient Mesopotamia, Sirius, named KAK.SI.DI by the Babylonians, was seen as an arrow aiming towards Orion, while the southern stars of Canis Major and a part of Puppis were viewed as a bow, named BAN in the Three Stars Each tablets, dating to around 1100 BC. In the later compendium of Babylonian astronomy and astrology titled MUL.APIN, the arrow, Sirius, was also linked with the warrior Ninurta, and the bow with Ishtar, daughter of Enlil.[2] Ninurta was linked to the later deity Marduk, who was said to have slain the ocean goddess Tiamat with a great bow, and worshipped as the principal deity in Babylon.[3] The Ancient Greeks replaced the bow and arrow depiction with that of a dog.[4]

In Greek Mythology, Canis Major represented the dog Laelaps, a gift from Zeus to Europa; or sometimes the hound of Procris, Diana's nymph; or the one given by Aurora to Cephalus, so famed for its speed that Zeus elevated it to the sky.[5] It was also considered to represent one of Orion's hunting dogs,[6] pursuing Lepus the Hare or helping Orion fight Taurus the Bull; and is referred to in this way by Aratos, Homer and Hesiod. The ancient Greeks refer only to one dog, but by Roman times, Canis Minor appears as Orion's second dog. Alternative names include Canis Sequens and Canis Alter.[5] Canis Syrius was the name used in the 1521 Alfonsine Tables.[5]

The Roman myth refers to Canis Major as Custos Europae, the dog guarding Europa but failing to prevent her abduction by Jupiter in the form of a bull; and as Janitor Lethaeus, "the watchdog".[7] In medieval Arab astronomy, the constellation became Al Kalb al Akbar, "the Greater Dog", transcribed as Alcheleb Alachbar by 17th century writer Edmund Chilmead. Islamic scholar Abū Rayḥān al-Bīrūnī referred to Orion as Al Kalb al Jabbār, "the Dog of the Giant".[5] Among the Merazig of Tunisia, shepherds note six constellations that mark the passage of the dry, hot season. One of them, called Merzem, includes the stars of Canis Major and Canis Minor and is the herald of two weeks of hot weather.[8]

In non-western astronomy

In Chinese astronomy, the modern constellation of Canis Major lies in The Vermillion Bird of the South (南方朱雀, Nán Fāng Zhū Què), where the stars were classified in several separate asterisms of stars. The Military Market (Jūnshì 軍市) was a circular pattern of stars containing Nu3, Beta, Xi1 and Xi2, and some stars from Lepus.[9] The Wild Cockerel (Yějī 野雞) was at the centre of the Military Market, although it is uncertain which stars depicted what. Schlegel reported that the stars Omicron and Pi Canis Majoris might have been them,[10] while Beta or Nu2 have also been proposed.[11] Sirius was Tiānláng (天狼), the Celestial Wolf,[12] denoting invasion and plunder.[11] Southeast of the Wolf was the asterism Húshǐ (弧矢), the celestial Bow and Arrow, which was interpreted as containing Delta, Epsilon, Eta and Kappa Canis Majoris and Delta Velorum. Alternatively, the arrow was depicted by Omicron2 and Eta and aiming at Sirius (the Wolf), while the bow comprised Kappa, Epsilon, Sigma, Delta and 164 Canis Majoris, and Pi and Omicron Puppis.[13]

Both the Maori people and the people of the Tuamotus recognized the figure of Canis Major as a distinct entity, though it was sometimes absorbed into other constellations. Te Huinga-o-Rehua, also called Te Putahi-nui-o-Rehua and Te Kahui-Takurua, ("The Assembly of Rehua" or "The Assembly of Sirius") was a Maori constellation that included both Canis Minor and Canis Major, along with some surrounding stars.[14][15] Related was Taumata-o-Rehua, also called Pukawanui, the Mirror of Rehua, formed from an undefined group of stars in Canis Major.[16][17] They called Sirius Rehua and Takarua, corresponding to two of the names for the constellation, though Rehua was a name applied to other stars in various Maori groups and other Polynesian cosmologies.[18][19] The Tuamotu people called Canis Major Muihanga-hetika-o-Takurua, "the abiding assemblage of Takurua".[20]

The Tharumba people of the Shoalhaven River saw three stars of Canis Major as Wunbula (Bat) and his two wives Murrumbool (Mrs Brown Snake) and Moodtha (Mrs Black Snake); bored of following their husband around, the women try to bury him while he is hunting a wombat down its hole. He spears them and all three are placed in the sky as the constellation Munowra.[21] To the Boorong people of Victoria, Sigma Canis Majoris was Unurgunite, and its flanking stars Delta and Epsilon were his two wives.[22] The moon, Mityan "native cat" sought to lure the further wife (Epsilon) away, but Unurgunite assaulted him and he has been wandering the sky ever since.[23]


Canis Major as depicted in Urania's Mirror, a set of constellation cards published in London c.1825. Next to it are Lepus and Columba (partly cut off).

