Epoch J2000 Equinox J2000
|Constellation||Piscis Austrinus (Fomalhaut A+B), Aquarius (Fomalhaut C)|
|Right ascension||22h 57m 39.0465s|
|Declination||−29° 37′ 20.050″|
|Apparent magnitude (V)||1.16|
|TW Piscis Austrini|
|Right ascension||22h 56m 24.05327s|
|Declination||−31° 33′ 56.0351″|
|Apparent magnitude (V)||6.48|
|Right ascension||22h 48m 04.47s|
|Declination||−24° 22′ 07.5″|
|Apparent magnitude (V)||12.618|
|Spectral type||A3 V / K5Vp / M4V|
|U−B color index||0.08 / 1.02 / ?|
|B−V color index||0.09 / 1.10 / 1.683|
|Variable type||None / BY Draconis / ?|
|Radial velocity (Rv)||+6.5 km/s|
|Proper motion (μ)||RA: +328.95 mas/yr
Dec.: −164.67 mas/yr
|Parallax (π)||129.81 ± 0.47 mas|
|Distance||25.13 ± 0.09 ly
(7.70 ± 0.03 pc)
|Absolute magnitude (MV)||1.72|
|TW Piscis Austrini|
|Radial velocity (Rv)||+6 km/s|
|Proper motion (μ)||RA: −331.11 mas/yr
Dec.: −158.98 mas/yr
|Parallax (π)||131.42 ± 0.62 mas|
|Distance||24.82 ± 0.09 ly
(7.61 ± 0.04 pc)
|Absolute magnitude (MV)||7.08|
|Surface gravity (log g)||4.21 cgs|
|Metallicity [Fe/H]||−0.03 to −0.34 dex|
|Rotational velocity (v sin i)||93 km/s|
|TW Piscis Austrini|
|Mass||0.725 ± 0.036 M☉|
|Radius||0.629 ± 0.051 R☉|
|Temperature||4,711 ± 134 K|
|Rotational velocity (v sin i)||2.93 km/s|
|Age||4.4 × 108 years|
|Fomalhaut: α Piscis Austrini, α PsA, Alpha PsA, 24 Piscis Austrini, CPD −30° 6685, FK5 867, Gl 881, HD 216956, HIP 113368, HR 8728, SAO 191524|
|TW Piscis Austrini: Fomalhaut B, TW PsA, Gl 879, HR 8721, CD -32°17321, HD 216803, LTT 9283, GCTP 5562.00, SAO 214197, CP(D)-32 6550, HIP 113283|
|LP 876-10: Fomalhaut C, 2MASS J22480446-2422075, NLTT 54872, GSC 06964-01226|
|TW Piscis Austrini|
Fomalhaut (Alpha Piscis Austrini, Alpha PsA, α Piscis Austrini, α PsA) is the brightest star in the constellation Piscis Austrinus and one of the brightest stars in the sky. It is a class A star on the main sequence approximately 25 light-years (7.7 pc) from Earth as measured by the Hipparcos astrometry satellite. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. It is classified as a Vega-like star that emits excess infrared radiation, indicating it is surrounded by a circumstellar disk. Fomalhaut, K-type star TW Piscis Austrini and M-type star LP 876-10 constitute a trinary system.
Fomalhaut holds a special significance in extrasolar planet research, as it is the center of the first stellar system with an extrasolar planet candidate (Fomalhaut b) imaged at visible wavelengths. The image was published in Science in November 2008. Fomalhaut is the third brightest star known to have a planetary system (as viewed from Earth), after Pollux and the Sun.
At a declination of −29.6°, Fomalhaut is located south of the celestial equator, and hence is best viewed from the Southern Hemisphere. However, its southerly declination is not as great as that of stars such as Acrux, Alpha Centauri and Canopus, meaning that, unlike them, Fomalhaut is visible from a large part of the Northern Hemisphere as well. Its declination is greater than that of Sirius and similar to that of Antares. At 40°N, Fomalhaut rises above the horizon for eight hours and reaches only 20° above the horizon, while Capella which rises at approximately the same time will stay above the horizon for twenty hours. From England the star never appears much brighter than magnitude 2.2 due to it being so close to the horizon, and from southern Alaska or Scandinavia it never rises above the horizon at all. Fomalhaut can be located in these northern latitudes by the fact that the western (right-hand) side of the Square of Pegasus points to it. Continue the line from Beta to Alpha Pegasi towards the southern horizon: Fomalhaut is about 45˚ south of Alpha Pegasi, with no bright stars in between.
