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* [[Capricornus (constellation)|Capricornus]]
* [[Capricornus (constellation)|Capricornus]]
* [[Sagittarius (constellation)|Sagittarius]]
* [[Sagittarius (constellation)|Sagittarius]]
* [[Telescopium]](Corner)
* [[Telescopium]] (corner)
* [[Indus (constellation)|Indus]]
* [[Indus (constellation)|Indus]]
* [[Grus (constellation)|Grus]]
* [[Grus (constellation)|Grus]]
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| month = September
| month = September
| notes=}}
| notes=}}
'''Microscopium''' {{IPAc-en|ˌ|m|aɪ|k|r|ə|ˈ|s|k|ɒ|p|i|əm}} ("the [[Microscope]]") is a minor [[constellation]] in the [[southern celestial hemisphere]], one of twelve created in the 18th century by French [[astronomer]] [[Nicolas-Louis de Lacaille]] and one of several depicting scientific instruments. The name is a [[Latin]]ised form of the [[Ancient Greek|Greek]] word for [[microscope]]. Its [[star]]s are faint and hardly visible from most of the non-tropical [[Northern Hemisphere]].
'''Microscopium''' ("the [[Microscope]]") is a minor [[constellation]] in the [[southern celestial hemisphere]], one of twelve created in the 18th century by French [[astronomer]] [[Nicolas-Louis de Lacaille]] and one of several depicting scientific instruments. The name is a [[Latin]]ised form of the [[Ancient Greek|Greek]] word for [[microscope]]. Its [[star]]s are faint and hardly visible from most of the non-tropical [[Northern Hemisphere]].


The constellation's brightest star is [[Gamma Microscopii]] of [[apparent magnitude]] 4.68, a yellow giant 2.5 times the Sun's mass located 223 ± 8 light-years distant. It passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, possibly disturbing the outer Solar System. Two star systems—[[WASP-7]] and [[HD 205739]]—have been determined to have [[exoplanet|planets]], while two others—the young [[red dwarf]] star [[AU Microscopii]] and the sunlike [[HD 202628]]—have [[debris disk]]s. AU Microscopii and the binary red dwarf system [[AT Microscopii]] are probably a wide triple system and members of the [[Beta Pictoris moving group]]. Nicknamed "Speedy Mic", [[BO Microscopii]] is a star with an extremely fast rotation period of 9 hours, 7 minutes.
The constellation's brightest star is [[Gamma Microscopii]] of [[apparent magnitude]] 4.68, a yellow giant 2.5 times the Sun's mass located 223 ± 8 light-years distant. It passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, possibly disturbing the outer Solar System. Three star systems—[[WASP-7]], [[AU Microscopii]] and [[HD 205739]]—have been determined to have [[exoplanet|planets]], while other star —the Sun-like star [[HD 202628]]— has a [[debris disk]]. AU Microscopii and the binary red dwarf system [[AT Microscopii]] are probably a wide triple system and members of the [[Beta Pictoris moving group]]. Nicknamed "Speedy Mic", [[BO Microscopii]] is a star with an extremely fast rotation period of 9 hours, 7 minutes.


==Characteristics==
==Characteristics==
Microscopium is a small constellation bordered by a big brolic man [[Capricornus]] to the north, [[Piscis Austrinus]] and [[Grus (constellation)|Grus]] to the east, [[Sagittarius (constellation)|Sagittarius]] to the west, and [[Indus (constellation)|Indus]] to the south, touching on [[Telescopium]] to the southwest. The recommended three-letter abbreviation for the constellation, as adopted by the [[International Astronomical Union]] in 1922, is "Mic".<ref name=pa30_469>{{cite magazine | last=Russell | first=Henry Norris |author-link=Henry Norris Russell | title=The new international symbols for the constellations | magazine=[[Popular Astronomy (US magazine)|Popular Astronomy]] | volume=30 | page=469 | bibcode=1922PA.....30..469R | date=1922 }}</ref> The official constellation boundaries, as set by Belgian astronomer [[Eugène Joseph Delporte|Eugène Delporte]] in 1930, are defined by a polygon of four segments (''illustrated in infobox''). In the [[equatorial coordinate system]], the [[right ascension]] coordinates of these borders lie between {{RA|20|27.3}} and {{RA|21|28.4}}, while the [[declination]] coordinates are between −27.45° and −45.09°.<ref name=boundary>{{Cite journal | title=Microscopium, constellation boundary | journal=The Constellations| url=http://www.iau.org/public/constellations/#mic | access-date=13 July 2012 }}</ref> The whole constellation is visible to observers south of latitude [[45th parallel north|45°N]].<ref name=tirionconst>{{cite web| url=http://www.ianridpath.com/constellations2.htm | title=Constellations: Lacerta–Vulpecula | work= Star Tales |author=Ian Ridpath|publisher=Self-published | access-date= 29 November 2014| author-link=Ian Ridpath }}</ref>{{efn|1=While parts of the constellation technically rise above the horizon to observers between 45°N and [[62nd parallel north|62°N]], stars within a few degrees of the horizon are to all intents and purposes unobservable.<ref name=tirionconst/>}} Given that its brightest stars are of fifth magnitude, the constellation is invisible to the naked eye in areas with light polluted skies.<ref>{{cite book |last=Kambič |first=Bojan |title=Viewing the Constellations with Binoculars |publisher=Springer |date=2009 |page=341 |isbn=978-0-387-85354-3 |url=https://books.google.com/books?id=3vxLNPNHOcwC&pg=PA340}}</ref>{{efn|1=Objects of magnitude 5.0 are barely visible to the unaided eye in the night skies of city-suburban transition areas.<ref name=bortle/>}}
Microscopium is a small constellation bordered by [[Capricornus]] to the north, [[Piscis Austrinus]] and [[Grus (constellation)|Grus]] to the east, [[Sagittarius (constellation)|Sagittarius]] to the west, and [[Indus (constellation)|Indus]] to the south, touching on [[Telescopium]] to the southwest. The recommended three-letter abbreviation for the constellation, as adopted by the [[International Astronomical Union]] in 1922, is "Mic".<ref name=pa30_469>{{cite magazine | last=Russell | first=Henry Norris |author-link=Henry Norris Russell | title=The new international symbols for the constellations | magazine=[[Popular Astronomy (US magazine)|Popular Astronomy]] | volume=30 | page=469 | bibcode=1922PA.....30..469R | date=1922 }}</ref> The official constellation boundaries, as set by Belgian astronomer [[Eugène Joseph Delporte|Eugène Delporte]] in 1930, are defined by a polygon of four segments (''illustrated in infobox''). In the [[equatorial coordinate system]], the [[right ascension]] coordinates of these borders lie between {{RA|20|27.3}} and {{RA|21|28.4}}, while the [[declination]] coordinates are between −27.45° and −45.09°.<ref name=boundary>{{Cite journal | title=Microscopium, constellation boundary | journal=The Constellations| url=https://www.iau.org/public/themes/constellations/#mic | access-date=13 July 2012 }}</ref> The whole constellation is visible to observers south of latitude [[45th parallel north|45°N]].<ref name=tirionconst>{{cite web| url=http://www.ianridpath.com/constellations2.html | title=Constellations: Lacerta–Vulpecula | work= Star Tales |author=Ian Ridpath|publisher=Self-published | access-date= 29 November 2014| author-link=Ian Ridpath }}</ref>{{efn|1=While parts of the constellation technically rise above the horizon to observers between 45°N and [[62nd parallel north|62°N]], stars within a few degrees of the horizon are to all intents and purposes unobservable.<ref name=tirionconst/>}} Given that its brightest stars are of fifth magnitude, the constellation is invisible to the naked eye in areas with light polluted skies.<ref>{{cite book |last=Kambič |first=Bojan |title=Viewing the Constellations with Binoculars |publisher=Springer |date=2009 |page=341 |isbn=978-0-387-85354-3 |url=https://books.google.com/books?id=3vxLNPNHOcwC&pg=PA340}}</ref>{{efn|1=Objects of magnitude 5.0 are barely visible to the unaided eye in the night skies of city-suburban transition areas.<ref name=bortle/>}}