Canis Major is a constellation in the southern hemisphere's summer (or northern hemisphere's winter) sky, bordered by Monoceros (which lies between it and Canis Minor) to the north, Puppis to the east and southeast, Columba to the southwest, and Lepus to the west. The three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is 'CMa'.[24] The official constellation boundaries, as set by Eugène Delporte in 1930, are defined by a quadrilateral; in the equatorial coordinate system, the right ascension coordinates of these borders lie between 06h 12.5m and 07h 27.5m, while the declination coordinates are between −11.03° and −33.25°.[1] Covering 380 square degrees or 0.921% of the sky, it ranks 43rd of the 88 currently-recognized constellations in size.[25]

Notable features

The constellation Canis Major as it can be seen by the naked eye


Canis Major is a prominent constellation because of its many bright stars. These include Sirius (Alpha Canis Majoris), the brightest star in the night sky, as well as three other stars above magnitude 2.0.[6] Furthermore, two other stars are thought to have previously outshone all others in the night sky—Adhara (Epsilon Canis Majoris) shone at -3.99 around 4.7 million years ago, and Mirzam (Beta Canis Majoris) peaked at −3.65 around 4.42 million years ago, and another—NR Canis Majoris—will be brightest at magnitude −0.88 in about 2.87 million years' time.[26]

The German cartographer Johann Bayer used the Greek letters Alpha through Omicron to label the most prominent stars in the constellation, including three adjacent stars as Nu and two further pairs as Xi and Omicron,[27] while subsequent observers designated further stars in the southern parts of the constellation that were hard to discern from Central Europe.[3] Bayer's countryman Johann Elert Bode later added Sigma, Tau and Omega;[28] the French astronomer Nicolas Louis de Lacaille added lettered stars a to k (though none are in use today).[28] John Flamsteed numbered 31 stars, with 3 Canis Majoris being placed by Lacaille into Columba as Delta Columbae (Flamsteed had not recognised Columba as a distinct constellation).[29] He also labelled two stars—his 10 and 13 Canis Majoris—as Kappa1 and Kappa2 respectively, but subsequent cartographers such as Francis Baily and John Bevis dropped the fainter former star, leaving Kappa2 as the sole Kappa.[27] Flamsteed's listing of Nu1, Nu2, Nu3, Xi1, Xi2, Omicron1 and Omicron2 have all remained in use.[30]

At apparent magnitude −1.46, Sirius is one of the closest stars to Earth at a distance of 8.6 light-years. Its name comes from the Greek word for "scorching" or "searing". Sirius is also a binary star; its companion Sirius B is a white dwarf with a magnitude of 8.4—10,000 times fainter than Sirius A to observers on Earth.[31] The two orbit each other every 50 years. Their closest approach last occurred in 1993 and they will be at their greatest separation between 2020 and 2025. Sirius was the basis for the ancient Egyptian calendar.[6] The star marked the Great Dog's mouth on Bayer's star atlas.[32]

Flanking Sirius are Beta and Gamma Canis Majoris. Also called Mirzam or Murzim, Beta is a blue-white Beta Cephei variable star of magnitude 2.0, which varies by a few hundredths of a magnitude over a period of six hours.[33] Mirzam is 500 light-years from Earth, and its traditional name means "the announcer", referring to its position as the "announcer" of Sirius, as it rises a few minutes before Sirius does.[6] Gamma, also known as Muliphein, is a fainter star of magnitude 4.12, in reality a blue-white bright giant of spectral type B8IIe located 441 light-years from earth.[34] Iota Canis Majoris, lying between Sirius and Gamma, is another star that has been classified as a Beta Cephei variable, varying from magnitude 4.36 to 4.40 over a period of 1.92 hours.[35] However it is a remote blue-white supergiant star of spectral type B3Ib, around 46,000 times as luminous as the sun and, at 2500 light-years distant, 300 times further away than Sirius.[36]

