Pisces
Constellation
Pisces
List of stars in Pisces
AbbreviationPsc
GenitivePiscium
Pronunciation/ˈpaɪsiːz/; genitive /ˈpɪʃiəm/
Symbolismthe Fishes
Right ascension1h
Declination+15°
QuadrantNQ1
Area889 sq. deg. (14th)
Main stars18
Bayer/Flamsteed
stars		86
Stars with planets13
Stars brighter than 3.00m0
Stars within 10.00 pc (32.62 ly)8
Brightest starη Psc (Alpherg) (3.62m)
Messier objects1
Meteor showersPiscids
Bordering
constellations
Visible at latitudes between +90° and −65°.
Best visible at 21:00 (9 p.m.) during the month of November.

Pisces is a constellation of the zodiac. Its vast bulk – and main asterism viewed in most European cultures per Greco-Roman antiquity as a distant pair of fishes connected by one cord each that join at an apex – are in the Northern celestial hemisphere. Its old astronomical symbol is (♓︎). Its name is Latin for "fishes". It is between Aquarius, of similar size, to the southwest and Aries, which is smaller, to the east. The ecliptic and the celestial equator intersect within this constellation and in Virgo. This means the sun passes directly overhead of the equator, on average, at approximately this point in the sky, at the March equinox.

Features

The constellation Pisces as it can be seen by naked eye

The March equinox is currently located in Pisces, due south of Psc, and, due to precession, slowly drifting due west, just below the western fish towards Aquarius.

Stars

Although Pisces is a large constellation, there are only two stars brighter than magnitude 4 in Pisces. It is also the second dimmest of the zodiac constellations.

  • Alrescha ("the cord"), otherwise Alpha Piscium (α Psc), 309.8 lightyears, class A2, magnitude 3.62. Variable binary star.[1]
  • Fumalsamakah[2] ("mouth of the fish"), otherwise Beta Piscium (β Psc), 492 lightyears, class B6Ve, magnitude 4.48
  • Delta Piscium (δ Psc), 305 lightyears, class K5III, magnitude 4.44. Like other stars near the ecliptic, Delta Piscium is subject to lunar occultations.[3]
  • Epsilon Piscium (ε Psc), 190 lightyears, class K0III, magnitude 4.27. Has a candidate exoplanet.[4]
  • Revati[2] ("rich"), otherwise Zeta Piscium (ζ Psc), 148 lightyears, class A7IV, magnitude 5.21. Quintuple star system.[5]
  • Alpherg ("emptying"),[2] otherwise Eta Piscium (η Psc), 349 lightyears, class G7 IIIa, magnitude 3.62. It is a Gamma Cassiopeiae variable[6] with a weak magnetic field.[7]
  • Torcular ("thread"),[2] otherwise Omicron Piscium (ο Psc), 258 lightyears, class K0III, magnitude 4.2. It is an evolved red giant star on the horizontal branch.[8]
  • Omega Piscium (ω Psc), 106 lightyears, class F4IV, magnitude 4.03. It is an F-type star that is either a subgiant or on the main sequence.[9][10]
  • Gamma Piscium (γ Psc), 138 lightyears, magnitude 3.70. The star hosts an exoplanet which was discovered in 2021.[4] It has a spectral type of G8 III.[11]
  • Van Maanen's Star is the closest-known solitary white dwarf to us, with a dim apparent magnitude. It is located about 2° to the south of the star Delta Piscium,[12] with a relatively high proper motion of 2.978″ annually along a position angle of 155.538°.[13] It is closer to the Sun than any other solitary white dwarf. It is too faint to be seen with the naked eye.[12] Like other white dwarfs, it is a very dense star: its mass has been estimated to be about 67% of the Sun's,[14] yet it has only 1% of the Sun's radius.[15] The outer atmosphere has a temperature of approximately 6,110 K,[14] which is relatively cool for a white dwarf. As all white dwarfs steadily radiate away their heat over time, this temperature can be used to estimate its age, thought to be around 3 billion years.[16] It was originally thought to be an F-type star before the properties of white dwarfs were known.[17][18]

Due to the dimness of these stars, the constellation is essentially invisible in or near any major city due to light pollution.