==Features==
==Features==
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===Stars===
===Stars===
{{See also|List of stars in Microscopium}}
{{See also|List of stars in Microscopium}}
French astronomer [[Nicolas-Louis de Lacaille]] charted and designated ten stars with the [[Bayer designation]]s [[Alpha Microscopii|Alpha]] through to [[Iota Microscopii|Iota]] in 1756. A star in neighbouring Indus that Lacaille had labelled Nu Indi turned out to be in Microscopium, so Gould renamed it [[Nu Microscopii]]. [[Francis Baily]] considered Gamma and Epsilon Microscopii to belong to the neighbouring constellation Piscis Austrinus, but subsequent cartographers did not follow this.{{sfn|Wagman|2003|pp=181, 210}} In his 1725 ''Catalogus Britannicus'', John Flamsteed labelled the stars 1, 2, 3 and 4 Piscis Austrini, which became Gamma Microscopii, [[2 Piscis Austrini|HR 8076]], [[3 Piscis Austrini|HR 8110]] and Epsilon Microscopii respectively.{{sfn|Wagman|2003|p=458}}<!-- cites previous 4 sentences --> Within the constellation's borders, there are 43 stars brighter than or equal to [[apparent magnitude]]&nbsp;6.5.{{efn|1=Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.<ref name=bortle>{{cite web|url=http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|title=The Bortle Dark-Sky Scale|last=Bortle|first=John E.|date=February 2001|work=[[Sky & Telescope]]|publisher=Sky Publishing Corporation|access-date=29 November 2014}}</ref>}}<ref name=tirionconst/>
French astronomer [[Nicolas-Louis de Lacaille]] charted and designated ten stars with the [[Bayer designation]]s [[Alpha Microscopii|Alpha]] through to [[Iota Microscopii|Iota]] in 1756. A star in neighbouring Indus that Lacaille had labelled Nu Indi turned out to be in Microscopium, so Gould renamed it [[Nu Microscopii]]. [[Francis Baily]] considered Gamma and Epsilon Microscopii to belong to the neighbouring constellation Piscis Austrinus, but subsequent cartographers did not follow this.{{sfn|Wagman|2003|pp=181, 210}} In his 1725 ''Catalogus Britannicus'', John Flamsteed labelled the stars 1, 2, 3 and 4 Piscis Austrini, which became Gamma Microscopii, [[2 Piscis Austrini|HR 8076]], [[3 Piscis Austrini|HR 8110]] and Epsilon Microscopii respectively.{{sfn|Wagman|2003|p=458}}<!-- cites previous 4 sentences --> Within the constellation's borders, there are 43 stars brighter than or equal to [[apparent magnitude]]&nbsp;6.5.{{efn|1=Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.<ref name=bortle>{{cite web|url=http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|title=The Bortle Dark-Sky Scale|last=Bortle|first=John E.|date=February 2001|work=[[Sky & Telescope]]|publisher=Sky Publishing Corporation|access-date=29 November 2014|archive-date=16 December 2012|archive-url=https://archive.today/20121216144730/http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|url-status=dead}}</ref>}}<ref name=tirionconst/>


Depicting the eyepiece of the microscope is [[Gamma Microscopii]],<ref name="motz">{{cite book|last=Motz|first=Lloyd|author2=Nathanson, Carol|title=The Constellations: An Enthusiast's Guide to the Night Sky|publisher=Aurum Press|location=London|date=1991|pages=369–370|isbn=978-1-85410-088-7}}</ref> which—at magnitude of&nbsp;4.68—is the brightest star in the constellation. Having spent much of its 620-million-year lifespan as a blue-white [[main sequence]] star, it has swollen and cooled to become a yellow [[giant star|giant]] of [[Stellar classification#Spectral types|spectral type]] G6III, with a diameter ten times that of the Sun.<ref name=kalergamma>{{cite web| url=http://stars.astro.illinois.edu/sow/gammamic.html |title=Gamma Mic |work=Stars |author= Kaler, James B. |access-date=13 July 2012}}</ref> Measurement of its parallax yields a distance of 223 ± 8 light years from Earth.<ref name=Gaia-DR2gamma>{{cite DR2|6781898461559620480}}</ref> It likely passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, at around 2.5 times the mass of the Sun, it is possibly massive enough and close enough to disturb the [[Oort cloud]].<ref name=aa575_A35>{{cite journal | last1=Bailer-Jones | first1=C.A.L. | title=Close encounters of the stellar kind | journal=Astronomy & Astrophysics | volume=575 | id=A35 | pages=13 | date=2015 | doi=10.1051/0004-6361/201425221 | bibcode=2015A&A...575A..35B |arxiv = 1412.3648 | s2cid=59039482 }}</ref> [[Alpha Microscopii]] is also an ageing yellow giant star of spectral type G7III with an apparent magnitude of 4.90.<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Alpha+Microscopii&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Alpha MicroscopiI |publisher = SIMBAD |access-date = 15 July 2012}}</ref> Located 400 ± 30 light-years away from Earth,<ref name=Gaia-DR2alpha>{{cite DR2|6780006508937236096}}</ref> it has swollen to 17.5&nbsp;times the diameter of the Sun.<ref name=kaleralfa>{{cite web| url=http://stars.astro.illinois.edu/sow/alphamic.html|title=Alpha Mic |work=Stars |author= Kaler, James B. |access-date=19 March 2015}}</ref> Alpha has a 10th magnitude companion, visible in 7.5&nbsp;cm telescopes,<ref>{{cite book |author1=Malin, David |author2=Frew, David J. | title = Hartung's Astronomical Objects for Southern Telescopes, with an Addendum for Northern Observatories: A Handbook for Amateur Observers | publisher = Cambridge University Press |year=1995 |location= Cambridge |page=287 | url=https://books.google.com/books?id=EQAYGmZT0o8C&pg=PA287 |isbn=978-0-521-55491-6}}</ref><ref name=ridpath07>{{cite book|author=Ridpath, Ian |author2=Tirion, Wil |date=2007 |title=Stars and Planets Guide|publisher= Princeton University Press|location= Princeton, New Jersey |isbn=978-0-691-13556-4|pages=184–185}}</ref> though this is a coincidental closeness rather than a true binary system.<ref name=kaleralfa/> [[Epsilon Microscopii]] lies 166 ± 5 light-years away,<ref name=Gaia-DR2eps>{{cite DR2|6784024126773616128}}</ref> and is a white star of apparent magnitude 4.7,<ref name=ridpath07/> and spectral type A1V.<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Epsilon+Microscopii&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Epsilon Microscopii |publisher = SIMBAD |access-date = 15 July 2012}}</ref> [[Theta1 Microscopii|Theta<sup>1</sup>]] and [[Theta2 Microscopii|Theta<sup>2</sup> Microscopii]] make up a wide double whose components are splittable to the naked eye. Both are white A-class [[Alpha² Canum Venaticorum variable|magnetic spectrum variable stars]] with strong metallic lines, similar to [[Cor Caroli]]. They mark the constellation's specimen slide.<ref name="motz"/>
Depicting the eyepiece of the microscope is [[Gamma Microscopii]],<ref name="motz">{{cite book|last=Motz|first=Lloyd|author2=Nathanson, Carol|title=The Constellations: An Enthusiast's Guide to the Night Sky|publisher=Aurum Press|location=London|date=1991|pages=369–370|isbn=978-1-85410-088-7}}</ref> which—at magnitude of&nbsp;4.68—is the brightest star in the constellation. Having spent much of its 620-million-year lifespan as a blue-white [[main sequence]] star, it has swollen and cooled to become a yellow [[giant star|giant]] of [[Stellar classification#Spectral types|spectral type]] G6III, with a diameter ten times that of the Sun.<ref name=kalergamma>{{cite web| url=http://stars.astro.illinois.edu/sow/gammamic.html |title=Gamma Mic |work=Stars |author= Kaler, James B. |access-date=13 July 2012}}</ref> Measurement of its parallax yields a distance of 223 ± 8 light years from Earth.<ref name=Gaia-DR2gamma>{{cite DR2|6781898461559620480}}</ref> It likely passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, at around 2.5 times the mass of the Sun, it is possibly massive enough and close enough to disturb the [[Oort cloud]].<ref name=aa575_A35>{{cite journal | last1=Bailer-Jones | first1=C.A.L. | title=Close encounters of the stellar kind | journal=Astronomy & Astrophysics | volume=575 | id=A35 | pages=13 | date=2015 | doi=10.1051/0004-6361/201425221 | bibcode=2015A&A...575A..35B |arxiv = 1412.3648 | s2cid=59039482 }}</ref> [[Alpha Microscopii]] is also an ageing yellow giant star of spectral type G7III with an apparent magnitude of 4.90.<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Alpha+Microscopii&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Alpha MicroscopiI |publisher = SIMBAD |access-date = 15 July 2012}}</ref> Located 400 ± 30 light-years away from Earth,<ref name=Gaia-DR2alpha>{{cite DR2|6780006508937236096}}</ref> it has swollen to 17.5&nbsp;times the diameter of the Sun.<ref name=kaleralfa>{{cite web| url=http://stars.astro.illinois.edu/sow/alphamic.html|title=Alpha Mic |work=Stars |author= Kaler, James B. |access-date=19 March 2015}}</ref> Alpha has a 10th magnitude companion, visible in 7.5&nbsp;cm telescopes,<ref>{{cite book |author1=Malin, David |author2=Frew, David J. | title = Hartung's Astronomical Objects for Southern Telescopes, with an Addendum for Northern Observatories: A Handbook for Amateur Observers | publisher = Cambridge University Press |year=1995 |location= Cambridge |page=287 | url=https://books.google.com/books?id=EQAYGmZT0o8C&pg=PA287 |isbn=978-0-521-55491-6}}</ref><ref name=ridpath07>{{cite book|author=Ridpath, Ian |author2=Tirion, Wil |date=2007 |title=Stars and Planets Guide|publisher= Princeton University Press|location= Princeton, New Jersey |isbn=978-0-691-13556-4|pages=184–185}}</ref> though this is a coincidental closeness rather than a true binary system.<ref name=kaleralfa/> [[Epsilon Microscopii]] lies 166 ± 5 light-years away,<ref name=Gaia-DR2eps>{{cite DR2|6784024126773616128}}</ref> and is a white star of apparent magnitude 4.7,<ref name=ridpath07/> and spectral type A1V.<ref>{{cite web |url = http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Epsilon+Microscopii&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id |title = Epsilon Microscopii |publisher = SIMBAD |access-date = 15 July 2012}}</ref> [[Theta1 Microscopii|Theta<sup>1</sup>]] and [[Theta2 Microscopii|Theta<sup>2</sup> Microscopii]] make up a wide double whose components are splittable to the naked eye. Both are white A-class [[Alpha² Canum Venaticorum variable|magnetic spectrum variable stars]] with strong metallic lines, similar to [[Cor Caroli]]. They mark the constellation's specimen slide.<ref name="motz"/>