Epsilon, Omicron2, Delta and Eta Canis Majoris were called Al Adzari "the virgins" in medieval Arabic tradition.[37] Marking the dog's right thigh on Bayer's atlas is Epsilon Canis Majoris,[32] also known as Adhara. At magnitude 1.5, it is the second-brightest star in Canis Major and the 23rd-brightest star in the sky. It is a blue-white supergiant of spectral type B2Iab, around 404 light-years from Earth.[38] This star is one of the brightest known extreme ultraviolet sources in the sky.[39] It is a binary star; the secondary is of magnitude 7.4. Its traditional name means "the virgins", having been transferred from the group of stars to Epsilon alone.[40] Nearby is Delta Canis Majoris, also called Wezen. It is a yellow-white supergiant of spectral type F8Iab and magnitude 1.84, around 1605 light-years from Earth.[41] With a traditional name meaning "the weight", Wezen is 17 times as massive and 50,000 times as luminous as the Sun. If located in the centre of the Solar System, it would extend out to Earth as its diameter is 200 times that of the Sun. Only around 10 million years old, Wezen has stopped fusing hydrogen in its core. Its outer envelope is beginning to expand and cool, and in the next 100,000 years it will become a red supergiant as its core fuses heavier and heavier elements. Once it has a core of iron, it will collapse and explode as a supernova.[42] Nestled between Adhara and Wezen lies Sigma Canis Majoris, known as Unurgunite to the Boorong and Wotjobaluk people,[22] a red supergiant of spectral type K7Ib that varies irregularly between magnitudes 3.43 and 3.51.[43]

Also called Aludra, Eta Canis Majoris is a blue-white supergiant of spectral type B5Ia with a luminosity 176,000 times and diameter around 80 times that of the Sun.[44] Classified as an Alpha Cygni type variable star, Aludra varies in brightness from magnitude 2.38 to 2.48 over a period of 4.7 days.[45] It is located 1120 light-years away. To the west of Adhara lies 3.0-magnitude Zeta Canis Majoris or Furud, around 362 light-years distant from Earth.[46] It is a spectroscopic binary, whose components orbit each other every 1.85 years, the combined spectrum indicating a main star of spectral type B2.5V.[47]

Between these stars and Sirius lie Omicron1, Omicron2, and Pi Canis Majoris. Omicron2 is a massive supergiant star about 21 times as massive as the Sun.[48] Only 7 million years old,[48] it has exhausted the supply of hydrogen at its core and is now processing helium.[33] It has an Alpha Cygni variable that undergoes periodic non-radial pulsations, which cause its brightness to cycle from magnitude 2.93 to 3.08 over a 24.44-day interval.[49] Omicron1 is an orange K-type supergiant of spectral type K2.5Iab that is an irregular variable star, varying between apparent magnitudes 3.78 and 3.99.[50] Around 18 times as massive as the Sun, it shines with 65,000 times its luminosity.[51]

North of Sirius lie Theta and Mu Canis Majoris, Theta being the most northerly star with a Bayer designation in the constellation.[52] Around 8 billion years old, it is an orange giant of spectral type K4III that is around as massive as the Sun but has expanded to 30 times the Sun's diameter.[53] Mu is a multiple star system located around 1244 light-years distant,[54] its components discernible in a small telescope as a 5.3-magnitude yellow-hued and 7.1-magnitude bluish star.[55] The brighter star is a giant of spectral type K2III,[54] while the companion is a main sequence star of spectral type B9.5V.[56] Nu Canis Majoris is a yellow-hued giant star of magnitude 5.7, 278 light-years away; it is at the threshold of naked-eye visibility. It has a companion of magnitude 8.1.[6]

At the southern limits of the constellation lie Kappa and Lambda Canis Majoris. Although of similar spectra and nearby each other as viewed from Earth, they are unrelated.[25] Kappa is a Gamma Cassiopeiae variable of spectral type B2Vne,[57] which brightened by 50% between 1963 and 1978, from magnitude 3.96 or so to 3.52.[36] It is around 659 light-years distant.[58] Lambda is a blue-white B-type main sequence dwarf with an apparent magnitude of 4.48 located around 423 light-years from Earth.[59] It is 3.7 times as wide as and 5.5 times as massive as the Sun, and shines with 940 times its luminosity.[52]

Canis Major is also home to many variable stars. EZ Canis Majoris is a Wolf-Rayet star of spectral type WN4 that varies between magnitudes 6.71 and 6.95 over a period of 3.766 days; the cause of its variability is unknown but thought to be related to its stellar wind and rotation.[60] VY Canis Majoris is one of the largest stars known, a remote red supergiant located around 3800 light-years away from Earth. Estimates of its size, mass and luminosity have varied, with figures of 600 to 3000 times the radius, and 60,000 to 500,000 times the luminosity of the Sun. It was observed in 2011 using interferometry with the Very Large Telescope, yielding a radius of 1420 ± 120 solar radii, surface temperature of around 3490 K (and hence spectral type M4Ia) and a luminosity 270,000 times that of the Sun. Its current mass has been revised at 9–25 solar masses, having shed material from an initial 15–35 solar masses.[61] W Canis Majoris is a type of red giant known as a carbon star—a semiregular variable, it ranges between magnitudes 6.27 and 7.09 over a period of 160 days.[62] A cool star, it has a surface temperature of around 2900 K and a radius 234 times that of the Sun, its distance estimated at 1444–1450 light-years from Earth.[63] At the other extreme in size is RX J0720.4-3125, a neutron star with a radius of around 5 km.[64] Exceedingly faint, it has an apparent magnitude of 26.6.[65] Its spectrum and temperature appear to be mysteriously changing over several years. The nature of the changes are unclear, but it is possible they were caused by an event such as the star's absorption of an accretion disc.[64]