Deep-sky objects

M74 is a loosely wound (type Sc) spiral galaxy in Pisces, found at a distance of 30 million light years (redshift 0.0022). It has many clusters of young stars and the associated nebulae, showing extensive regions of star formation. It was discovered by Pierre Méchain, a French astronomer, in 1780. A type II-P supernova was discovered in the outer regions of M74 by Robert Evans in June 2003; the star that underwent the supernova was later identified as a red supergiant with a mass of 8 solar masses.[19] It is the brightest member of the M74 Group.[20][21][22]

NGC 488 is an isolated face-on prototypical spiral galaxy.[23] Two supernovae have been observed in the galaxy.[24]

NGC 520 is a pair of colliding galaxies located 105 million light-years away.[25]

CL 0024+1654 is a massive galaxy cluster that lenses the galaxy behind it, creating arc-shaped images of the background galaxy. The cluster is primarily made up of yellow elliptical and spiral galaxies, at a distance of 3.6 billion light-years from Earth (redshift 0.4), half as far away as the background galaxy, which is at a distance of 5.7 billion light-years (redshift 1.67).[19]

History and mythology

From Urania's Mirror (1824)

Pisces originates from some composition of the Babylonian constellations Šinunutu4 "the great swallow" in current western Pisces, and Anunitum the "Lady of the Heaven" (supposedly Inanna), at the place of the northern fish. In the first-millennium BC texts known as the Astronomical Diaries, part of the constellation was also called DU.NU.NU (Rikis-nu.mi, "the fish cord or ribbon").[26]

Greco-Roman period

Pisces is associated with the Greek legend that Aphrodite and her son Eros either shape-shifted into forms of fishes to escape, or were rescued by two fishes.

In the Greek version according to Hyginus, Aphrodite and Eros while visiting Syria fled from the monster Typhon by leaping into the Euphrates River and transforming into fishes (Poeticon astronomicon 2.30, citing Diognetus Erythraeus).[27] The Roman variant of the story has Venus and Cupid (counterparts for Aphrodite and Eros) carried away from this danger on the backs of two fishes (Ovid Fasti 2.457ff).[28][29]

There is also a different origin tale that Hyginus preserved in another work. According to this, an egg rolled into the Euphrates, and some fishes nudged this to shore, after which the doves sat on the egg until Aphrodite (thereafter called the Syrian Goddess) hatched out of it. The fishes were then rewarded by being placed in the skies as a constellation (Fabulae 197).[30][31] This story is also recorded by the Third Vatican Mythographer.[32]

Modern period

Pisces in Hevelius' map (1690)

In 1690, the astronomer Johannes Hevelius in his Firmamentum Sobiescianum regarded the constellation Pisces as being composed of four subdivisions:[33]

  • Piscis Boreus (the North Fish): σ – 68 – 65 – 67 – ψ1 – ψ2 – ψ3 – χ – φ – υ – 91 – τ – 82 – 78 Psc.
  • Linum Boreum (the North Cord):[33] χ – ρ,94 – VX(97) – η – π – ο – α Psc.
  • Linum Austrinum (the South Cord):[33] α – ξ – ν – μ – ζ – ε – δ – 41 – 35 – ω Psc.
  • Piscis Austrinus (the South Fish):[33] ω – ι – θ – 7 – β – 5 – κ,9 – λ – TX(19) Psc.

"Piscis Austrinus" more often refers to a separate constellation in its own right.

In 1754, the botanist and author John Hill proposed to sever a southern zone of Pisces as Testudo (the Turtle).[34] 24 – 27 – YY(30) – 33 – 29 Psc.,[35] It would host a natural but quite faint asterism in which the star 20 Psc is the head of the turtle. While Admiral Smyth mentioned the proposal,[36] it was largely neglected by other astronomers, and it is now obsolete.[35]

Western folklore

The Fishes are in the German lore of Antenteh, who owned just a tub and a crude cabin when he met two magical fish. They offered him a wish, which he refused. However, his wife begged him to return to the fish and ask for a beautifully furnished home. This wish was granted, but her desires were not satisfied. She then asked to be a queen and have a palace, but when she asked to become a goddess, the fish became angry and took the palace and home, leaving the couple with the tub and cabin once again. The tub is sometimes recognized as the Great Square of Pegasus.[37]

In non-Western astronomy

The stars of Pisces were incorporated into several constellations in Chinese astronomy. Wai-ping ("Outer Enclosure") was a fence that kept a pig farmer from falling into the marshes and kept the pigs where they belonged. It was represented by Alpha, Delta, Epsilon, Zeta, Mu, Nu, and Xi Piscium. The marshes were represented by the four stars designated Phi Ceti. The northern fish of Pisces was a part of the House of the Sandal, Koui-siou.[38]