Many notable objects are too faint to be seen with the naked eye. AX Microscopii, better known as [[Lacaille 8760]], is a [[red dwarf]] which lies only 12.9&nbsp;light-years from the [[Solar System]]. At magnitude 6.68, it is the brightest red dwarf in the sky.<ref name=st200307>{{cite magazine | first1=Ken | last1=Croswell |date=July 2002 | page=32 | title=The Brightest Red Dwarf | magazine=Sky & Telescope | url=http://www.kencroswell.com/thebrightestreddwarf.html | access-date=15 July 2012}}</ref> [[BO Microscopii]] is a rapidly rotating star that has 80% the diameter of the Sun. Nicknamed "Speedy Mic", it has a rotation period of 9&nbsp;hours 7&nbsp;minutes.<ref name=mnras365_2_530>{{cite journal | last1=Dunstone | first1=N.J. | last2=Barnes | first2=J.R. | last3=Collier Cameron | first3=A. | last4=Jardine | first4=M. | title=The coronal structure of Speedy Mic – I. A densely packed prominence system beyond corotation | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=365 | issue=2 | pages=530–538 |date=2006 | doi=10.1111/j.1365-2966.2005.09729.x | bibcode=2006MNRAS.365..530D |arxiv = astro-ph/0510739 | s2cid=11048210 }}</ref> An active star, it has prominent [[solar flare|stellar flares]] that average 100&nbsp;times stronger than those of the Sun, and are emitting energy mainly in the X-ray and ultraviolet bands of the spectrum.<ref name=aaa478_1_L11>{{cite journal | last1=Wolter | first1=U. | last2=Robrade | first2=J. | last3=Schmitt | first3=J.H.M.M. | last4=Ness | first4=J.U. | title=Doppler imaging an X-ray flare on the ultrafast rotator BO Mic. A contemporaneous multiwavelength study using XMM-Newton and VLT | journal=Astronomy and Astrophysics | volume=478 | issue=1 | pages=L11–L14 |date=2008 | doi=10.1051/0004-6361:20078838 | bibcode=2008A&A...478L..11W |arxiv = 0712.0899 | s2cid=62827486 }}</ref> It lies 218 ± 4 light-years away from the Sun.<ref name=Gaia-DR2bo>{{cite DR2|6778413151435607680}}</ref> [[AT Microscopii]] is a binary star system, both members of which are flare star red dwarfs. The system lies close to and may form a very wide triple system with [[AU Microscopii]],<ref name="Caballero2009">{{cite journal| last1 = Caballero | first1 = J.A. |date=November 2009 | title = Reaching the boundary between stellar kinematic groups and very wide binaries. The Washington double stars with the widest angular separations
Many notable objects are too faint to be seen with the naked eye. AX Microscopii, better known as [[Lacaille 8760]], is a [[red dwarf]] which lies only 12.9&nbsp;light-years from the [[Solar System]]. At magnitude 6.68, it is the brightest red dwarf in the sky.<ref name=st200307>{{cite magazine | first1=Ken | last1=Croswell |date=July 2002 | page=32 | title=The Brightest Red Dwarf | magazine=Sky & Telescope | url=http://www.kencroswell.com/thebrightestreddwarf.html | access-date=15 July 2012}}</ref> [[BO Microscopii]] is a rapidly rotating star that has 80% the diameter of the Sun. Nicknamed "Speedy Mic", it has a rotation period of 9&nbsp;hours 7&nbsp;minutes.<ref name=mnras365_2_530>{{cite journal | last1=Dunstone | first1=N.J. | last2=Barnes | first2=J.R. | last3=Collier Cameron | first3=A. | last4=Jardine | first4=M. | title=The coronal structure of Speedy Mic – I. A densely packed prominence system beyond corotation | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=365 | issue=2 | pages=530–538 |date=2006 | doi=10.1111/j.1365-2966.2005.09729.x | doi-access=free | bibcode=2006MNRAS.365..530D |arxiv = astro-ph/0510739 | s2cid=11048210 }}</ref> An active star, it has prominent [[solar flare|stellar flares]] that average 100&nbsp;times stronger than those of the Sun, and are emitting energy mainly in the X-ray and ultraviolet bands of the spectrum.<ref name=aaa478_1_L11>{{cite journal | last1=Wolter | first1=U. | last2=Robrade | first2=J. | last3=Schmitt | first3=J.H.M.M. | last4=Ness | first4=J.U. | title=Doppler imaging an X-ray flare on the ultrafast rotator BO Mic. A contemporaneous multiwavelength study using XMM-Newton and VLT | journal=Astronomy and Astrophysics | volume=478 | issue=1 | pages=L11–L14 |date=2008 | doi=10.1051/0004-6361:20078838 | bibcode=2008A&A...478L..11W |arxiv = 0712.0899 | s2cid=62827486 }}</ref> It lies 218 ± 4 light-years away from the Sun.<ref name=Gaia-DR2bo>{{cite DR2|6778413151435607680}}</ref> [[AT Microscopii]] is a binary star system, both members of which are flare star red dwarfs. The system lies close to and may form a very wide triple system with [[AU Microscopii]],<ref name="Caballero2009">{{cite journal| last1 = Caballero | first1 = J.A. |date=November 2009 | title = Reaching the boundary between stellar kinematic groups and very wide binaries. The Washington double stars with the widest angular separations
| journal = Astronomy and Astrophysics | volume = 507 | issue = 1 | pages = 251–259 | bibcode = 2009A&A...507..251C | doi = 10.1051/0004-6361/200912596 | arxiv = 0908.2761| s2cid = 118194112 }}</ref> a young star which appears to be a [[planetary system]] in the making with a [[debris disk]]. The three stars are candidate members of the [[Beta Pictoris moving group]], one of the nearest [[Stellar kinematics|associations of stars]] that share a common motion through space.<ref name="McCarthyWhite2012">{{cite journal | last1 = McCarthy | first1 = Kyle | last2 = White | first2 = Russel J. |date=2012 | title = The Sizes of the Nearest Young Stars | journal = [[The Astronomical Journal]] | volume = 143 | issue = 6 | pages = 134–168 | bibcode = 2012AJ....143..134M | doi = 10.1088/0004-6256/143/6/134 | arxiv = 1201.6600| s2cid = 118538522 }}</ref>
| journal = Astronomy and Astrophysics | volume = 507 | issue = 1 | pages = 251–259 | bibcode = 2009A&A...507..251C | doi = 10.1051/0004-6361/200912596 | arxiv = 0908.2761| s2cid = 118194112 }}</ref> a young star which has a [[planetary system]] in the making with a [[debris disk]]. The three stars are candidate members of the [[Beta Pictoris moving group]], one of the nearest [[Stellar kinematics|associations of stars]] that share a common motion through space.<ref name="McCarthyWhite2012">{{cite journal | last1 = McCarthy | first1 = Kyle | last2 = White | first2 = Russel J. |date=2012 | title = The Sizes of the Nearest Young Stars | journal = [[The Astronomical Journal]] | volume = 143 | issue = 6 | pages = 134–168 | bibcode = 2012AJ....143..134M | doi = 10.1088/0004-6256/143/6/134 | arxiv = 1201.6600| s2cid = 118538522 }}</ref>