Tau Canis Majoris is a Beta Lyrae-type eclipsing multiple star system that varies from magnitude 4.32 to 4.37 over 1.28 days.[66] Its four main component stars are hot O-type stars, with a combined mass 80 times that of the Sun and shining with 500,000 times its luminosity, but little is known of their individual properties. A fifth component, a magnitude 10 star, lies 13,000 AU distant. The system is only 5 million years old.[33] UW Canis Majoris is another Beta Lyrae-type star 3000 light-years from Earth; it is an eclipsing binary that ranges in magnitude from a minimum of 5.3 to a maximum of 4.8. It has a period of 4.4 days;[6] its components are two massive hot blue stars, one a blue supergiant of spectral type O7.5-8 Iab, while its companion is a slightly cooler, less evolved and less luminous supergiant of spectral type O9.7Ib. The stars are 200,000 and 63,000 times as luminous as the Sun. However the fainter star is the more massive at 19 solar masses to the primary's 16.[67] R Canis Majoris is another eclipsing binary that varies from magnitude 5.7 to 6.34 over 1.13 days,[68] with a third star orbiting these two every 93 years. The shortness of the orbital period and the low ratio between the two main components make this an unusual Algol-type system.[69]

Seven star systems have been found to have planets. Nu2 Canis Majoris is an ageing orange giant of spectral type K1III of apparent magnitude 3.91 located around 64 light-years distant.[70] Around 1.5 times as massive and 11 times as luminous as the Sun, it is orbited over a period of 763 days by a planet 2.6 times as massive as Jupiter.[71] HD 47536 is likewise an ageing orange giant found to have a planetary system—echoing the fate of our own Solar System in a few billion years as the Sun ages and becomes a giant.[72] Conversely, HD 45364 is a star 107 light-years distant that is a little smaller and cooler than the Sun, of spectral type G8V, which has two planets discovered in 2008. With orbital periods of 228 and 342 days, the planets have a 3:2 orbital resonance, which helps stabilise the system.[73] HD 47186 is another sunlike star with two planets; the inner—HD 47186 b—takes four days to complete an orbit and has been classified as a Hot Neptune, while the outer—HD 47186 c—has an eccentric 3.7-year period orbit and has a similar mass to Saturn.[74] HD 43197 is a sunlike star around 183 light-years distant that has a Jupiter-size planet with an eccentric orbit.[75]

Z Canis Majoris is a star system a mere 300,000 years old composed of two pre-main-sequence stars—a FU Orionis star and a Herbig Ae/Be star,[76] which has brightened episodically by two magnitudes to magnitude 8 in 1987, 2000, 2004 and 2008.[77] The more massive Herbig Ae/Be star is enveloped in an irregular roughly spherical cocoon of dust that has an inner diameter of 20 and outer diameter of 50 AU. The cocoon has a hole in it through which light shines that covers an angle of 5 to 10 degrees of its circumference. Both stars are surrounded by a large envelope of in-falling material left over from the original cloud that formed the system. Both stars are emitting jets of material, that of the Herbig Ae/Be star being much larger—11.7 light-years (3.6 parsecs) long.[78] Meanwhile, FS Canis Majoris is another star with infra-red emissions indicating a compact shell of dust, however it appears to be a main-sequence star that has absorbed material from a companion. These stars are thought to be significant contributors to interstellar dust.[79]

