Phoenix (constellation)

Phoenix
Constellation

Abbreviation Phe
Genitive Phoenicis
Pronunciation
  • /ˈfiːnɪks/
  • genitive /fᵻˈnaɪsᵻs/
Symbolism the Phoenix
Right ascension 23h 26.5m to 02h 25.0m[1]
Declination −39.31° to −57.84°[1]
Family Bayer
Quadrant SQ1
Area 469 sq. deg. (37th)
Main stars 4
Bayer/Flamsteed
stars		 25
Stars with planets 10
Stars brighter than 3.00m 1
Stars within 10.00 pc (32.62 ly) 1
Brightest star α Phe (Ankaa) (2.40m)
Nearest star Gliese 915
(27.24 ly, 8.35 pc)
Messier objects 0
Meteor showers Phoenicids
Bordering
constellations
Visible at latitudes between +32° and −80°.
Best visible at 21:00 (9 p.m.) during the month of November.

Phoenix is a minor constellation in the southern sky. Named after the mythical phoenix, it was first depicted on a celestial atlas by Johann Bayer in his 1603 Uranometria. The French explorer and astronomer Nicolas Louis de Lacaille charted the brighter stars and gave their Bayer designations in 1756. The constellation stretches from roughly −39° to −57° declination, and from 23.5h to 2.5h of right ascension. The constellations Phoenix, Grus, Pavo and Tucana, are known as the Southern Birds.

The brightest star, Alpha Phoenicis, is named Ankaa, an Arabic word meaning 'the Phoenix'. It is an orange giant of apparent magnitude 2.4. Next is Beta Phoenicis, actually a binary system composed of two yellow giants with a combined apparent magnitude of 3.3. Nu Phoenicis has a dust disk, while the constellation has ten star systems with known planets and the recently discovered galaxy clusters El Gordo and the Phoenix Cluster—located 7.2 and 5.7 billion light years away respectively, two of the largest objects in the visible universe. Phoenix is the radiant of two annual meteor showers: the Phoenicids in December, and the July Phoenicids.

History

The constellation Phoenix as depicted in Johann Gabriel Doppelmayr's Atlas Coelestis, ca. 1742.
The "southern birds", as depicted in Johann Bayer's Uranometria. Phoenix is on the lower left.

Phoenix was the largest of the twelve constellations established by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman. It first appeared on a 35-cm diameter celestial globe published in 1597 (or 1598) in Amsterdam by Plancius with Jodocus Hondius. The first depiction of this constellation in a celestial atlas was in Johann Bayer's Uranometria of 1603.[2] De Houtman included it in his southern star catalog the same year under the Dutch name Den voghel Fenicx, "The Bird Phoenix",[3] symbolising the phoenix of classical mythology.[4] One name of the brightest star Alpha Phoenicis—Ankaa—is derived from the Arabic العنقاء al-‘anqā’ "the phoenix", and was coined sometime after 1800 in relation to the constellation.[5]

Celestial historian Richard Allen noted that unlike the other constellations introduced by Plancius and La Caille, Phoenix has actual precedent in ancient astronomy, as the Arabs saw this formation as representing young ostriches, Al Ri'āl, or as a griffin or eagle.[6] In addition, the same group of stars was sometimes imagined by the Arabs as a boat, Al Zaurak, on the nearby river Eridanus.[7] He observed, "the introduction of a Phoenix into modern astronomy was, in a measure, by adoption rather than by invention."[6]

The Chinese incorporated Phoenix's brightest star, Ankaa (Alpha Phoenicis), and stars from the adjacent constellation Sculptor to depict Bakui, a net for catching birds.[4] Phoenix and the neighbouring constellation of Grus together were seen by Julius Schiller as portraying Aaron the High Priest.[6] These two constellations, along with nearby Pavo and Tucana, are called the Southern Birds.[8]

Characteristics

Phoenix is a small constellation bordered by Fornax and Sculptor to the north, Grus to the west, Tucana to the south, touching on the corner of Hydrus to the south, and Eridanus to the east and southeast. The bright star Achernar is nearby.[9] The three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is 'Phe'.[10] The official constellation boundaries, as set by Eugène Delporte in 1930, are defined by a polygon of 10 segments. In the equatorial coordinate system, the right ascension coordinates of these borders lie between 23h 26.5m and 02h 25.0m, while the declination coordinates are between −39.31° and −57.84°.[1] This means it remains below the horizon to anyone living north of the 40th parallel in the Northern Hemisphere, and remains low in the sky for anyone living north of the equator. It is most visible from locations such as Australia and South Africa during late Southern Hemisphere spring.[7] Most of the constellation lies within, and can be located by, forming a triangle of the bright stars Achernar, Fomalhaut and Beta Ceti—Ankaa lies roughly in the centre of this.[11]

Features

The constellation Phoenix as it can be seen by the naked eye.