Fomalhaut is a young star, for many years thought to be only 100 to 300 million years old, with a potential lifespan of a billion years. A 2012 study gave a slightly higher age of 440±40 million years. The surface temperature of the star is around 8,590 K (8,320 °C). Fomalhaut's mass is about 1.92 times that of the Sun, its luminosity is about 16.6 times greater, and its diameter is roughly 1.84 times as large.
Fomalhaut is slightly metal-deficient as compared to the Sun, which means it is composed of a smaller percentage of elements other than hydrogen and helium. The metallicity is typically determined by measuring the abundance of iron in the photosphere relative to the abundance of hydrogen. A 1997 spectroscopic study measured a value equal to 93% of the Sun's abundance of iron.[nb 1] A second 1997 study deduced a value of 78% by assuming Fomalhaut has the same metallicity as the neighboring star TW Piscis Austrini, which has since been argued to be a physical companion. In 2004, a stellar evolutionary model of Fomalhaut yielded a metallicity of 79%. Finally, in 2008, a spectroscopic measurement gave a significantly lower value of 46%.
Fomalhaut has been claimed to be one of approximately 16 stars belonging to the Castor Moving Group. This is an association of stars that share a common motion through space and have been claimed to be physically associated. Other members of this group include Castor and Vega. The moving group has an estimated age of 200±100 million years and originated from the same location. Unfortunately more recent work that has found that purported members of the Castor Moving Group appear to not only have a wide range of ages, but their velocities are too different to have been possibly associated with one another in the distant past. Hence, "membership" to this dynamical group has no bearing on the age of the Fomalhaut system.
Debris disks and planet
|This section's factual accuracy may be compromised due to out-of-date information. (May 2013)|
Fomalhaut is surrounded by several debris disks.
The inner disk is a high-carbon small-grain (10-300 nm) ash disk clustering at 0.1 AU from the star. Next is a disk of larger particles with inner edge 0.4-1 AU of the star. The innermost disk is unexplained as yet.
The outermost disk is at a radial distance of 133 AU (1.99×1010 km; 1.24×1010 mi), in a toroidal shape with a very sharp inner edge, all inclined 24 degrees from edge-on. The dust is distributed in a belt about 25 AU wide. The geometric center of the disk is offset by about 15 AU (2.2×109 km; 1.4×109 mi) from Fomalhaut. The disk is sometimes referred to as "Fomalhaut's Kuiper belt". Fomalhaut's dusty disk is believed to be protoplanetary, and emits considerable infrared radiation. Measurements of Fomalhaut's rotation indicate that the disk is located in the star's equatorial plane, as expected from theories of star and planet formation.
On November 13, 2008, astronomers announced an object, which they assumed to be an extrasolar planet, orbiting just inside the outer debris ring. This was the first extrasolar orbiting object to be seen with visible light, captured by the Hubble Space Telescope. A planet's existence had been previously suspected from the sharp, elliptical inner edge of that disk. The mass of the planet, Fomalhaut b, was estimated to be no more than three times the mass of Jupiter but at least the mass of Neptune. There are indications that the orbit is not apsidally aligned with the dust disk, which may indicate that additional planets may be responsible for the dust disk's structure.
However M-band images taken from the MMT Observatory put strong limits on the existence of gas giants within 40 AU of the star and Spitzer Space Telescope imaging suggested that the object Fomalhaut b was more likely to be a dust cloud. In 2012, two independent studies confirmed that Fomalhaut b does exist; but it is shrouded by debris, so it may be a gravitationally-bound accumulation of rubble rather than a whole planet.
Herschel Space Observatory images of Fomalhaut reveal a large amount of fluffy micrometer-sized dust is present in the outer dust belt. Because such dust is expected to be blown out of the system by stellar radiation pressure on short timescales, its presence indicates a constant replenishment by collisions of planetesimals. The fluffy morphology of the grains suggests a cometary origin. The collision rate is estimated to be approximately 2000 kilometre-sized comets per day.
Observations of the star's outer dust ring by the Atacama Large Millimeter Array point to the existence of two planets in the system, neither one at the orbital radius proposed for the HST-discovered Fomalhaut b.
If there are additional planets from 4 to 10 AU, they must be under 20 MJ; if from 2.5 outward, then 30 MJ.