Deep-sky objects

The band of the Milky Way goes through Canis Major, with only patchy obscurement by interstellar dust clouds. It is bright in the northeastern corner of the constellation, as well as in a triangular area between Adhara, Wezen and Aludra, with many stars visible in binoculars. Canis Major boasts several open clusters.[80] The only Messier object is M41 (NGC 2287), an open cluster with a combined visual magnitude of 4.5, around 2300 light-years from Earth. Located 4 degrees south of Sirius, it contains contrasting blue, yellow and orange stars and covers an area the apparent size of the full Moon—in reality around 25 light-years in diameter.[81] Its most luminous stars have already evolved into giants. The brightest is a 6.3-magnitude star of spectral type K3. Located in the field is 12 Canis Majoris, though this star is only 670 light-years distant.[82] NGC 2360, known as Caroline's Cluster after its discoverer Caroline Herschel, is an open cluster located 3.5 degrees west of Muliphein and has a combined apparent magnitude of 7.2. Around 15 light-years in diameter, it is located 3700 light-years away from Earth,[83] and has been dated to around 2.2 billion years old.[84] NGC 2362 is a small, compact open cluster, 5200 light-years from Earth. It contains about 60 stars, of which Tau Canis Majoris is the brightest member.[6] Located around 3 degrees northeast of Wezen, it covers an area around 12 light-years in diameter, though the stars appear huddled around Tau when seen through binoculars. It is a very young open cluster as its member stars are only a few million years old. Lying 2 degrees southwest of NGC 2362 is NGC 2354 a fainter open cluster of magnitude 6.5, with around 15 member stars visible with binoculars.[81] Located around 30' northeast of NGC 2360,[85] NGC 2359 (Thor's Helmet or the Duck Nebula) is a relatively bright emission nebula in Canis Major, with an approximate magnitude of 10, which is 10,000 light-years from Earth. The nebula is shaped by HD 56925, an unstable Wolf-Rayet star embedded within it.[86]


In 2003, an overdensity of stars in the region was announced to be the Canis Major Dwarf, the closest satellite galaxy to Earth. However, there remains debate over whether it represents a disrupted dwarf galaxy or in fact a variation in the thin and thick disk and spiral arm populations of the Milky Way. Investigation of the area yielded only ten RR Lyrae variables—consistent with the Milky Way's halo and thick disk populations rather than a separate dwarf spheroidal galaxy.[88] On the other hand, a globular cluster in Puppis, NGC 2298—which appears to be part of the Canis Major dwarf system—is extremely metal-poor, suggesting it did not arise from the Milky Way's thick disk, and instead is of extragalactic origin.[89]

[87] ESO 489-056 is an irregular dwarf- and Low-surface-brightness galaxy that has one of the lowest metallicities known.[95]