The [[Astronomical Society of Southern Africa]] in 2003 reported that observations of four of the [[Mira variable]]s in Microscopium were very urgently needed as data on their light curves was incomplete.<ref name=cooper>{{cite journal|last=Cooper|first=Tim|date=2003|title=Presidential address: Amateur Observations – Successes and Opportunities|journal=Monthly Notes of the Astronomical Society of Southern Africa|volume=62|pages=234–240|bibcode=2003MNSSA..62..234C}}</ref> Two of them—[[R Microscopii|R]] and [[S Microscopii]]—are challenging stars for novice amateur astronomers,<ref>{{cite book |last=Levy |first=David H. |title=Observing Variable Stars: A Guide for the Beginner |publisher=Cambridge University Press |location=Cambridge |date=1998 |pages=172 |isbn=978-0-521-62755-9 |url=https://books.google.com/books?id=5-O2cd937FMC&pg=PA172}}</ref> and the other two, [[U Microscopii|U]] and [[RY Microscopii]], are more difficult still.<ref name=cooper/> Another red giant, [[T Microscopii]], is a [[Semiregular variable star|semiregular variable]] that ranges between magnitudes 7.7 and 9.6 over 344 days.<ref>{{cite book |authors=Arnold, H.J.P; Doherty, Paul; Moore, Patrick |title=The Photographic Atlas of the Stars |publisher=CRC Press |location=Boca Raton, Florida |date=1999 |page=53 |isbn=978-0-7503-0654-6 |url=https://books.google.com/books?id=YjcvJUfnWBAC&pg=PA148}}</ref> Of apparent magnitude 11, [[DD Microscopii]] is a [[symbiotic star]] system composed of an orange giant of spectral type K2III and [[white dwarf]] in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system has a low [[metallicity]]. Combined with its high galactic latitude, this indicates that the star system has its origin in the [[galactic halo]] of the [[Milky Way]].<ref name=pereira2009>{{cite journal |title=High-Resolution Spectroscopic Observations of Four Yellow-Type Symbiotic Stars: CD-43°14304, Hen 3-1213, Hen 3-863, and StHα 176 |authors=Pereira, C.B.; Roig, F. |journal=The Astronomical Journal |volume=137 |issue=1 |pages=118–128 |year=2009 |doi=10.1088/0004-6256/137/1/118 |bibcode=2009AJ....137..118P|doi-access=free }}</ref>
The [[Astronomical Society of Southern Africa]] in 2003 reported that observations of four of the [[Mira variable]]s in Microscopium were very urgently needed as data on their light curves was incomplete.<ref name=cooper>{{cite journal|last=Cooper|first=Tim|date=2003|title=Presidential address: Amateur Observations – Successes and Opportunities|journal=Monthly Notes of the Astronomical Society of Southern Africa|volume=62|pages=234–240|bibcode=2003MNSSA..62..234C}}</ref> Two of them—[[R Microscopii|R]] and [[S Microscopii]]—are challenging stars for novice amateur astronomers,<ref>{{cite book |last=Levy |first=David H. |title=Observing Variable Stars: A Guide for the Beginner |publisher=Cambridge University Press |location=Cambridge |date=1998 |pages=172 |isbn=978-0-521-62755-9 |url=https://books.google.com/books?id=5-O2cd937FMC&pg=PA172}}</ref> and the other two, [[U Microscopii|U]] and [[RY Microscopii]], are more difficult still.<ref name=cooper/> Another red giant, [[T Microscopii]], is a [[Semiregular variable star|semiregular variable]] that ranges between magnitudes 7.7 and 9.6 over 344 days.<ref>{{cite book |author1=Arnold, H.J.P |author2=Doherty, Paul |author3=Moore, Patrick |title=The Photographic Atlas of the Stars |publisher=CRC Press |location=Boca Raton, Florida |date=1999 |page=53 |isbn=978-0-7503-0654-6 |url=https://books.google.com/books?id=YjcvJUfnWBAC&pg=PA148}}</ref> Of apparent magnitude 11, [[DD Microscopii]] is a [[symbiotic star]] system composed of an orange giant of spectral type K2III and [[white dwarf]] in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system has a low [[metallicity]]. Combined with its high galactic latitude, this indicates that the star system has its origin in the [[galactic halo]] of the [[Milky Way]].<ref name=pereira2009>{{cite journal |title=High-Resolution Spectroscopic Observations of Four Yellow-Type Symbiotic Stars: CD-43°14304, Hen 3-1213, Hen 3-863, and StHα 176 |author1=Pereira, C.B. |author2=Roig, F. |journal=The Astronomical Journal |volume=137 |issue=1 |pages=118–128 |year=2009 |doi=10.1088/0004-6256/137/1/118 |bibcode=2009AJ....137..118P|doi-access=free }}</ref>