(in order from star)
|Inner hot disk||0.08–0.11 AU||—||—|
|Outer hot disk||0.21–0.62 AU or 0.88–1.08 AU||—||—|
|10 AU belt||8–12 AU||—||—|
|Interbelt dust disk||35–133 AU||—||—|
|Main belt||133–158 AU||−66.1°||—|
|Main belt outer halo||158–209 AU||—||—|
Fomalhaut B (TW Piscis Austrini)
Fomalhaut forms a binary star with the K4-type star TW Piscis Austrini (TW PsA, Fomalhaut B). TW Piscis Austrini lies 0.28 parsecs (0.91 light years) away from Fomalhaut, and its space velocity agrees with that of Fomalhaut within 0.1±0.5 km/s, consistent with being a bound companion. A recent age estimate for TW PsA (400±70 million years), agrees very well with the isochronal age for Fomalhaut (450±40 million years), further arguing for the two stars forming a physical binary.
The designation TW Piscis Austrini is astronomical nomenclature for a variable star. Fomalhaut B is a flare star of the type known as a BY Draconis variable. It varies slightly in apparent magnitude, ranging from 6.44 to 6.49 over a 10.3 day period. While smaller than the Sun, it is relatively large for a flare star. Most flare stars are red M-type dwarfs.
Fomalhaut C (LP 876-10)
LP 876-10 (Fomalhaut C) is also associated with the Fomalhaut system, making it a trinary star. In October 2013, Eric Mamajek and collaborators from the RECONS consortium announced that the previously known high proper motion star LP 876-10 had a distance, velocity, and color-magnitude position consistent with being a 3rd member of the Fomalhaut system. LP 876-10 was originally catalogued as a high proper motion star by Willem Luyten in his 1979 NLTT catalogue, however a precise trigonometric parallax and radial velocity was only measured quite recently. LP 876-10 is a red dwarf star of spectral type M4 V, and located even further from Fomalhaut A than TW PsA—about 5.7° away from Fomalhaut A in the sky in the neighbouring constellation Aquarius, whereas both Fomalhaut A and TW PsA are located in constellation Piscis Austrinus. Its current separation from Fomalhaut A is about 0.77 parsecs (2.5 light years), and it is currently located 0.987 parsecs (3.2 light years) away from TW PsA (Fomalhaut B). LP 876-10 is located well within the tidal radius of the Fomalhaut system, which is 1.9 parsecs (6.2 light years). Although LP 876-10 is itself catalogued as a binary star in the Washington Double Star Catalog (called "WSI 138"), there was no sign of a close-in stellar companion in the imaging, spectral, or astrometric data in the Mamajek et al. study. In December 2013, Kennedy et al. reported the discovery of a cold dusty debris disks associated with Fomalhaut C, using infrared images from the Herschel Space Observatory. Multiple star systems hosting multiple debris disks are exceedingly rare.
(in order from star)
|Debris disk||~10–<40 AU||—||—|
Etymology and cultural significance
Fomalhaut has had various names ascribed to it through time. Its modern name derives from Arabic fum al-ḥawt, meaning "mouth of the [Southern] Fish" (فُمْ اَلْحَوْتْ), a translation of how the classical astronomer Ptolemy labeled it.
The star has been recognized by many cultures of the northern hemisphere, including the Arabs, Persians and Chinese. It marked the solstice in 2500 BC. It was also a marker for the worship of Demeter in Eleusis.
Ptolemy put it in Aquarius as well as Piscis Austrinus. In the 1600s Bayer firmly planted it in the primary position of Piscis Austrinus. Following Ptolemy, Flamsteed in 1725 denoted it 79 Aquarii as well as 24 Piscis Austrini. The current name reflects modern consensus on Bayer's decision, that the star belongs in Piscis Austrinus.
Another name in Western use is "the Lonely Star of Autumn", because it is the only first-magnitude star in the autumn sky of mid-northern latitudes.
- It was called Hastorang by the Persians, one of the four "royal stars".
- The name Fom al-Haut comes from scientific Arabic فم الحوت fam al-ħūt (al-janūbī) "the mouth of the [Southern] Fish".
- The Latin names are ōs piscis merīdiāni, ōs piscis merīdionālis, ōs piscis notii "the mouth of the Southern Fish".
