Sextans

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Sextans is a faint, minor constellation on the celestial equator which was introduced in 1687 by Polish astronomer Johannes Hevelius. Its name is Latin for the astronomical sextant, an instrument that Hevelius made frequent use of in his observations.

CharacteristicsEdit

Sextans is a medium sized constellation bordering Leo to the north, touching on Hydra to the southwest, and Crater to the southeast. The recommended three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is "Sex".<ref name=pa30_469>Template:Cite magazine</ref> The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined by a square. In the equatorial coordinate system, the right ascension coordinates of these borders lie between Template:RA and Template:RA, while the declination coordinates are between +6.43° and −11.7°.<ref name = border>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Since it is close to the ecliptic plane, the Moon and planets regularly cross the constellation, especially its northeastern corner.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Notable featuresEdit

StarsEdit

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File:SextansCC.jpg

The constellation Sextans as it can be seen by the naked eye

John Flamsteed labeled 41 stars for the constellation.<ref name="wagman">Template:Cite book</ref> Francis Baily intended to give Bayer designations to some of the stars but because none of them were above magnitude 4.5, he left them unlettered.<ref name="wagman"/> Rather, it was Benjamin Apthorp Gould who lettered some of the stars. He labeled the five brightest stars using Greek letters Alpha (α) to Epsilon (ε) in his Uranometria Argentina.<ref name="wagman"/> All together, there are 38 stars that are brighter than or equal to apparent magnitude 6.5.Template:Efn<ref name=tirionconst>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Bright starsEdit

Alpha Sextantis is the brightest star in the constellation and the only star above the fifth magnitude with an apparent magnitude of 4.49. It is an ageing A-type star of spectral class A0 III<ref name = Cowley1969>Template:Cite journal</ref> located 280Template:± light-years away<ref name=vanLeeuwen2007>Template:Citation</ref> from the Solar System. At the age of 385 million years,<ref name=Bowman>Template:Cite journal</ref> it is exhausting hydrogen at its core and leaving the main sequence.
γ Sextantis is the second brightest star in the constellation with an apparent magnitude of 5.05. It is a binary star consisting of two A-type main-sequence stars with classes of A1 V and A4 V respectively.<ref name=Edwards1976>Template:Citation</ref> The stars take 77.55 years to circle each other in an eccentric orbit<ref name=Heintz1982>Template:Citation</ref> and the system is located 280Template:± light-years away from the Solar System.<ref name=vanLeeuwen2007/> The separation of the stars is four-tenths of an arcsecond,<ref name=Heintz1982/> making it difficult to observe without the use of a telescope with an aperture of 30 cm.
β Sextantis is slightly fainter at magnitude 5.07;<ref name=Crawford1971>Template:Citation</ref> it is said to be 364Template:± light-years distant.<ref name = GaiaDR2>Template:Cite DR2</ref> Beta Sextantis is a B-type main-sequence star of spectral class B6 V and it has been used as a standard in the MK spectral classification system.<ref name=Mathys1986>Template:Citation</ref> It is suspected to be a Alpha² Canum Venaticorum variable with a period of 15.4 days.<ref name=Kholopov1989>Template:Citation</ref>

Multiple star systemsEdit

Sextans contains a few notable multiple star systems within its boundaries.

35 Sextantis is a triple star system consisting of two evolved K-type giants of equal mass, with both stars being twice as massive as the Sun.<ref name = Tokovinin2008>Template:Cite journal</ref> The secondary is itself a single-lined spectroscopic binary consisting of a Template:Solar mass companion and itself.<ref name = Tokovinin2008/> The system is located approximately 700 light years away.<ref name = GaiaDR3A>Template:Cite DR3</ref><ref name = GaiaDR3B>Template:Cite DR3</ref> The outer pair has a separation of 6.8" and both stars take roughly 23,000 years to orbit each other while the B subsystem takes 1,528 days to circle each other in a relatively eccentric orbit.<ref name = Tokovinin2007>Template:Cite journal</ref>

There are a few notable variable stars, including 25, 23 Sextantis, and LHS 292. NGC 3115, an edge-on lenticular galaxy, is the only noteworthy deep-sky object. It also lies near the ecliptic, which causes the Moon, and some of the planets to occasionally pass through it for brief periods of time.

The constellation is the location of the field studied by the COSMOS project, undertaken by the Hubble Space Telescope.

COSMOS projectEdit

Sextans B is a fairly bright dwarf irregular galaxy at magnitude 6.6, 4.3 million light-years from Earth. It is part of the Local Group of galaxies.Template:Sfn

CL J1001+0220 is as of 2016 the most distant-known galaxy cluster at redshift z=2.506, 11.1 billion light-years from Earth.<ref name=AJ-828-1>Template:Cite journal</ref>

In June 2015, astronomers reported evidence for population III stars in the Cosmos Redshift 7 galaxy (at z = 6.60) found in Sextans. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.<ref name="AJ-20150604">Template:Cite journal</ref><ref name="NYT-20150617">Template:Cite news</ref>

Depictions of the constellationEdit

ReferencesEdit

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Template:Cite book
Ian Ridpath and Wil Tirion (2007). Stars and Planets Guide, Collins, London. Template:ISBN. Princeton University Press, Princeton. Template:ISBN.