Stars

Further information: List of stars in Phoenix

A curved line of stars comprising Alpha, Kappa, Mu, Beta, Nu and Gamma Phoenicis was seen as a boat by the ancient Arabs.[6] French explorer and astronomer Nicolas Louis de Lacaille charted and designated 27 stars with the Bayer designations Alpha through to Omega in 1756. Of these, he labelled two stars close together Lambda, and assigned Omicron, Psi and Omega to three stars, which subsequent astronomers such as Benjamin Gould felt were too dim to warrant their letters. A different star was subsequently labelled Psi Phoenicis, while the other two designations fell out of use.[12]

Ankaa is the brightest star in the constellation. It is an orange giant of apparent visual magnitude 2.37 and spectral type K0.5IIIb,[13] 77 light years distant from Earth and orbited by a secondary object about which little is known.[14] Lying close by Ankaa is Kappa Phoenicis, a main sequence star of spectral type A5IVn and apparent magnitude 3.90.[15] Located centrally in the asterism,[7] Beta Phoenicis is the second brightest star in the constellation and another binary star. Together the stars, both yellow giants of spectral type G8, shine with an apparent magnitude of 3.31, though the components are of individual apparent magnitudes of 4.0 and 4.1 and orbit each other every 168 years.[16] Zeta Phoenicis is an Algol-type eclipsing binary, with an apparent magnitude fluctuating between 3.9 and 4.4 with a period of around 1.7 days (40 hours); its dimming results from the component two blue-white B-type stars, which orbit and block out each other from Earth. The two stars are 0.05 AU from each other, while a third star is around 600 AU away from the pair, and has an orbital period exceeding 5000 years.[17] The system is around 300 light years distant.[18] In 1976, researchers Clausen, Gyldenkerne, and Grønbech calculated that a nearby 8th magnitude star is a fourth member of the system.[19]

Gamma Phoenicis is a red giant of spectral type M0IIIa[20] and varies between magnitudes 3.39 and 3.49. It lies 235 light years away.[21] Psi Phoenicis is another red giant, this time of spectral type M4III,[22] and has an apparent magnitude that ranges between 4.3 and 4.5 over a period of around 30 days.[23] Lying 340 light years away,[22] it has around 85 times the diameter, but only 85% of the mass, of our sun.[24] W Phoenicis is a Mira variable, ranging from magnitude 8.1 to 14.4 over 333.95 days. A red giant, its spectrum ranges between M5e and M6e.[25] Located 6.5 degrees west of Ankaa is SX Phoenicis, a variable star which ranges from magnitude 7.1 to 7.5 over a period of a mere 79 minutes. Its spectral type varies between A2 and F4.[26] It gives its name to a group of stars known as SX Phoenicis variables.[27] Rho and BD Phoenicis are Delta Scuti variables—short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study astroseismology.[28] Rho is spectral type F2III,[29] and ranges between magnitudes 5.20 and 5.26 over a period of 2.85 hours.[30] BD is of spectral type A1V,[31] and ranges between magnitudes 5.90 and 5.94.[32]

Nu Phoenicis is a yellow-white main sequence star of spectral type F9V and magnitude 4.96.[33] Lying some 49 light years distant, it is around 1.2 times as massive as our sun,[34] and likely to be surrounded by a disk of dust.[35] It is the closest star in the constellation that is visible with the unaided eye.[23] Gliese 915 is a white dwarf only 26 light years away. It is of magnitude 13.05, too faint to be seen with the naked eye.[36] White dwarfs are extremely dense stars compacted into a volume the size of the Earth.[37] With around 85% of the mass of the Sun, Gliese 915 has a surface gravity of 108.39 ± 0.01 (2.45 · 108) cm·s−2, or approximately 250,000 of Earth's.[38]

Ten stars have been found to have planets to date, and four planetary systems have been discovered with the SuperWASP project. HD 142 is a yellow giant that has an apparent magnitude of 5.7, and has a planet (HD 142 b)1.36 times the mass of Jupiter which orbits every 328 days.[39] HD 2039 is a yellow subgiant with an apparent magnitude of 9.0 around 330 light years away which has a planet (HD 2039 b) triple the mass of Jupiter. WASP-18 is a star of magnitude 9.29 which was discovered to have a hot Jupiter-like planet (WASP-18b) taking less than a day to orbit the star.[40] The planet is suspected to be causing WASP-18 to appear older than it really is.[41] WASP-4 and WASP-5 are solar-type yellow stars around 1000 light years distant and of 13th magnitude, each with a single planet larger than Jupiter.[42] WASP-29 is an orange dwarf of spectral type K4V and visual magnitude 11.3, which has a planetary companion of similar size and mass to Saturn. The planet completes an orbit every 3.9 days.[43]