See also

References

  1. ↑ Wraight, K. T.; Fossati, L.; Netopil, M.; Paunzen, E.; Rode-Paunzen, M.; Bewsher, D.; Norton, A. J.; White, Glenn J. (2012). "A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars". Monthly Notices of the Royal Astronomical Society. 420 (1): 757. arXiv:1110.6283. Bibcode:2012MNRAS.420..757W. doi:10.1111/j.1365-2966.2011.20090.x. S2CID 14811051.
  2. 1 2 3 4 "Naming Stars". IAU.org. Retrieved 8 August 2018.
  3. ↑ Meyer, C.; et al. (1995), "Observations of lunar occultations at Observatoire de la Cote d'Azur", Astronomy and Astrophysics Supplement, 110: 107, Bibcode:1995A&AS..110..107M.
  4. 1 2 Teng, Huan-Yu; Sato, Bun'ei; Takarada, Takuya; Omiya, Masashi; Harakawa, Hiroki; Izumiura, Hideyuki; Kambe, Eiji; Takeda, Yoichi; Yoshida, Michitoshi; Itoh, Yoichi; Ando, Hiroyasu; Kokubo, Eiichiro (2022), "Regular radial velocity variations in nine G- and K-type giant stars: Eight planets and one planet candidate", Publications of the Astronomical Society of Japan, 74: 92–127, arXiv:2112.07169, doi:10.1093/pasj/psab112
  5. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  6. ↑ Cvetković, Z.; Novaković, B. (March 2010), "Eight new and three recalculated orbits for binaries", Astronomische Nachrichten, 331 (3): 304, Bibcode:2010AN....331..304C, doi:10.1002/asna.200911250.
  7. ↑ Aurière, M.; Konstantinova-Antova, R.; Charbonnel, C.; Wade, G. A.; Tsvetkova, S.; Petit, P.; Dintrans, B.; Drake, N. A.; Decressin, T.; Lagarde, N.; Donati, J. F.; Roudier, T.; Lignières, F.; Schröder, K. P.; Landstreet, J. D.; Lèbre, A.; Weiss, W. W.; Zahn, J. P. (February 2015), "The magnetic fields at the surface of active single G-K giants", Astronomy & Astrophysics, 574: 30, arXiv:1411.6230, Bibcode:2015A&A...574A..90A, doi:10.1051/0004-6361/201424579, S2CID 118504829, A90.
  8. ↑ Reffert, Sabine; et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy and Astrophysics, 574A (2): 116–129, arXiv:1412.4634, Bibcode:2015A&A...574A.116R, doi:10.1051/0004-6361/201322360, S2CID 59334290.
  9. ↑ Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–18, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117, S2CID 122811461.
  10. ↑ Griffin, R. F.; Redman, R. O. (1960), "Photoelectric measurements of the λ4200 A CN band and the G band in G8-K5 spectra", Monthly Notices of the Royal Astronomical Society, 120 (4): 287–316, Bibcode:1960MNRAS.120..287G, doi:10.1093/mnras/120.4.287.
  11. ↑ Baines, Ellyn K.; et al. (2018). "Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer". The Astronomical Journal. 155 (1). 30. arXiv:1712.08109. Bibcode:2018AJ....155...30B. doi:10.3847/1538-3881/aa9d8b. S2CID 119427037.
  12. 1 2 Burnham, Robert (1978), Burnham's celestial handbook: an observer's guide to the universe beyond the solar system, Dover books explaining science, vol. 3 (2nd ed.), Courier Dover Publications, pp. 1474–1477, ISBN 0-486-23673-0.
  13. ↑ Sion, Edward M.; et al. (June 2014), "The White Dwarfs within 25 pc of the Sun: Kinematics and Spectroscopic Subtypes", The Astronomical Journal, 147 (6): 11, arXiv:1401.4989, Bibcode:2014AJ....147..129S, doi:10.1088/0004-6256/147/6/129, S2CID 119184859, 129.
  14. 1 2 Limoges, M. -M.; et al. (August 2015), "Physical Properties of the Current Census of Northern White Dwarfs within 40 pc of the Sun", The Astrophysical Journal Supplement Series, 219 (2): 35, arXiv:1505.02297, Bibcode:2015ApJS..219...19L, doi:10.1088/0067-0049/219/2/19, S2CID 118494290, 19.