  1. ^ a b c "Canis Major, Constellation Boundary". The Constellations (International Astronomical Union). Retrieved 15 November 2012. 
  2. ^ Rogers, John H. (1998). "Origins of the Ancient Constellations: I. The Mesopotamian traditions". Journal of the British Astronomical Association 108 (1): 9–28.  
  3. ^ a b Wagman 2003, p. 71.
  4. ^ Rogers, John H. (1998). "Origins of the Ancient Constellations: II. The Mediterranean Traditions". Journal of the British Astronomical Association 108 (2): 79–89.  
  5. ^ a b c d Allen 1963, p. 117.
  6. ^ a b c d e f g Ridpath & Tirion 2001, pp. 98–99.
  7. ^ Allen 1963, p. 118.
  8. ^ Oxby, Claire (October 1999). "A Review of African Ethno-Astronomy: With Particular Reference to Saharan Livestock-Keepers". La Ricerca Folklorica (40): 57–58.  
  9. ^ Schlegel 1967, p. 428.
  10. ^ Schlegel 1967, p. 430.
  11. ^ a b Ridpath, Ian. "Canis Major – the Greater Dog". Star Tales. self-published. Retrieved 1 March 2014. 
  12. ^ Schlegel 1967, p. 431.
  13. ^ Schlegel 1967, p. 434.
  14. ^ Makemson 1941, p. 212.
  15. ^ Makemson 1941, p. 215.
  16. ^ Makemson 1941, p. 258.
  17. ^ Makemson 1941, p. 247.
  18. ^ Makemson 1941, p. 249.
  19. ^ Makemson 1941, p. 254.
  20. ^ Makemson 1941, p. 236.
  21. ^ Ridley, William (1875). Kámilarói, and other Australian languages (2nd ed.). Sydney, New South Wales: T. Richards, government printer. pp. 144–45. 
  22. ^ a b Hamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae". Journal of Astronomical History & Heritage 13 (3): 220–34.  
  23. ^ Smyth, Robert Brough (1878). The Aborigines of Victoria: with Notes Relating to the Habits of the Natives of other Parts of Australia and Tasmania. Melbourne, Victoria: J. Ferres, government printer. pp. 433–34. 
  24. ^ Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy 30: 469–71.  
  25. ^ a b Bagnall, Philip M. (2012). The Star Atlas Companion: What You Need to Know about the Constellations. New York, New York: Springer. pp. 99–106.  
  26. ^ Tomkin, Jocelyn (April 1998). "Once and Future Celestial Kings". Sky and Telescope 95 (4): 59–63.  
  27. ^ a b Wagman 2003, p. 73.
  28. ^ a b Wagman 2003, p. 74.
  29. ^ Wagman 2003, p. 368.
  30. ^ Wagman 2003, pp. 73-74.
  31. ^ Holberg, J.B. (2007). Sirius: Brightest Diamond in the Night Sky. Chichester, United Kingdom: Praxis Publishing. p. 214.  
  32. ^ a b Wagman 2003, p. 504.
  33. ^ a b c Kaler, James B. (4 May 2007). "Mirzam". Stars. University of Illinois. Retrieved 2 January 2012. 
  34. ^ "Gamma Canis Majoris - Star in Cluster". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 16 February 2014. 
  35. ^ Watson, Christopher (4 January 2010). "Iota Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 2 March 2014. 
  36. ^ a b Kaler, James B. (26 February 2010). "Iota Canis Majoris". Stars. University of Illinois. Retrieved 2 March 2014. 
  37. ^ Knobel, Edward B. (1895). "Al Achsasi Al Mouakket, on a Catalogue of Stars in the Calendarium of".  
  38. ^ "Epsilon Canis Majoris - Double Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 16 February 2014. 
  39. ^ Wilkinson, E.; Green, J.C.; McLean, R.; Welsh, B.; Green; McLean; Welsh (1996). "Extreme Ultraviolet Spectrum of ɛ Canis Majoris Between 600-920 Å". Bull. American Astron. Soc. 28 (2): 915.  
  40. ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts:  
  41. ^ "Delta Canis Majoris – Variable Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 16 February 2014. 
  42. ^ Kaler, James B. "Wezen". Stars website. University of Illinois. Retrieved 17 February 2014. 
  43. ^ Watson, Christopher (4 January 2010). "Sigma Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 24 February 2014. 
  44. ^ Jerzykiewicz, M.; Molenda-Zakowicz, J.; Molenda-Zakowicz (2000). "Empirical Luminosities and Radii of Early-Type Stars after Hipparcos". Acta Astronomica 50: 369–80.  
  45. ^ Watson, Christopher (3 May 2013). "Eta Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 February 2014. 
  46. ^ "Zeta Canis Majoris - Cepheid Variable". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 17 February 2014. 
  47. ^ Kaler, James B. (2 February 2007). "Furud". Stars website. University of Illinois. Retrieved 17 February 2014. 
  48. ^ a b Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011). "A Catalogue of Young Runaway Hipparcos Stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200.  
  49. ^ Lefèvre, L.; Marchenko, S. V.; Moffat, A. F. J.; Acker, A. (November 2009). "A systematic study of variability among OB-stars based on HIPPARCOS photometry". Astronomy and Astrophysics 507 (2): 1141–1201.  