[[HD 205739]] is a yellow-white main sequence star of spectral type F7V that is around 1.22&nbsp;times as massive and 2.3&nbsp;times as luminous as the Sun. It has a Jupiter-sized planet with an orbital period of 280&nbsp;days that was discovered by the [[methods of detecting extrasolar planets#Radial velocity|radial velocity]] method.<ref name="LopezMorales2008">{{cite journal | title=Two Jupiter-Mass Planets Orbiting HD 154672 and HD 205739 | last1=López-Morales | first1=Mercedes | last2=Butler | first2=R. Paul | last3=Fischer | first3=Debra A. | last4=Minniti | first4=Dante | last5=Shectman | first5=Stephen A. | last6=Takeda | first6=Genya | last7=Adams | first7=Fred C. | last8=Wright | first8=Jason T. | last9=Arriagada | first9=Pamela | journal=The Astronomical Journal | volume=136 | issue=5 | pages=1901–1905 | date=2008 | arxiv=0809.1037 | bibcode=2008AJ....136.1901L | doi=10.1088/0004-6256/136/5/1901 | s2cid=119242543 }}</ref> [[WASP-7]] is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28&nbsp;times as massive as the Sun. Its [[hot Jupiter]] planet—[[WASP-7b]]—was discovered by [[Methods of detecting extrasolar planets#Transit method|transit method]] and found to orbit the star every 4.95&nbsp;days.<ref name="disc">{{ cite journal| title=Wasp-7: A Bright Transiting-Exoplanet System in the Southern Hemisphere| last1=Hellier|first1=Coel| date= 2008 | journal=The Astrophysical Journal Letters| volume=690| issue=1| pages=L89–L91| doi=10.1088/0004-637X/690/1/L89| last2=Anderson| first2=D.R.| last3=Gillon| first3=M.| last4=Lister| first4=T.A.| last5=Maxted| first5=P.F.L.| last6=Queloz| first6=D.| last7=Smalley| first7=B.| last8=Triaud| first8=A.H.M.J.| last9=West| first9=R.G. | last10=Wilson| first10=D.M.| last11=Alsubai| first11=K.| last12=Bentley| first12=S.J.| last13=Cameron| first13=A. Collier| last14=Hebb| first14=L.| last15=Horne| first15=K.| last16=Irwin| first16=J.| last17=Kane| first17=S.R.| last18=Mayor| first18=M.| last19=Pepe| first19=F.| last20=Pollacco| first20=D.| last21=Skillen| first21=I.| last22=Udry| first22=S.| last23=Wheatley| first23=P.J.| last24=Christian| first24=D.J.| last25=Enoch| first25=R.| last26=Haswell| first26=C.A.| last27=Joshi| first27=Y.C.| last28=Norton| first28=A.J.| last29=Parley| first29=N.| last30=Ryans| first30=R.| bibcode=2009ApJ...690L..89H|arxiv = 0805.2600 | s2cid=15962609}}</ref> [[HD 202628]] is a sunlike star of spectral type G2V with a debris disk that ranges from 158 to 220 AU distant. Its inner edge is sharply defined, indicating a probable planet orbiting between 86 and 158&nbsp;AU from the star.<ref name=nesvold>{{cite journal|author1=Nesvold, Erika R. |author2=Kuchner, Marc J. |date=2015|title=Gap Clearing by Planets in a Collisional Debris Disk|journal=The Astrophysical Journal|volume=798|issue=2 |id=83|page=10|doi= 10.1088/0004-637X/798/2/83 |bibcode=2015ApJ...798...83N|arxiv = 1410.7784 |s2cid=118667155 }}</ref>
[[HD 205739]] is a yellow-white main sequence star of spectral type F7V that is around 1.22&nbsp;times as massive and 2.3&nbsp;times as luminous as the Sun. It has a Jupiter-sized planet with an orbital period of 280&nbsp;days that was discovered by the [[methods of detecting extrasolar planets#Radial velocity|radial velocity]] method.<ref name="LopezMorales2008">{{cite journal | title=Two Jupiter-Mass Planets Orbiting HD 154672 and HD 205739 | last1=López-Morales | first1=Mercedes | last2=Butler | first2=R. Paul | last3=Fischer | first3=Debra A. | last4=Minniti | first4=Dante | last5=Shectman | first5=Stephen A. | last6=Takeda | first6=Genya | last7=Adams | first7=Fred C. | last8=Wright | first8=Jason T. | last9=Arriagada | first9=Pamela | journal=The Astronomical Journal | volume=136 | issue=5 | pages=1901–1905 | date=2008 | arxiv=0809.1037 | bibcode=2008AJ....136.1901L | doi=10.1088/0004-6256/136/5/1901 | s2cid=119242543 }}</ref> [[WASP-7]] is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28&nbsp;times as massive as the Sun. Its [[hot Jupiter]] planet—[[WASP-7b]]—was discovered by [[Methods of detecting extrasolar planets#Transit method|transit method]] and found to orbit the star every 4.95&nbsp;days.<ref name="disc">{{ cite journal| title=Wasp-7: A Bright Transiting-Exoplanet System in the Southern Hemisphere| last1=Hellier|first1=Coel| date= 2008 | journal=The Astrophysical Journal Letters| volume=690| issue=1| pages=L89–L91| doi=10.1088/0004-637X/690/1/L89| last2=Anderson| first2=D.R.| last3=Gillon| first3=M.| last4=Lister| first4=T.A.| last5=Maxted| first5=P.F.L.| last6=Queloz| first6=D.| last7=Smalley| first7=B.| last8=Triaud| first8=A.H.M.J.| last9=West| first9=R.G. | last10=Wilson| first10=D.M.| last11=Alsubai| first11=K.| last12=Bentley| first12=S.J.| last13=Cameron| first13=A. Collier| last14=Hebb| first14=L.| last15=Horne| first15=K.| last16=Irwin| first16=J.| last17=Kane| first17=S.R.| last18=Mayor| first18=M.| last19=Pepe| first19=F.| last20=Pollacco| first20=D.| last21=Skillen| first21=I.| last22=Udry| first22=S.| last23=Wheatley| first23=P.J.| last24=Christian| first24=D.J.| last25=Enoch| first25=R.| last26=Haswell| first26=C.A.| last27=Joshi| first27=Y.C.| last28=Norton| first28=A.J.| last29=Parley| first29=N.| last30=Ryans| first30=R.| bibcode=2009ApJ...690L..89H|arxiv = 0805.2600 | s2cid=15962609}}</ref> [[HD 202628]] is a sunlike star of spectral type G2V with a debris disk that ranges from 158 to 220 AU distant. Its inner edge is sharply defined, indicating a probable planet orbiting between 86 and 158&nbsp;AU from the star.<ref name=nesvold>{{cite journal|author1=Nesvold, Erika R. |author2=Kuchner, Marc J. |date=2015|title=Gap Clearing by Planets in a Collisional Debris Disk|journal=The Astrophysical Journal|volume=798|issue=2 |id=83|page=10|doi= 10.1088/0004-637X/798/2/83 |bibcode=2015ApJ...798...83N|arxiv = 1410.7784 |s2cid=118667155 }}</ref>
Line 62: Line 62:
===Deep sky objects===
===Deep sky objects===
[[File:Arp-Madore 2026-424.tif|thumb|[[Arp-Madore 2026-424]] taken by Hubble.<ref>{{cite web |title=Hubble Captures Cosmic Face |url=https://www.spacetelescope.org/news/heic1919/ |website=www.spacetelescope.org |access-date=31 October 2019 |language=en}}</ref>]]
[[File:Arp-Madore 2026-424.tif|thumb|[[Arp-Madore 2026-424]] taken by Hubble.<ref>{{cite web |title=Hubble Captures Cosmic Face |url=https://www.spacetelescope.org/news/heic1919/ |website=www.spacetelescope.org |access-date=31 October 2019 |language=en}}</ref>]]
Describing Microscopium as "totally unremarkable", astronomer [[Patrick Moore]] concluded there was nothing of interest for amateur observers.<ref name="binocs">{{cite book |last=Moore |first=Patrick |author-link=Patrick Moore |title=Exploring the Night Sky with Binoculars |publisher=Cambridge University Press |location=Cambridge |date=2000 |page=[https://archive.org/details/exploringnightsk00moor/page/110 110] |isbn=978-0-521-79390-2 |url=https://archive.org/details/exploringnightsk00moor|url-access=registration }}</ref> [[NGC 6925]] is a [[barred spiral galaxy]] of apparent magnitude 11.3 which is lens-shaped, as it lies almost edge-on to observers on Earth, 3.7 degrees west-northwest of Alpha Microscopii.<ref name=bakich2010>{{cite book |first=Michael E. |last=Bakich |date=2010 |page=289 |title=1001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers |series=Patrick Moore's Practical Astronomy Series |publisher=Springer |isbn=978-1-4419-1776-8 |url=https://books.google.com/books?id=qEhpS7d5ZdAC&pg=PA289}}</ref> [[SN 2011ei]], a [[Supernova#Type II|Type II Supernova]] in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011.<ref name=Rochester>{{cite web |title=Supernova 2011ei in NGC 6925 |url=http://www.rochesterastronomy.org/sn2011/sn2011ei.html |website=Rochester Astronomy |access-date=20 June 2015 |archive-url=https://web.archive.org/web/20150620113815/http://www.rochesterastronomy.org/sn2011/sn2011ei.html |archive-date=20 June 2015 |url-status=dead }}</ref> [[NGC 6923]] lies nearby and is a magnitude fainter still.<ref name="cambridge">{{cite book |author=Moore, Patrick |author2=Tirion, Wil |title=Cambridge Guide to Stars and Planets |publisher=Cambridge University Press |location=Cambridge |date=1997 |page=[https://archive.org/details/cambridgeguideto00moor/page/210 210] |isbn=978-0-521-58582-8 |url=https://archive.org/details/cambridgeguideto00moor|url-access=registration }}</ref> The [[Microscopium Void]] is a roughly rectangular region of relatively empty space, bounded by incomplete sheets of galaxies from other voids.<ref name=AA-229-1>{{cite journal |authors=Maurellis, A.; Fairall, A.P.; Matravers, D.R.; Ellis, G.F.R. |journal=Astronomy and Astrophysics |volume=229 |issue=1 |year=1990 |pages=75–79 |title=A two-dimensional sheet of galaxies between two southern voids |issn=0004-6361 |bibcode=1990A&A...229...75M}}</ref> The [[Microscopium Supercluster]] is an overdensity of galaxy clusters that was first noticed in the early 1990s. The component Abell clusters [[Abell 3695|3695]] and [[Abell 3696|3696]] are likely to be gravitationally bound, while the relations of Abell clusters [[Abell 3693|3693]] and [[Abell 3705|3705]] in the same field are unclear.<ref>{{cite journal |last=Pearson |first=David W. |author2=Batuski, David J. |date=2013 |title=Locating bound structure in an accelerating universe |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=436 |issue=1 |pages=796–806 |doi=10.1093/mnras/stt1614|arxiv = 1308.5154 |bibcode = 2013MNRAS.436..796P |s2cid=119271703 }}</ref><!-- cites previous 2 refs -->
Describing Microscopium as "totally unremarkable", astronomer [[Patrick Moore]] concluded there was nothing of interest for amateur observers.<ref name="binocs">{{cite book |last=Moore |first=Patrick |author-link=Patrick Moore |title=Exploring the Night Sky with Binoculars |publisher=Cambridge University Press |location=Cambridge |date=2000 |page=[https://archive.org/details/exploringnightsk00moor/page/110 110] |isbn=978-0-521-79390-2 |url=https://archive.org/details/exploringnightsk00moor|url-access=registration }}</ref> [[NGC 6925]] is a [[barred spiral galaxy]] of apparent magnitude 11.3 which is lens-shaped, as it lies almost edge-on to observers on Earth, 3.7 degrees west-northwest of Alpha Microscopii.<ref name=bakich2010>{{cite book |first=Michael E. |last=Bakich |date=2010 |page=289 |title=1001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers |series=Patrick Moore's Practical Astronomy Series |publisher=Springer |isbn=978-1-4419-1776-8 |url=https://books.google.com/books?id=qEhpS7d5ZdAC&pg=PA289}}</ref> [[SN 2011ei]], a [[Supernova#Type II|Type II Supernova]] in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011.<ref name=Rochester>{{cite web |title=Supernova 2011ei in NGC 6925 |url=http://www.rochesterastronomy.org/sn2011/sn2011ei.html |website=Rochester Astronomy |access-date=20 June 2015 |archive-url=https://web.archive.org/web/20150620113815/http://www.rochesterastronomy.org/sn2011/sn2011ei.html |archive-date=20 June 2015 |url-status=dead }}</ref> [[NGC 6923]] lies nearby and is a magnitude fainter still.<ref name="cambridge">{{cite book |author=Moore, Patrick |author2=Tirion, Wil |title=Cambridge Guide to Stars and Planets |publisher=Cambridge University Press |location=Cambridge |date=1997 |page=[https://archive.org/details/cambridgeguideto00moor/page/210 210] |isbn=978-0-521-58582-8 |url=https://archive.org/details/cambridgeguideto00moor|url-access=registration }}</ref> The [[Microscopium Void]] is a roughly rectangular region of relatively empty space, bounded by incomplete sheets of galaxies from other voids.<ref name=AA-229-1>{{cite journal |author1=Maurellis, A. |author2=Fairall, A.P. |author3=Matravers, D.R. |author4=Ellis, G.F.R. |journal=Astronomy and Astrophysics |volume=229 |issue=1 |year=1990 |pages=75–79 |title=A two-dimensional sheet of galaxies between two southern voids |issn=0004-6361 |bibcode=1990A&A...229...75M}}</ref> The [[Microscopium Supercluster]] is an overdensity of galaxy clusters that was first noticed in the early 1990s. The component Abell clusters [[Abell 3695|3695]] and [[Abell 3696|3696]] are likely to be gravitationally bound, while the relations of Abell clusters [[Abell 3693|3693]] and [[Abell 3705|3705]] in the same field are unclear.<ref>{{cite journal |last=Pearson |first=David W. |author2=Batuski, David J. |date=2013 |title=Locating bound structure in an accelerating universe |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=436 |issue=1 |pages=796–806 |doi=10.1093/mnras/stt1614|doi-access=free |arxiv = 1308.5154 |bibcode = 2013MNRAS.436..796P |s2cid=119271703 }}</ref><!-- cites previous 2 refs -->