  15. ↑ Giammichele, N.; et al. (April 2012), "Know Your Neighborhood: A Detailed Model Atmosphere Analysis of Nearby White Dwarfs", The Astrophysical Journal Supplement, 199 (2): 29, arXiv:1202.5581, Bibcode:2012ApJS..199...29G, doi:10.1088/0067-0049/199/2/29, S2CID 118304737. Based on log L/L☉ = −3.77.
  16. ↑ Sion, Edward M.; et al. (December 2009), "The White Dwarfs Within 20 Parsecs of the Sun: Kinematics and Statistics", The Astronomical Journal, 138 (6): 1681–1689, arXiv:0910.1288, Bibcode:2009AJ....138.1681S, doi:10.1088/0004-6256/138/6/1681, S2CID 119284418.
  17. ↑ Holberg, J. B. (May 2009), "The Discovery of the Existence of White Dwarf Stars: 1862 to 1930", Journal for the History of Astronomy, 40 (2): 137–154, Bibcode:2009JHA....40..137H, doi:10.1177/002182860904000201, S2CID 117939625.
  18. ↑ van Maanen, A. (December 1917), "Two Faint Stars with Large Proper Motion", Publications of the Astronomical Society of the Pacific, 29 (172): 258–259, Bibcode:1917PASP...29..258V, doi:10.1086/122654.
  19. 1 2 Wilkins, Jamie; Dunn, Robert (2006). 300 Astronomical Objects: A Visual Reference to the Universe (1st ed.). Buffalo, New York: Firefly Books. ISBN 978-1-55407-175-3.
  20. ↑ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge University Press. ISBN 978-0-521-35299-4.
  21. ↑ A. Garcia (1993). "General study of group membership. II – Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90. Bibcode:1993A&AS..100...47G.
  22. ↑ G. Giuricin; C. Marinoni; L. Ceriani; A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal. 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. S2CID 9618325.
  23. ↑ Sil'chenko, O. K. (March 1999). "Chemically decoupled nucleus and the structure of the nuclear region in the spiral galaxy NGC 488". Astronomy Letters. 25 (3): 140–8. Bibcode:1999AstL...25..140S. Retrieved 29 December 2015.
  24. ↑ List of Supernovae IAU Central Bureau for Astronomical Telegrams. Retrieved 29 December 2015.
  25. ↑ Cappellari, Michele; et al. (May 2011). "The ATLAS3D project - I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria". Monthly Notices of the Royal Astronomical Society. 413 (2): 813–836. arXiv:1012.1551. Bibcode:2011MNRAS.413..813C. doi:10.1111/j.1365-2966.2010.18174.x. S2CID 15391206.
  26. ↑ Origins of the ancient constellations: I. The Mesopotamian traditions by J. H. Rogers 1998, page 19 page 19 (table 3, rows 2-3) and page 27
  27. ↑ Hard (2015), pp. 84–85.
  28. ↑ Hard (2015), pp. 85–86.
  29. ↑ Publius Ovidius Naso (1995). Ovid's Fasti: Roman Holidays. Translated by Betty Rose Nagle. Indiana University Press. pp. 69–70, 182. ISBN 9-780-25320-933-7.
  30. ↑ Rigoglioso, Marguerite (2009). The Cult of Divine Birth in Ancient Greece. Springer. p. 248. ISBN 978-0-230-62091-9.
  31. ↑ Ridpath (1988), p. 108.
  32. ↑ Van Berg, Paul-Louis (1972). Corpus Cultus Deae Syriae - Ccds: Les Sources Litteraires - Repertoire Des Sources Grecques Et Latines - Sauf Le De Dea Syria - (in French). Brill Archive. pp. 37–38. ISBN 9-789-00403-503-4.
  33. 1 2 3 4 Hevelius, J., (1690) Firmamentum Sobiescianum, Leipzig, Fig.NN
  34. ↑ Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 163 342. ISBN 978-0-486-21079-7.
  35. 1 2 Ciofi, Claudio; Torre, Pietro, Costellazioni Estinte (nate dal 1700 al 1800): Sezione di Ricerca per la Cultura Astronomica
  36. ↑ Smyth, W. H., (1884) The Bedford Catalogue, p. 23
  37. ↑ Staal (1988), pp. 45–46.
  38. ↑ Staal (1988), pp. 45–47.

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