- The name Difda al Auwel comes from the colloquial Arabic الضفدع الأول aḍ-ḍifdiˤ al-’awwal "the first frog" (the second frog is Beta Ceti).
- The Chinese name 北落師門/北落师门 (Mandarin: Běilàshīmén) meaning North Gate of the Military Camp, because this star is marking itself and stand alone in North Gate of the Military Camp asterism, Encampment mansion (see : Chinese constellation). 北落师门 (Běilàshīmén) westernized into Pi Lo Sze Mun in R.H. Allen's work.
- To the Moporr Aboriginal people of South Australia, it is a masculine being called Buunjill. The Wardaman people of the Northern Territory called Fomalhaut Menggen —white cockatoo.
Fomalhaut/Earthwork B in Mounds State Park near Anderson, Indiana, lines up with the rising of the star Fomalhaut in the fall months, according to the Indiana Department of Natural Resources. In 1980, astronomer Jack Robinson proposed that the rising azimuth of Fomalhaut was marked by cairn placements at both the Bighorn and Moose Mountain Medicine Wheels in Wyoming, USA and Saskatchewan, Canada, respectively.
The New Scientist magazine termed it the "Great Eye of Sauron" due to its shape and debris ring, when viewed from a distance, bearing similarity to the aforementioned "Eye" in the Peter Jackson Lord of the Rings films.
In Walter Tevis' novel Steps of the Sun, Fomalhaut is visited by the protagonist and two potentially inhabitable planets are found (and described). Parts of Philip K Dick's novel Lies, Inc (originally titled The Unteleported Man) are set on the fictional planet Fomalhaut IX.
- Calculation of metallicity: if m = [Fe/H], then the ratio of iron to hydrogen for Fomalhaut divided by the ratio of iron to hydrogen for the Sun is given by 10m.
||Constructs such as ibid., loc. cit. and idem are discouraged by Wikipedia's style guide for footnotes, as they are easily broken. Please improve this article by replacing them with named references (quick guide), or an abbreviated title. (March 2013)|
- van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357
- "V* TW PsA -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-01-20.
- "LP 876-10 -- Double or multiple star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2014-07-30.
- Demory, B.-O. et al. (October 2009), "Mass-radius relation of low and very low-mass stars revisited with the VLTI", Astronomy and Astrophysics 505 (1): 205–215, arXiv:0906.0602, Bibcode:2009A&A...505..205D, doi:10.1051/0004-6361/200911976
- Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99). Bibcode:1966CoLPL...4...99J.
- Mamajek, E.E. (August 2012). "On the Age and Binarity of Fomalhaut". Astrophysical Journal Letters 754 (2): L20. arXiv:1206.6353. Bibcode:2012ApJL..754...20M. doi:10.1088/2041-8205/754/2/L20.
- Di Folco, E.; Thévenin, F.; Kervella, P.; Domiciano de Souza, A.; Coudé du Foresto, V.; Ségransan, D.; Morel, P. (November 2004). "VLTI near-IR interferometric observations of Vega-like stars. Radius and age of α PsA, β Leo, β Pic, ɛ Eri and τ Cet". Astronomy and Astrophysics 426 (2): 601–617. Bibcode:2004A&A...426..601D. doi:10.1051/0004-6361:20047189. This paper lists [Fe/H] = −0.10 dex.
- Dunkin, S. K.; Barlow, M. J.; Ryan, Sean G.; Barlow; Ryan (April 1997). "High-resolution spectroscopy of Vega-like stars - I. Effective temperatures, gravities and photospheric abundances". Monthly Notices of the Royal Astronomical Society 286 (3): 604–616. Bibcode:1997MNRAS.286..604D. doi:10.1093/mnras/286.3.604. This paper lists [Fe/H] = −0.03 dex.
- Saffe, C.; Gómez, M.; Pintado, O.; González, E. (October 2008). "Spectroscopic metallicities of Vega-like stars". Astronomy and Astrophysics 490 (1): 297–305. arXiv:0805.3936. Bibcode:2008A&A...490..297S. doi:10.1051/0004-6361:200810260. This paper lists [Fe/H] = −0.34 dex.