WISE J003231.09-494651.4 and WISE J001505.87-461517.6 are two brown dwarfs discovered by the Wide-field Infrared Survey Explorer, and are 63 and 49 light years away respectively.[44] Initially hypothesised before they were belatedly discovered,[45] brown dwarfs are objects more massive than planets, but which are of insufficient mass for hydrogen fusion characteristic of stars to occur. Many are being found by sky surveys.[46]

Phoenix contains HE0107-5240, possibly one of the oldest stars yet discovered. It has around 1/200,000 the metallicity that the Sun has and hence must have formed very early in the history of the universe.[47] With a visual magnitude of 15.17,[48] it is around 10,000 times dimmer than the faintest stars visible to the naked eye and is 36000 light years distant.[47]

Deep-sky objects

The constellation does not lie on the galactic plane of the Milky Way, and there are no prominent star clusters.[9] NGC 625 is a dwarf irregular galaxy of apparent magnitude 11.0 and lying some 12.7 million light years distant. Only 24000 light years in diameter, it is an outlying member of the Sculptor Group. NGC 625 is thought to have been involved in a collision and is experiencing a burst of active star formation.[49] NGC 37 is a lenticular galaxy of apparent magnitude 14.66. It is approximately 42 kiloparsecs (137,000 light-years) in diameter and about 12.9 billion years old.[50] Robert's Quartet (composed of the irregular galaxy NGC 87, and three spiral galaxies NGC 88, NGC 89 and NGC 92) is a group of four galaxies located around 160 million light-years away which are in the process of colliding and merging. They are within a circle of radius of 1.6 arcmin, corresponding to about 75,000 light-years.[51] Located in the galaxy ESO 243-49 is HLX-1, an intermediate-mass black hole—the first one of its kind identified. It is thought to be a remnant of a dwarf galaxy that was absorbed in a collision with ESO 243-49.[52] Before its discovery, this class of black hole was only hypothesized.[53]

Lying within the bounds of the constellation is the gigantic Phoenix cluster, which is around 7.3 million light years wide and 5.7 billion light years away, making it one of the most massive galaxy clusters. It was first discovered in 2010, and the central galaxy is producing an estimated 740 new stars a year.[54] Larger still is El Gordo, or officially ACT-CL J0102-4915, whose discovery was announced in 2012.[55] Located around 7.2 billion light years away, it is composed of two subclusters in the process of colliding, resulting in the spewing out of hot gas, seen in X-rays and infrared images.[56]

Meteor showers

Phoenix is the radiant of two annual meteor showers. The Phoenicids, also known as the December Phoenicids, were first observed on 3 December 1887. The shower was particularly intense in December 1956, and is thought related to the breakup of the short-period comet 289P/Blanpain. It peaks around 4–5 December, though is not seen every year.[57] A very minor meteor shower peaks around July 14 with around one meteor an hour, though meteors can be seen anytime from July 3 to 18; this shower is referred to as the July Phoenicids.[58]