===Meteor showers===
===Meteor showers===
[[File:Sidney Hall - Urania's Mirror - Sagittarius and Corona Australis, Microscopium, and Telescopium.png|thumb|Seen in the 1824 star chart set ''[[Urania's Mirror]]'' (in the lower left)]]
[[File:Sidney Hall - Urania's Mirror - Sagittarius and Corona Australis, Microscopium, and Telescopium.png|thumb|Seen in the 1824 star chart set ''[[Urania's Mirror]]'' (in the lower left)]]
The [[Microscopids]] are a minor [[meteor shower]] that appear from June to mid-July.<ref>{{cite journal |authors=Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal; Barentsen, Geert |title=Results of the IMO Video Meteor Network |date= July 2012 |journal=WGN, Journal of the International Meteor Organization |volume=40 |issue=5 |pages=181–186 |bibcode=2012JIMO...40..181M }}</ref>
The [[Microscopids]] are a minor [[meteor shower]] that appear from June to mid-July.<ref>{{cite journal |author1=Molau, Sirko |author2=Kac, Javor |author3=Berko, Erno |author4=Crivello, Stefano |author5=Stomeo, Enrico |author6=Igaz, Antal |author7=Barentsen, Geert |title=Results of the IMO Video Meteor Network |date= July 2012 |journal=WGN, Journal of the International Meteor Organization |volume=40 |issue=5 |pages=181–186 |bibcode=2012JIMO...40..181M }}</ref>


==History==
==History==
The stars that comprise Microscopium are in a region previously considered the hind feet of Sagittarius, a neighbouring constellation.<ref>{{cite book |author=Rubie, G. |year=1830 |title=The British Celestial Atlas |page=[https://archive.org/details/britishcelestia00rubigoog/page/n52 36] |url=https://archive.org/details/britishcelestia00rubigoog |quote=The British Celestial Atlas Rubie. |publisher=Baldwin & Cradock |location=London, United Kingdom|bibcode=1830bcat.book.....R }}</ref> [[John Ellard Gore]] wrote that [[al-Sufi]] seems to have reported that [[Ptolemy]] had seen the stars but he (Al Sufi) did not pinpoint their positions.<ref>{{cite book |author=Gore, John Ellard |author-link=John Ellard Gore |title= Astronomical Curiosities: Facts and Fallacies |url=https://books.google.com/books?id=p85jRCneOXEC&q=microscopium&pg=PT1 |year=1909 |publisher=Library of Alexandria |isbn=978-1-4655-2442-3}}</ref> Microscopium itself was introduced in 1751–52 by Lacaille with the French name ''le Microscope'',<ref name=ridpathlac>{{cite web |url=http://www.ianridpath.com/startales/lacaille.htm |title=Lacaille's Southern Planisphere of 1756 |work=Star Tales |author=Ridpath, Ian |publisher=Self-published |access-date=19 March 2015|author-link=Ian Ridpath }}</ref><ref>{{cite journal |author=Lacaille, Nicolas Louis |year=1756 |title=Relation abrégée du Voyage fait par ordre du Roi au cap de Bonne-espérance |journal=Mémoires de l'Académie Royale des Sciences |pages=519–592 [589] |url=http://gallica.bnf.fr/ark:/12148/bpt6k35505/f787 |language=fr}}</ref> after he had observed and catalogued 10,000 southern stars during a two-year stay at the [[Cape of Good Hope]]. He devised fourteen new constellations in uncharted regions of the [[Southern Celestial Hemisphere]] not visible from Europe. All but one honoured instruments that symbolised the [[Age of Enlightenment]].{{sfn|Wagman|2003|pp=6–7}} Commemorating the [[Optical microscope#compound microscope|compound microscope]],<ref name=ridpathmic>{{cite web |url=http://www.ianridpath.com/startales/microscopium.htm |title=Microscopium the Microscope |work=Star Tales |author=Ridpath, Ian |publisher=Self-published |access-date=19 March 2015|author-link=Ian Ridpath }}</ref> the Microscope's name had been Latinised by Lacaille to ''Microscopium'' by 1763.<ref name=ridpathlac/>
Microscopium lies in a region where Ptolemy had listed six 'unformed' stars behind the tail of Piscis Austrinus.<ref name=ridpathmic>{{cite web |url=http://www.ianridpath.com/startales/microscopium.html |title=Microscopium the Microscope |work=Star Tales |author=Ridpath, Ian |publisher=Online edition |access-date=22 July 2023|author-link=Ian Ridpath }}</ref> [[Al-Sufi]] did not include these stars in his revision of the ''Almagest'', presumably because he could not identify them.<ref>{{Cite thesis|last=Hafez|first=Ihsan|date=October 2010|title=Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of re-discovery|url=https://researchonline.jcu.edu.au/28854/|journal=James Cook University|page=251|type=phd}}</ref> Microscopium was introduced in 1751–52 by Lacaille with the French name ''le Microscope'',<ref name=ridpathlac>{{cite web |url=http://www.ianridpath.com/startales/lacaille.html |title=Lacaille's Southern Planisphere of 1756 |work=Star Tales |author=Ridpath, Ian |publisher=Online edition |access-date=19 March 2015|author-link=Ian Ridpath }}</ref><ref>{{cite journal |author=Lacaille, Nicolas Louis |year=1756 |title=Relation abrégée du Voyage fait par ordre du Roi au cap de Bonne-espérance |journal=Mémoires de l'Académie Royale des Sciences |pages=519–592 [589] |url=http://gallica.bnf.fr/ark:/12148/bpt6k35505/f787 |language=fr}}</ref> after he had observed and catalogued 10,000 southern stars during a two-year stay at the [[Cape of Good Hope]]. He devised fourteen new constellations in uncharted regions of the [[Southern Celestial Hemisphere]] not visible from Europe. All but one honoured instruments that symbolised the [[Age of Enlightenment]].{{sfn|Wagman|2003|pp=6–7}} Commemorating the [[Optical microscope#compound microscope|compound microscope]],<ref name=ridpathmic/> the Microscope's name had been Latinised by Lacaille to ''Microscopium'' by 1763.<ref name=ridpathlac/>


==See also==
==See also==
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{{Commons|Microscopium}}
{{Commons|Microscopium}}
* [http://www.allthesky.com/constellations/indus/constell.html The Deep Photographic Guide to the Constellations: Microscopium]
* [http://www.allthesky.com/constellations/indus/constell.html The Deep Photographic Guide to the Constellations: Microscopium]
* [http://astrojan.eu5.org/microsc.htm The clickable Microscopium]
* [http://astrojan.nhely.hu/microsc.htm The clickable Microscopium]


{{Clear}}
{{Clear}}

Latest revision as of 15:54, 27 September 2024

"The Microscope" redirects here. For the instrument, see microscope. For other uses, see Microscope (disambiguation).

Microscopium
Constellation
Microscopium
List of stars in Microscopium
AbbreviationMic
GenitiveMicroscopii
Pronunciation/ˌmaɪkrəˈskɒpiəm/, genitive /ˌmaɪkrəˈskɒpiaɪ/
Symbolismthe Microscope
Right ascension21h
Declination−36°
QuadrantSQ4
Area210 sq. deg. (66th)
Main stars5
Bayer/Flamsteed
stars		13
Stars with planets2
Stars brighter than 3.00m0
Stars within 10.00 pc (32.62 ly)2
Brightest starγ Mic (4.67m)
Messier objects0
Meteor showersMicroscopids
Bordering
constellations
Visible at latitudes between +45° and −90°.
Best visible at 21:00 (9 p.m.) during the month of September.