- Perryman, Michael (2010), The Making of History's Greatest Star Map, Heidelberg: Springer-Verlag, doi:10.1007/978-3-642-11602-5
- Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society 25: 1319, Bibcode:1993AAS...183.1710G, retrieved 2012-02-04
- B. Mennesson, O. Absil, J. Lebreton, J.-C. Augereau, E. Serabyn, M. M. Colavita, R. Millan-Gabet, W. Liu, P.Hinz, P. Thebault (2012), "An interferometric study of the Fomalhaut inner debris disk II. Keck Nuller mid-infrared observations", Astrophysical Journal, arXiv:1211.7143, Bibcode:2013ApJ...763..119M, doi:10.1088/0004-637X/763/2/119
- Mamajek, Eric E.; Bartlett, Jennifer L.; Seifahrt, Andreas; Henry, Todd J.; Dieterich, Sergio B.; Lurie, John C.; Kenworthy, Matthew A.; Jao, Wei-Chun; Riedel, Adric R.; Subasavage, John P.; Winters, Jennifer G.; Finch, Charlie T.; Ianna, Philip A.; Bean, Jacob (2013). "The Solar Neighborhood. XXX. Fomalhaut C". The Astronomical Journal 146 (6): 154. arXiv:1310.0764. Bibcode:2013AJ....146..154M. doi:10.1088/0004-6256/146/6/154.
- Kalas, Paul; et al. (2008). "Optical Images of an Exosolar Planet 25 Light-Years from Earth". Science 322 (5906): 1345–1348. arXiv:0811.1994. Bibcode:2008Sci...322.1345K. doi:10.1126/science.1166609. PMID 19008414.
- "ALMA Reveals Workings of Nearby Planetary System". ESO Press Release. Retrieved 13 April 2012.
- Fred Schaaf (2008). The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars. John Wiley & Sons. p. 231. ISBN 047024917X.
- "Shallow Sky Object of the Month: Fomalhaut". Houston Astronomical Society. August 2013. Retrieved 2014-07-30.
- Barrado y Navascues, D. (1998). "The Castor moving group. The age of Fomalhaut and VEGA". Astronomy and Astrophysics 339: 831–839. arXiv:astro-ph/9905243. Bibcode:1998A&A...339..831B.
- "Elusive Planet Reshapes a Ring Around Neighboring Star". HubbleSite - newscenter (Space Telescope Science Institute (STScI)). June 22, 2005.
- Barrado y Navascues, David; Stauffer, John R.; Hartmann, Lee; Balachandran, Suchitra C. (January 1997). "The Age of Gliese 879 and Fomalhaut". Astrophysical Journal 475: 313. arXiv:astro-ph/9704021. Bibcode:1997ApJ...475..313B. doi:10.1086/303518. This paper lists [Fe/H] = −0.11 dex.
- Kalas, Paul; Graham, James R.; Clampin, Mark (2005). "A planetary system as the origin of structure in Fomalhaut's dust belt". Nature 435 (7045): 1067–1070. arXiv:astro-ph/0506574. Bibcode:2005Natur.435.1067K. doi:10.1038/nature03601. PMID 15973402.
- The disc was reported by Holland, Wayne S.; et al. (1998). "Submillimetre images of dusty debris around nearby stars". Nature 392 (6678): 788–791. Bibcode:1998Natur.392..788H. doi:10.1038/33874. They noted that the disc was centered on a cavity, which they suggested might have been swept out by planets.
- "Fomalhaut's Kuiper Belt". Sky & Telescope. Retrieved October 16, 2007.
- "Hubble Directly Observes a Planet Orbiting Another Star". Retrieved November 13, 2008.
- Le Bouquin, Jean-Baptiste; et al. (2009). "The spin-orbit alignment of the Fomalhaut planetary system probed by optical long baseline interferometry". arXiv:0904.1688 [astro-ph.SR].
- "From afar, the first optical photos of an exoplanet". AFP. 2008-11-13.
- Predictions for a planet just inside Fomalhaut's eccentric ring, Alice C. Quillen, Monthly Notices of the Royal Astronomical Society, 372, #1 (October 2006), pp. L14–L18, doi:10.1111/j.1745-3933.2006.00216.x, Bibcode: 2006MNRAS.372L..14Q.
- Paul Kalas (2008-11-13). "Direct Image Of Extrasolar Planet". Retrieved 2008-11-14. (at 3 minutes 45 seconds: "... has to be less than three Jupiter masses. In fact our lower limit to Fomalhaut b is Neptune")
- Chiang, E; et al. (2008). "Fomalhaut's Debris Disk and Planet: Constraining the Mass of Fomalhaut b From Disk Morphology". arXiv:0811.1985v1 [astro-ph].