  50. ^ Watson, Christopher (4 January 2010). "Omicron1 Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 15 February 2014. 
  51. ^ Kaler, James B. "Omicron1 Canis Majoris". Stars. University of Illinois. Retrieved 24 February 2014. 
  52. ^ a b Kaler, James B. (8 March 2013). "Theta Canis Majoris". Stars website. University of Illinois. Retrieved 18 February 2014. 
  53. ^ da Silva, L.; Girardi, L.; Pasquini, L.; Setiawan, J.; von der Lühe, O.; de Medeiros, J.R.; Hatzes, A.; Döllinger, M.P.; Weiss, A. (2006). "Basic Physical Parameters of a Selected Sample of Evolved Stars". Astronomy and Astrophysics 458 (2): 609–23.  
  54. ^ a b "18 Canis Majoris". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 18 February 2014. 
  55. ^ Consolmagno, Guy (2011). Turn Left at Orion: Hundreds of Night Sky Objects to See in a Home Telescope – and How to Find Them. Cambridge, United Kingdom: Cambridge University Press. p. 81.  
  56. ^ "HD 51251 -- Star in double system". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 18 February 2014. 
  57. ^ Watson, Christopher (4 January 2010). "Kappa Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 24 February 2014. 
  58. ^ "Kappa Canis Majoris - Be Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 2 March 2014. 
  59. ^ "Lambda Canis Majoris - Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 2 March 2014. 
  60. ^ The IUE Mega Campaign: Wind Structure and Variability of HD 50896 (WN5) Astrophysical Journal Letters 452 #1, pp. L57 (October 1995) Bibcode: 1995ApJ...452L..57S
  61. ^ Wittkowski, M.; Hauschildt, P.H.; Arroyo-Torres, B.; Marcaide, J.M. (2012). "Fundamental Properties and Atmospheric Structure of the Red Supergiant VY CMa based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics 540: L12.  
  62. ^ Otero, Sebastian Alberto (7 November 2011). "W Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 12 March 2014. 
  63. ^ van Belle, Gerard T.; Paladini, Claudia; Aringer, Bernhard; Hron, Josef; Ciardi, David (2013). "The PTI Carbon Star Angular Size Survey: Effective Temperatures and Non-sphericity". The Astrophysical Journal 775 (1): article id. 45, 19 pp.  
  64. ^ a b Hohle, M.M.; Haberl, F.; Vink, J.; de Vries, C.P.; Turolla, R.; Zane, S.; Méndez, M. "The Continued Spectral and Temporal Evolution of RX J0720.4-3125". Monthly Notices of the Royal Astronomical Society 423 (2): 1194–99.  
  65. ^ Kaplan, D.L.; van Kerkwijk, M.H.; Marshall, H.L.; Jacoby, B.A.; Kulkarni, S. R.; Frail, D.A. (2002). "The Nearby Neutron Star RX J0720.4-3125 from Radio to X-rays". The Astrophysical Journal 590 (2): 1008.  
  66. ^ Watson, Christopher (4 January 2010). "Tau Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 21 March 2014. 
  67. ^ Bagnuolo, William G. , Jr.; Gies, Douglas R.; Hahula, Michael E.; Wiemker, Rafael; Wiggs, Michael S. (1994). "Tomographic Separation of Composite Spectra. 2: The Components of 29 UW Canis Majoris". The Astrophysical Journal 423: 446–55.  
  68. ^ Watson, Christopher (4 January 2010). "R Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 18 February 2014. 
  69. ^ Budding, E.; Butland, R. (2011). "Observations and Analysis of the System R Canis Majoris". Monthly Notices of the Royal Astronomical Society 418 (3): 1764–73. Bibcode:2011MNRAS.418.1764B. doi:10.1111/j.1365-2966.2011.19597.x. 
  70. ^ "7 Canis Majoris - Variable Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 26 February 2014. 
  71. ^ Wittenmyer; Endl, Michael; Wang, Liang; Johnson, John Asher; Tinney, C.G.; O'Toole, S.J. (2011). "The Pan-Pacific Planet Search. I. A Giant Planet Orbiting 7 CMa". The  
  72. ^ "Distant World in Peril Discovered from La Silla: Giant Exoplanet Orbits Giant Star". ESO for the Public (Press release). Garching, Germany:  
  73. ^ Correia, A. C. M.; Udry, S.; Mayor, M.; Benz, W.; Bertaux, J.-L.; Bouchy, F.; Laskar, J.; Lovis, C.; Mordasini, C.; Pepe, F.; Queloz, D. (2009). "The HARPS Search for Southern Extra-solar Planets XVI. HD 45364, a Pair of Planets in a 3:2 Mean Motion Resonance". Astronomy and Astrophysics 496 (2): 521–26.  
  74. ^ Bouchy, F.; Mayor, M.; Lovis, C.; Udry, S.; Benz, W.; Bertaux, J.-L.; Delfosse, X.; Mordasini, C.; Pepe, F. (2009). "The HARPS Search for Southern Extra-solar Planets. XVII. Super-Earth and Neptune-mass Planets in Multiple Planet Systems HD 47186 and HD 181433". Astronomy and Astrophysics 496 (2): 527–31.  