References

  1. 1 2 3 "Phoenix, constellation boundary". The Constellations. International Astronomical Union. Retrieved 23 August 2012.
  2. ↑ Ridpath, Ian The South Will Rise Again!. "Bayer's Southern Star Chart". self-published. Retrieved August 15, 2013.
  3. ↑ Ridpath, Ian. "Frederick de Houtman's catalogue". self-published. Retrieved August 15, 2013.
  4. 1 2 Ridpath, Ian. "Phoenix – the Phoenix". self-published. Retrieved August 18, 2013.
  5. ↑ Kunitsch, Paul; Smart, Tim (2006). A Dictionary of Modern Star names: A Short Guide to 254 Star Names and Their Derivations. Cambridge, Massachusetts: Sky Publishing Corp. p. 49. ISBN 978-1-931559-44-7.
  6. 1 2 3 4 Allen, Richard Hinckley (1963) [1899]. Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. pp. 335–36. ISBN 0-486-21079-0.
  7. 1 2 3 Motz, Lloyd; Nathanson, Carol (1991). The Constellations: An Enthusiast's Guide to the Night Sky. London, United Kingdom: Aurum Press. pp. 371–72. ISBN 1-85410-088-2.
  8. ↑ Moore, Patrick (2000). Exploring the Night Sky with Binoculars. Cambridge, United Kingdom: Cambridge University Press. p. 48. ISBN 0521793904.
  9. 1 2 Klepešta, Josef; Rükl, Antonín (1974) [1969]. Constellations. Hamlyn. pp. 214–15. ISBN 0-600-00893-2.
  10. ↑ Russell, Henry Norris (1922). "The new international symbols for the constellations". Popular Astronomy. 30: 469–71. Bibcode:1922PA.....30..469R.
  11. ↑ Heifetz, Milton; Tirion, Wil (2007). A Walk Through the Southern Sky: A Guide to Stars and Constellations and Their Legends. Cambridge, United Kingdom: Cambridge University Press. pp. 30–31. ISBN 1139461389.
  12. ↑ 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, VA: The McDonald & Woodward Publishing Company. pp. 203–04. ISBN 978-0-939923-78-6.
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  14. ↑ Kaler, Jim. "Ankaa". Stars. University of Illinois. Retrieved 24 August 2012.
  15. ↑ "Kappa Phoenicis". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 25 August 2012.
  16. ↑ Kaler, Jim. "Beta Phoenicis". Stars. University of Illinois. Retrieved 24 August 2012.
  17. ↑ Kaler, Jim. "Zeta Phoenicis". Stars. University of Illinois. Retrieved 18 June 2013.
  18. ↑ "Zeta Phoenicis – Eclipsing binary of Algol type (detached)". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 4 September 2013.
  19. ↑ Grønbech, K.; Gyldenkerne, K.; Grønbech, B. (1976). "Four-color photometry of eclipsing binaries. IIIb: Zeta Phoenicis, analysis of light curves and determination of absolute dimensions". Astronomy and Astrophysics. 46: 205–12. Bibcode:1976A&A....46..205C.
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  22. 1 2 "Psi Phoenicis – Semi-regular pulsating Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 12 May 2013.
  23. 1 2 Bagnall, Philip M. (2012). The Star Atlas Companion: What You Need to Know about the Constellations. New York, New York: Springer. pp. 359–61. ISBN 1-4614-0830-X.
  24. ↑ Neilson, Hilding R.; Lester, John B. (2008). "Determining parameters of cool giant stars by modeling spectrophotometric and interferometric observations using the SAtlas program". Astronomy and Astrophysics. 490 (2): 807–10. arXiv:0809.1875Freely accessible. Bibcode:2008A&A...490..807N. doi:10.1051/0004-6361:200810627.
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  26. ↑ Burnham, Robert Jr. (1978). Burnham's Celestial Handbook. III. New York, New York: Dover. pp. 1455–57. ISBN 0-486-24065-7.
  27. ↑ Landes, H.; Bambery, K. R.; Coates, D. W.; Thompson, K. (2007). "Long-Term Changes in the Periods of SX Phe" (PDF). Publications of the Astronomical Society of Australia. 24: 41–45. Bibcode:2007PASA...24...41L. doi:10.1071/AS06025.
  28. ↑ Templeton, Matthew (16 July 2010). "Delta Scuti and the Delta Scuti Variables". Variable Star of the Season. AAVSO (American Association of Variable Star Observers). Retrieved 19 June 2013.
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  30. ↑ "Rho Phe". International Variable Star Index. AAVSO. 4 January 2010. Retrieved 18 June 2013.
  31. ↑ "V* BD Phe – Variable Star of delta Sct type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 18 June 2013.
  32. ↑ "BD Phe". International Variable Star Index. AAVSO. 4 January 2010. Retrieved 18 June 2013.
  33. ↑ "LHS 1220 – High proper-motion Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 11 May 2013.