- Kenworthy, Matthew A.; et al. (2008). "MMT/AO 5 micron Imaging Constraints on the Existence of Giant Planets Orbiting Fomalhaut at ~13-40 AU". arXiv:0811.2443v1 [astro-ph].
- Markus, J.; et al. (2012). "Infrared Non-detection of Fomalhaut b—Implications for the Planet Interpretation". arXiv:1201.4388v2 [astro-ph.EP].
- Raphael Galicher, Christian Marois, B. Zuckerman, Bruce Macintosh. "Fomalhaut b: Independent Analysis of the Hubble Space Telescope Public Archive Data". The Astrophysical Journal. arXiv:1210.6745. Bibcode:2013ApJ...769...42G. doi:10.1088/0004-637X/769/1/42.
- Thayne Currie; et al. "Direct Imaging Confirmation and Characterization of a Dust-Enshrouded Candidate Exoplanet Orbiting Fomalhaut". The Astrophysical Journal Letters. arXiv:1210.6620. Bibcode:2012ApJ...760L..32C. doi:10.1088/2041-8205/760/2/L32.
- Acke, B. (2012). "Herschel images of Fomalhaut. An extrasolar Kuiper belt at the height of its dynamical activity". Astronomy & Astrophysics (class: astro-ph). arXiv:1204.5037. Bibcode:2012A&A...540A.125A. doi:10.1051/0004-6361/201118581.
- Boley, A. et al. (2012). "Constraining the Planetary System of Fomalhaut Using High-Resolution ALMA Observations". arXiv:1204.0007v1.
- Matthew A. Kenworthy and Tiffany Meshkat (2012). "Coronagraphic Observations of Fomalhaut at Solar System Scales". Astrophysical Journal (class: astro-ph). arXiv:1212.1459. Bibcode:2013ApJ...764....7K. doi:10.1088/0004-637X/764/1/7.
- Kalas, Paul; Graham, James R.; Fitzgerald, Michael P.; Clampin, Mark (2013). "STIS Coronagraphic Imaging of Fomalhaut: Main Belt Structure and the Orbit of Fomalhaut b". The Astrophysical Journal 775 (1): article id. 56. arXiv:1305.2222. Bibcode:2013ApJ...775...56K. doi:10.1088/0004-637X/775/1/56.
- Kennedy, Grant M. et al. (2013-12-17). "Discovery of the Fomalhaut C debris disc". Monthly Notices of the Royal Astronomical Society. arXiv:1312.5315. Bibcode:2014MNRAS.438L..96K. doi:10.1093/mnrasl/slt168.
- "Fomalhaut had first visible exoplanet".
- Ibid, citing Richard Hinckley Allen
- Wagman, M. (August 1987). "Flamsteed's Missing Stars". Journal for the History of Astronomy, Vol.18, NO. 3/AUG, P.209, 1987 18: 212. Bibcode:1987JHA....18..209W.
- Richard Hinckley Allen:Star Names — Their Lore and Meaning (Piscis Australis, the Southern Fish)
- (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 7 日
- Dawson, James (1881). Australian Aborigines. Sydney: George Robertson. p. 100. ISBN 0-85575-118-5.
- Harney, Bill Yidumduma; Cairns, Hugh C. (2004) . Dark Sparklers (Revised ed.). Merimbula, New South Wales: Hugh C. Cairns. p. 204. ISBN 0-9750908-0-1.
- Robinson, J.H. (September 1980). "Fomalhaut and cairn D at the Big Horn and Moose Mountain Medicine Wheels". Bulletin of the Astronomical Society, Vol. 12, p. 887 12: 887. Bibcode:1980BAAS...12..887R.
- Ivan Semeniuk (22 June 2005). "Hubble spies lord of the stellar rings". New Scientist.
|Wikimedia Commons has media related to Fomalhaut.|
- "Fomalhaut". SolStation. Retrieved November 23, 2005.
- Preprint of planet discovery paper
- Astrobites summary of Janson et al. 2012, the Spitzer IR non-detection of Fomalhaut b
- Astrobites summary of Boley et al. 2012, the ALMA observations of the Fomalhaut ring system
- "Eye of Sauron" debris ring
- Researchers find that bright nearby double star Fomalhaut is actually a triple (Astronomy magazine : October 8, 2013)