  75. ^ Naef, D.; Mayor, M.; Curto, G. Lo; Bouchy, F.; Lovis, C.; Moutou, C.; Benz, W.; Pepe, F.; Queloz, D. (2010). "The HARPS Search for Southern Extrasolar Planets XXIII. 8 Planetary Companions to Low-activity Solar-type Stars". Astronomy and Astrophysics 523. A15.  
  76. ^ Szeifert, T.; Hubrig, S.; Schöller, M.; Schütz, O.; Stelzer, B.; Mikulášek, Z. (2010). "The Nature of the Recent Extreme Outburst of the Herbig Be/FU Orionis Binary Z Canis Majoris". Astronomy and Astrophysics 509: L7.  
  77. ^ Whelan, E.T.; Dougados, C.; Perrin, M. D.; Bonnefoy, M.; Bains, I.; Redman, M.P.; Ray, T.P.; Bouy, H.; Benisty, M.; Bouvier, J.; Chauvin, G.; Garcia, P.J.V.; Grankvin, K.; Malbet, F. (2010). "The 2008 Outburst in the Young Stellar System Z CMa: The First Detection of Twin Jets". The Astrophysical Journal Letters 720 (1): L119–24.  
  78. ^ Canovas, H.; Min, M.; Jeffers, S.V.; Rodenhuis, M.; Keller, C.U. (2012). "Constraining the Circumbinary envelope of Z Canis Majoris via Imaging Polarimetry". Astronomy & Astrophysics 543 (A70): 8 pp.  
  79. ^ Miroshnichenko, Anatoly S. (2007). "Toward Understanding the B[e] Phenomenon. I. Definition of the Galactic FS CMa Stars". The Astrophysical Journal 667 (1): 497–504.  
  80. ^ Crossen, Craig; Rhemann, Gerald (2004). Sky Vistas: Astronomy for Binoculars and Richest-Field Telescopes. New York, New York: Springer. pp. 113–15.  
  81. ^ a b Kambic, Bojan (2009). Viewing the Constellations with Binoculars: 250+ Wonderful Sky Objects to See and Explore. New York, New York: Springer. pp. 230–32.  
  82. ^ De Laet, Rony (2011). The Casual Sky Observer's Guide: Stargazing with Binoculars and Small Telescopes. New York, New York: Springer. pp. 95–97.  
  83. ^ O'Meara, Stephen James (2002). The Caldwell Objects. Cambridge, United Kingdom: Cambridge University Press. pp. 231–33.  
  84. ^ Mermilliod, Jean-Claude; Mayor, Michel (1990). "Red Giants in Open Clusters. III - Binarity and Stellar Evolution in Five Intermediate-age Clusters: NGC 2360, 2423, 5822, 6811, and IC 4756". Astronomy and Astrophysics 273 (1): 61–72.  
  85. ^ Thompson, Robert and Barbara (2007). Illustrated Guide to Astronomical Wonders: From Novice to Master Observer. Sebastopol, California: O'Reilly Media, Inc. p. 144.  
  86. ^ Levy, David H. (2005). Deep Sky Objects. Amherst, New York: Prometheus Books. p. 108.  
  87. ^ a b "Stars Fleeing a Cosmic Crash". ESA/Hubble Picture of the Week. Retrieved 14 August 2013. 
  88. ^ Mateu, Cecilia; Vivas, A. Katherina; Zinn, Robert; Miller, Lissa R.; Abad, Carlos; Vivas; Zinn; Miller; Abad (2009). "No Excess of RR Lyrae Stars in the Canis Major Overdensity". The Astronomical Journal 37 (5): 4412–23.  
  89. ^ O'Meara, Stephen James (2011). Deep-Sky Companions: The Secret Deep. Cambridge, United Kingdom: Cambridge University Press. p. 139.  
  90. ^ Wilkins & Dunn 2006, p. 456.
  91. ^ Kirshner, Robert P.; Arp, H.C.; Dunlap, J.R.; Arp; Dunlap (1976). "Observations of Supernovae - 1975a in NGC 2207 and 1975b in the Perseus Cluster". Astrophysical Journal 207 (1): 44–52.  
  92. ^ Jha, S.; Garnavich, P.; Challis, P.; Kirshner, R.; Berlind, P.; Garnavich, P.; Challis, P.; Kirshner, R.; Berlind, P. (1999). "Supernova 1999ec in NGC 2207". IAUC 7269: 2.  
  93. ^ Bishop, David. "Bright Supernovae - 2003". Rochester University. Retrieved 7 March 2014. 
  94. ^ Conseil, E.; Fraser, M.; Inserra, C.; Walton, N.; Blagorodnova, N.; Nicholl, M.; Benetti, S.; Pastorello, A.; Valenti, S.; Taubenberger, S.; Smartt, S. J.; Smith, K.; Young, D.; Sullivan, M.; Gal-Yam, A.; Yaron, O. (2013). "Supernova 2013ai in NGC 2207 = Psn J06161835-2122329". Central Bureau Electronic Telegrams 3431 (3431): 1.  
  95. ^ Kunth, Daniel; Östlin, Goran (2000). "The Most Metal-poor Galaxies". The Astronomy and Astrophysics Review 10 (1–2): 1–79.  

Cited texts

  • Allen, Richard Hinckley (1963) [1899]. Star Names: Their Lore and Meaning. New York, New York: Dover.  
  • Makemson, Maud Worcester (1941). The Morning Star Rises: An Account of Polynesian Astronomy. New Haven, Connecticut: Yale University Press. 
  • Ridpath, Ian; Tirion, Wil (2001). Stars and Planets Guide. Princeton, New Jersey: Princeton University Press.  
  • Schlegel, Gustaaf (1967) [1875]. Uranographie Chinoise (in French). Taipei, Republic of China: Ch'eng Wen Publishing Company. 
  • Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, Virginia: The McDonald & Woodward Publishing Company.  
  • Wilkins, Jamie; Dunn, Robert (2006). 300 Astronomical Objects: A Visual Reference to the Universe. Buffalo, New York: Firefly Books.  

External links

  • The Deep Photographic Guide to the Constellations: Canis Major