Microscopium ("the Microscope") is a minor constellation in the southern celestial hemisphere, one of twelve created in the 18th century by French astronomer Nicolas-Louis de Lacaille and one of several depicting scientific instruments. The name is a Latinised form of the Greek word for microscope. Its stars are faint and hardly visible from most of the non-tropical Northern Hemisphere.

The constellation's brightest star is Gamma Microscopii of apparent magnitude 4.68, a yellow giant 2.5 times the Sun's mass located 223 ± 8 light-years distant. It passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, possibly disturbing the outer Solar System. Three star systems—WASP-7, AU Microscopii and HD 205739—have been determined to have planets, while other star —the Sun-like star HD 202628— has a debris disk. AU Microscopii and the binary red dwarf system AT Microscopii are probably a wide triple system and members of the Beta Pictoris moving group. Nicknamed "Speedy Mic", BO Microscopii is a star with an extremely fast rotation period of 9 hours, 7 minutes.

Characteristics

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Microscopium is a small constellation bordered by Capricornus to the north, Piscis Austrinus and Grus to the east, Sagittarius to the west, and Indus to the south, touching on Telescopium to the southwest. The recommended three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is "Mic".[1] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined by a polygon of four segments (illustrated in infobox). In the equatorial coordinate system, the right ascension coordinates of these borders lie between 20h 27.3m and 21h 28.4m , while the declination coordinates are between −27.45° and −45.09°.[2] The whole constellation is visible to observers south of latitude 45°N.[3][a] Given that its brightest stars are of fifth magnitude, the constellation is invisible to the naked eye in areas with light polluted skies.[4][b]

Features

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

Stars

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See also: List of stars in Microscopium

French astronomer Nicolas-Louis de Lacaille charted and designated ten stars with the Bayer designations Alpha through to Iota in 1756. A star in neighbouring Indus that Lacaille had labelled Nu Indi turned out to be in Microscopium, so Gould renamed it Nu Microscopii. Francis Baily considered Gamma and Epsilon Microscopii to belong to the neighbouring constellation Piscis Austrinus, but subsequent cartographers did not follow this.[6] In his 1725 Catalogus Britannicus, John Flamsteed labelled the stars 1, 2, 3 and 4 Piscis Austrini, which became Gamma Microscopii, HR 8076, HR 8110 and Epsilon Microscopii respectively.[7] Within the constellation's borders, there are 43 stars brighter than or equal to apparent magnitude 6.5.[c][3]

Depicting the eyepiece of the microscope is Gamma Microscopii,[8] which—at magnitude of 4.68—is the brightest star in the constellation. Having spent much of its 620-million-year lifespan as a blue-white main sequence star, it has swollen and cooled to become a yellow giant of spectral type G6III, with a diameter ten times that of the Sun.[9] Measurement of its parallax yields a distance of 223 ± 8 light years from Earth.[10] It likely passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, at around 2.5 times the mass of the Sun, it is possibly massive enough and close enough to disturb the Oort cloud.[11] Alpha Microscopii is also an ageing yellow giant star of spectral type G7III with an apparent magnitude of 4.90.[12] Located 400 ± 30 light-years away from Earth,[13] it has swollen to 17.5 times the diameter of the Sun.[14] Alpha has a 10th magnitude companion, visible in 7.5 cm telescopes,[15][16] though this is a coincidental closeness rather than a true binary system.[14] Epsilon Microscopii lies 166 ± 5 light-years away,[17] and is a white star of apparent magnitude 4.7,[16] and spectral type A1V.[18] Theta1 and Theta2 Microscopii make up a wide double whose components are splittable to the naked eye. Both are white A-class magnetic spectrum variable stars with strong metallic lines, similar to Cor Caroli. They mark the constellation's specimen slide.[8]

Many notable objects are too faint to be seen with the naked eye. AX Microscopii, better known as Lacaille 8760, is a red dwarf which lies only 12.9 light-years from the Solar System. At magnitude 6.68, it is the brightest red dwarf in the sky.[19] BO Microscopii is a rapidly rotating star that has 80% the diameter of the Sun. Nicknamed "Speedy Mic", it has a rotation period of 9 hours 7 minutes.[20] An active star, it has prominent stellar flares that average 100 times stronger than those of the Sun, and are emitting energy mainly in the X-ray and ultraviolet bands of the spectrum.[21] It lies 218 ± 4 light-years away from the Sun.[22] AT Microscopii is a binary star system, both members of which are flare star red dwarfs. The system lies close to and may form a very wide triple system with AU Microscopii,[23] a young star which has a planetary system in the making with a debris disk. The three stars are candidate members of the Beta Pictoris moving group, one of the nearest associations of stars that share a common motion through space.[24]

The Astronomical Society of Southern Africa in 2003 reported that observations of four of the Mira variables in Microscopium were very urgently needed as data on their light curves was incomplete.[25] Two of them—R and S Microscopii—are challenging stars for novice amateur astronomers,[26] and the other two, U and RY Microscopii, are more difficult still.[25] Another red giant, T Microscopii, is a semiregular variable that ranges between magnitudes 7.7 and 9.6 over 344 days.[27] Of apparent magnitude 11, DD Microscopii is a symbiotic star system composed of an orange giant of spectral type K2III and white dwarf in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system has a low metallicity. Combined with its high galactic latitude, this indicates that the star system has its origin in the galactic halo of the Milky Way.[28]

HD 205739 is a yellow-white main sequence star of spectral type F7V that is around 1.22 times as massive and 2.3 times as luminous as the Sun. It has a Jupiter-sized planet with an orbital period of 280 days that was discovered by the radial velocity method.[29] WASP-7 is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28 times as massive as the Sun. Its hot Jupiter planet—WASP-7b—was discovered by transit method and found to orbit the star every 4.95 days.[30] HD 202628 is a sunlike star of spectral type G2V with a debris disk that ranges from 158 to 220 AU distant. Its inner edge is sharply defined, indicating a probable planet orbiting between 86 and 158 AU from the star.[31]

Deep sky objects

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Arp-Madore 2026-424 taken by Hubble.[32]

Describing Microscopium as "totally unremarkable", astronomer Patrick Moore concluded there was nothing of interest for amateur observers.[33] NGC 6925 is a barred spiral galaxy of apparent magnitude 11.3 which is lens-shaped, as it lies almost edge-on to observers on Earth, 3.7 degrees west-northwest of Alpha Microscopii.[34] SN 2011ei, a Type II Supernova in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011.[35] NGC 6923 lies nearby and is a magnitude fainter still.[36] The Microscopium Void is a roughly rectangular region of relatively empty space, bounded by incomplete sheets of galaxies from other voids.[37] The Microscopium Supercluster is an overdensity of galaxy clusters that was first noticed in the early 1990s. The component Abell clusters 3695 and 3696 are likely to be gravitationally bound, while the relations of Abell clusters 3693 and 3705 in the same field are unclear.[38]

Meteor showers

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Seen in the 1824 star chart set Urania's Mirror (in the lower left)

The Microscopids are a minor meteor shower that appear from June to mid-July.[39]

History

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Microscopium lies in a region where Ptolemy had listed six 'unformed' stars behind the tail of Piscis Austrinus.[40] Al-Sufi did not include these stars in his revision of the Almagest, presumably because he could not identify them.[41] Microscopium was introduced in 1751–52 by Lacaille with the French name le Microscope,[42][43] after he had observed and catalogued 10,000 southern stars during a two-year stay at the Cape of Good Hope. He devised fourteen new constellations in uncharted regions of the Southern Celestial Hemisphere not visible from Europe. All but one honoured instruments that symbolised the Age of Enlightenment.[44] Commemorating the compound microscope,[40] the Microscope's name had been Latinised by Lacaille to Microscopium by 1763.[42]

See also

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Notes

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  1. ^ While parts of the constellation technically rise above the horizon to observers between 45°N and 62°N, stars within a few degrees of the horizon are to all intents and purposes unobservable.[3]
  2. ^ Objects of magnitude 5.0 are barely visible to the unaided eye in the night skies of city-suburban transition areas.[5]
  3. ^ Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.[5]