  34. ↑ Zechmeister, M.; Kürster, M.; Endl, M.; Lo Curto, G.; et al. (2013). "The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars". Astronomy & Astrophysics. 552: A78. arXiv:1211.7263Freely accessible. Bibcode:2013A&A...552A..78Z. doi:10.1051/0004-6361/201116551.
  35. ↑ Maldonado, J.; Eiroa, C.; Villaver, E.; Montesinos, B.; et al. (2012). "Metallicity of solar-type stars with debris discs and planets". Astronomy & Astrophysics. 541: A40. arXiv:1202.5884Freely accessible. Bibcode:2012A&A...541A..40M. doi:10.1051/0004-6361/201218800.
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  38. ↑ Subasavage, John P.; Jao; Henry; Bergeron; et al. (2009). "The Solar Neighbourhood. XXI. Parallax Results from the CTIOPI 0.9 m Program: 20 New Member of the 25 Parsec White Dwarf Sample". The Astronomical Journal. 137 (6): 4547–60. Bibcode:2009AJ....134.4547S. doi:10.1088/0004-6256/137/6/4547.
  39. ↑ Kaler, Jim. "HR 6 Phoenicis". Stars. University of Illinois. Retrieved 24 August 2012.
  40. ↑ Hellier, Coel; Anderson, D.R.; Cameron, A. Collier; Gillon, M.; et al. (2009). "An orbital period of 0.94 days for the hot-Jupiter planet WASP-18b". Nature. Nature Publishing Group. 460 (7259): 1098–1100. Bibcode:2009Natur.460.1098H. doi:10.1038/nature08245. PMID 19713926.
  41. ↑ "NASA's Chandra X-ray Observatory Finds Planet That Makes Star Act Deceptively Old". Chandra X-ray Observatory. Retrieved 20 September 2014.
  42. ↑ Gillon, M.; Smalley, B.; Hebb, L.; Anderson, D. R.; et al. (2009). "Improved parameters for the transiting hot Jupiters WASP-4b and WASP-5b". Astronomy and Astrophysics. 496: 259–67. arXiv:0812.1998Freely accessible. Bibcode:2009A&A...496..259G. doi:10.1051/0004-6361:200810929.
  43. ↑ Hellier, Coel; Anderson, D. R.; Collier Cameron, A.; Gillon, M.; et al. (2010). "WASP-29b: A Saturn-sized transiting exoplanet" (PDF). The Astrophysical Journal Letters. 723 (1): L60–63. arXiv:1009.5318Freely accessible. Bibcode:2010ApJ...723L..60H. doi:10.1088/2041-8205/723/1/L60.
  44. ↑ Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; et al. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal. 753 (2): 156. arXiv:1205.2122Freely accessible. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156.
  45. ↑ Jameson, R.F.; Hodgkin, S.T. (1997). "Brown Dwarfs and Low Mass Stars". Brown Dwarfs. Leicester, United Kingdom: University of Leicester. Retrieved 16 August 2013.
  46. ↑ "Science: Brown Dwarfs". Wide-field Infrared Survey Explorer. NASA. 31 August 2011. Retrieved 16 August 2013.
  47. 1 2 Christlieb, Norbert (30 October 2002). "A Glimpse of the Young Milky Way: VLT UVES Observes Most Metal-Deficient Star Known". European Southern Observatory. Retrieved 26 July 2013.
  48. ↑ "2MASS J01092916-5224341 – Carbon Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 17 August 2013.
  49. ↑ O'Meara, Stephen James (2011). Deep-Sky Companions: The Secret Deep. Cambridge, United Kingdom: Cambridge University Press. pp. 40–43. ISBN 978-0-521-19876-9.
  50. ↑ "NED results for NGC 37". NED via University of California. Retrieved 19 August 2013.
  51. ↑ Boffin, Henri (4 November 2005). "eso0535 — Photo Release: Cosmic Portrait of a Perturbed Family". European Southern Observatory. Retrieved 24 August 2012.
  52. ↑ Waugh, Rob (15 February 2012). "Star wars: Hubble captures remains of shredded galaxy around rare new kind of black hole". Daily Mail. Retrieved 4 September 2013.
  53. ↑ "Astronomers spot the very first intermediate-mass black hole". The Bunsen Burner. T.E. Holdings LLC. 9 July 2012. Retrieved 15 August 2013.
  54. ↑ Chu, Jennifer (15 August 2012). "Most massive and luminous galaxy cluster identified". MIT News. Cambridge, Massachusetts: Massachusetts Institute of Technology. Retrieved 25 August 2012.
  55. ↑ Perrotto, Trent J.; Anderson, Janet; Watzke, Megan (10 January 2012). "NASA's Chandra Finds Largest Galaxy Cluster in Early Universe". NASA. Retrieved 2 September 2013.
  56. ↑ Chandra X-ray Observatory (10 January 2012). "El Gordo: NASA's Chandra Finds Largest Galaxy Cluster in Early Universe". NASA. Retrieved 2 September 2013.
  57. ↑ Jenniskens, Peter (2006). Meteor Showers and Their Parent Comets. Cambridge, United Kingdom: Cambridge University Press. pp. 387–88. ISBN 978-0-521-85349-1.
  58. ↑ Levy, David H. (2008). David Levy's Guide to Observing Meteor Showers. Cambridge, United Kingdom: Cambridge University Press. p. 115. ISBN 978-0-521-69691-3.

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