References

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Citations

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  1. ^ Russell, Henry Norris (1922). "The new international symbols for the constellations". Popular Astronomy. Vol. 30. p. 469. Bibcode:1922PA.....30..469R.
  2. ^ "Microscopium, constellation boundary". The Constellations. Retrieved 13 July 2012.
  3. ^ a b c Ian Ridpath. "Constellations: Lacerta–Vulpecula". Star Tales. Self-published. Retrieved 29 November 2014.
  4. ^ Kambič, Bojan (2009). Viewing the Constellations with Binoculars. Springer. p. 341. ISBN 978-0-387-85354-3.
  5. ^ a b Bortle, John E. (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Sky Publishing Corporation. Archived from the original on 16 December 2012. Retrieved 29 November 2014.
  6. ^ Wagman 2003, pp. 181, 210.
  7. ^ Wagman 2003, p. 458.
  8. ^ a b Motz, Lloyd; Nathanson, Carol (1991). The Constellations: An Enthusiast's Guide to the Night Sky. London: Aurum Press. pp. 369–370. ISBN 978-1-85410-088-7.
  9. ^ Kaler, James B. "Gamma Mic". Stars. Retrieved 13 July 2012.
  10. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  11. ^ Bailer-Jones, C.A.L. (2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35.
  12. ^ "Alpha MicroscopiI". SIMBAD. Retrieved 15 July 2012.
  13. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  14. ^ a b Kaler, James B. "Alpha Mic". Stars. Retrieved 19 March 2015.
  15. ^ Malin, David; Frew, David J. (1995). Hartung's Astronomical Objects for Southern Telescopes, with an Addendum for Northern Observatories: A Handbook for Amateur Observers. Cambridge: Cambridge University Press. p. 287. ISBN 978-0-521-55491-6.
  16. ^ a b Ridpath, Ian; Tirion, Wil (2007). Stars and Planets Guide. Princeton, New Jersey: Princeton University Press. pp. 184–185. ISBN 978-0-691-13556-4.
  17. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  18. ^ "Epsilon Microscopii". SIMBAD. Retrieved 15 July 2012.
  19. ^ Croswell, Ken (July 2002). "The Brightest Red Dwarf". Sky & Telescope. p. 32. Retrieved 15 July 2012.
  20. ^ Dunstone, N.J.; Barnes, J.R.; Collier Cameron, A.; Jardine, M. (2006). "The coronal structure of Speedy Mic – I. A densely packed prominence system beyond corotation". Monthly Notices of the Royal Astronomical Society. 365 (2): 530–538. arXiv:astro-ph/0510739. Bibcode:2006MNRAS.365..530D. doi:10.1111/j.1365-2966.2005.09729.x. S2CID 11048210.
  21. ^ Wolter, U.; Robrade, J.; Schmitt, J.H.M.M.; Ness, J.U. (2008). "Doppler imaging an X-ray flare on the ultrafast rotator BO Mic. A contemporaneous multiwavelength study using XMM-Newton and VLT". Astronomy and Astrophysics. 478 (1): L11 – L14. arXiv:0712.0899. Bibcode:2008A&A...478L..11W. doi:10.1051/0004-6361:20078838. S2CID 62827486.
  22. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  23. ^ Caballero, J.A. (November 2009). "Reaching the boundary between stellar kinematic groups and very wide binaries. The Washington double stars with the widest angular separations". Astronomy and Astrophysics. 507 (1): 251–259. arXiv:0908.2761. Bibcode:2009A&A...507..251C. doi:10.1051/0004-6361/200912596. S2CID 118194112.
  24. ^ McCarthy, Kyle; White, Russel J. (2012). "The Sizes of the Nearest Young Stars". The Astronomical Journal. 143 (6): 134–168. arXiv:1201.6600. Bibcode:2012AJ....143..134M. doi:10.1088/0004-6256/143/6/134. S2CID 118538522.
  25. ^ a b Cooper, Tim (2003). "Presidential address: Amateur Observations – Successes and Opportunities". Monthly Notes of the Astronomical Society of Southern Africa. 62: 234–240. Bibcode:2003MNSSA..62..234C.
  26. ^ Levy, David H. (1998). Observing Variable Stars: A Guide for the Beginner. Cambridge: Cambridge University Press. p. 172. ISBN 978-0-521-62755-9.
  27. ^ Arnold, H.J.P; Doherty, Paul; Moore, Patrick (1999). The Photographic Atlas of the Stars. Boca Raton, Florida: CRC Press. p. 53. ISBN 978-0-7503-0654-6.
  28. ^ Pereira, C.B.; Roig, F. (2009). "High-Resolution Spectroscopic Observations of Four Yellow-Type Symbiotic Stars: CD-43°14304, Hen 3-1213, Hen 3-863, and StHα 176". The Astronomical Journal. 137 (1): 118–128. Bibcode:2009AJ....137..118P. doi:10.1088/0004-6256/137/1/118.
  29. ^ López-Morales, Mercedes; Butler, R. Paul; Fischer, Debra A.; Minniti, Dante; Shectman, Stephen A.; Takeda, Genya; Adams, Fred C.; Wright, Jason T.; Arriagada, Pamela (2008). "Two Jupiter-Mass Planets Orbiting HD 154672 and HD 205739". The Astronomical Journal. 136 (5): 1901–1905. arXiv:0809.1037. Bibcode:2008AJ....136.1901L. doi:10.1088/0004-6256/136/5/1901. S2CID 119242543.
  30. ^ Hellier, Coel; Anderson, D.R.; Gillon, M.; Lister, T.A.; Maxted, P.F.L.; Queloz, D.; Smalley, B.; Triaud, A.H.M.J.; West, R.G.; Wilson, D.M.; Alsubai, K.; Bentley, S.J.; Cameron, A. Collier; Hebb, L.; Horne, K.; Irwin, J.; Kane, S.R.; Mayor, M.; Pepe, F.; Pollacco, D.; Skillen, I.; Udry, S.; Wheatley, P.J.; Christian, D.J.; Enoch, R.; Haswell, C.A.; Joshi, Y.C.; Norton, A.J.; Parley, N.; Ryans, R. (2008). "Wasp-7: A Bright Transiting-Exoplanet System in the Southern Hemisphere". The Astrophysical Journal Letters. 690 (1): L89 – L91. arXiv:0805.2600. Bibcode:2009ApJ...690L..89H. doi:10.1088/0004-637X/690/1/L89. S2CID 15962609.
  31. ^ Nesvold, Erika R.; Kuchner, Marc J. (2015). "Gap Clearing by Planets in a Collisional Debris Disk". The Astrophysical Journal. 798 (2): 10. arXiv:1410.7784. Bibcode:2015ApJ...798...83N. doi:10.1088/0004-637X/798/2/83. S2CID 118667155. 83.
  32. ^ "Hubble Captures Cosmic Face". www.spacetelescope.org. Retrieved 31 October 2019.
  33. ^ Moore, Patrick (2000). Exploring the Night Sky with Binoculars. Cambridge: Cambridge University Press. p. 110. ISBN 978-0-521-79390-2.
  34. ^ Bakich, Michael E. (2010). 1001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers. Patrick Moore's Practical Astronomy Series. Springer. p. 289. ISBN 978-1-4419-1776-8.
  35. ^ "Supernova 2011ei in NGC 6925". Rochester Astronomy. Archived from the original on 20 June 2015. Retrieved 20 June 2015.
  36. ^ Moore, Patrick; Tirion, Wil (1997). Cambridge Guide to Stars and Planets. Cambridge: Cambridge University Press. p. 210. ISBN 978-0-521-58582-8.
  37. ^ Maurellis, A.; Fairall, A.P.; Matravers, D.R.; Ellis, G.F.R. (1990). "A two-dimensional sheet of galaxies between two southern voids". Astronomy and Astrophysics. 229 (1): 75–79. Bibcode:1990A&A...229...75M. ISSN 0004-6361.
  38. ^ Pearson, David W.; Batuski, David J. (2013). "Locating bound structure in an accelerating universe". Monthly Notices of the Royal Astronomical Society. 436 (1): 796–806. arXiv:1308.5154. Bibcode:2013MNRAS.436..796P. doi:10.1093/mnras/stt1614. S2CID 119271703.
  39. ^ Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal; Barentsen, Geert (July 2012). "Results of the IMO Video Meteor Network". WGN, Journal of the International Meteor Organization. 40 (5): 181–186. Bibcode:2012JIMO...40..181M.
  40. ^ a b Ridpath, Ian. "Microscopium the Microscope". Star Tales. Online edition. Retrieved 22 July 2023.
  41. ^ Hafez, Ihsan (October 2010). Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of re-discovery. James Cook University (phd). p. 251.
  42. ^ a b Ridpath, Ian. "Lacaille's Southern Planisphere of 1756". Star Tales. Online edition. Retrieved 19 March 2015.
  43. ^ Lacaille, Nicolas Louis (1756). "Relation abrégée du Voyage fait par ordre du Roi au cap de Bonne-espérance". Mémoires de l'Académie Royale des Sciences (in French): 519–592 [589].
  44. ^ Wagman 2003, pp. 6–7.

Cited texts

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  • 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. ISBN 978-0-939923-78-6.
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