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The Gemini Planet Imager (GPI) is a high contrast imaging instrument that was built for the Gemini South Telescope in Chile. The instrument achieves high contrast at small angular separations, allowing for the direct imaging and integral field spectroscopy of extrasolar planets around nearby stars.^[1] The collaboration involved in planning and building the Gemini Planet imager includes the American Museum of Natural History (AMNH), Dunlap Institute, Gemini Observatory, Herzberg Institute of Astrophysics (HIA), Jet Propulsion Laboratory, Lawrence Livermore National Lab (LLNL), Lowell Observatory, SETI Institute, The Space Telescope Science Institute (STSCI), the University of Montreal, University of California, Berkeley, University of California, Los Angeles (UCLA), University of California, Santa Cruz (UCSC), University of Georgia.^[2]

Specifications

The Gemini Planet Imager is being used at the Gemini South Telescope, located in Cerro Pachon, Chile. It saw the first light in November 2013, and entered regular operations in November 2014.^[2] It is designed to directly detect young gas giants via their thermal emission. It will operate at near-infrared wavelengths (Y - K bands), where planets will be reasonably bright, but thermal emission from the Earth's atmosphere is not too strong.^[3]

The system consists of multiple components, including a high-order adaptive optics system, a coronagraph, a calibration interferometer, and an integral field spectrograph. The adaptive optics system, being built at LLNL, uses a MEMS deformable mirror from Boston Micromachines Corporation to correct wavefront errors induced by motion of air in the atmosphere and the optics in the telescope. The coronagraph, being built at AMNH, blocks out the light from the star being observed, which is necessary in order to see a much dimmer companion. Before sending the GPI at Gemini South it was essential to test the coronagraph by reproducing the exact experimental conditions in which it was going to be used. A Photon etc. tunable laser source was used for this and helped determine that, at its most efficient wavelength, the imager could detect a planet only slightly more massive than Jupiter around a 100-million-year-old Sun-like star.^[4] The spectrograph, developed by UCLA and Montreal, images and takes spectra of any detected companion to the star, with a spectral resolving power of 34 - 83, depending on wavelength. The expected instrument performance will allow for detection of companions one ten millionth as bright as their hosts at angular separations of roughly 0.2-1 arcseconds, down to an H band magnitude of 23.^[5]

Scientific goals

Present day searches for exoplanets are insensitive to exoplanets located at the distances from their host star comparable to the semi-major axes of the gas giants in the Solar System, greater than about 5 AU. Surveys using the radial velocity method require observing a star over at least one period of revolution, which is roughly 30 years for a planet at the distance of Saturn. Existing adaptive optics instruments become ineffective at small angular separations, limiting them to semi-major axes larger than about 30 astronomical units. The high contrast of the Gemini Planet Imager at small angular separations will allow it to detect gas giants with semi-major axes of 5–30 astronomical units.^[6]

The Gemini Planet Imager will be most effective at detecting young gas giants, one million to one billion years old. The reason for this is that young planets retain heat from their formation, and only gradually cool. While a planet is still hot, it remains bright, and is thus more easily detected. This limits GPI to younger targets, but means that it will yield information about how gas giants form. In particular, the spectrograph will allow determination of the temperature and surface gravity, which yield information about the atmospheres and thermal evolution of gas giants.^[6]

In addition to its main goal of imaging exoplanets, GPI will be capable of studying protoplanetary disks, transition disks, and debris disks around young stars. This may provide clues about planet formation. The technique used to image disks with this instrument is called polarization differential imaging. Another science case is to study Solar System objects at high spatial resolution and high Strehl ratio. Asteroids and their moons, the satellites of Jupiter and Saturn, and the planets Uranus and Neptune are all good targets for GPI. The final ancillary science case is to study the mass loss from evolved stars via their outflow.^{[citation needed]}

Achievements

The planet 51 Eridani b is the first exoplanet discovered by the Gemini Planet Imager. It is a million times fainter than its parent star and shows the second strongest methane signature ever detected on an alien planet (after only GJ 504b), which should yield additional clues as to how the planet formed.^[7]

Evolution

In 2022, GPI was removed from the Gemini South telescope and shipped to the University of Notre Dame in Indiana to undergo a major upgrade of the whole system called GPI 2.0.^[8] GPI 2.0 will be installed on the Gemini North telescope and is expected to see first light in late 2024 or early 2025.

Gallery

GPI Image of star HR4796a showing the debris disk as seen through polarization measurements.

References

^ Macintosh et al. (2006), p. 1.
^ ^a ^b "GPI: Gemini Planet Imager". Retrieved 2010-03-07.
^ Graham et al. (2007), p 2.
^ S. R. Soummer; et al. (2009). Shaklan, Stuart B. (ed.). "The Gemini Planet Imager coronagraph testbed". Proc. SPIE 7440 Techniques and Instrumentation for Detection of Exoplanets IV. Techniques and Instrumentation for Detection of Exoplanets IV. 7440: 74400R. Bibcode:2009SPIE.7440E..0RS. doi:10.1117/12.826700. S2CID 122904075.
^ Macintosh et al. (2006), p. 3.
^ ^a ^b Macintosh et al. (2006), p. 2.
^ Bjorn, Carey. "Astronomers discover 'young Jupiter' exoplanet". ScienceDaily. Stanford University. Retrieved 17 August 2015.
^ "GPI 2.0". Retrieved 7 January 2024.

Bibliography

Graham, James R.; Macintosh, Bruce; Doyon, Rene; Gavel, Don; Larkin, James; Levine, Marty; Oppenheimer, Rebecca; Palmer, David; Saddlemyer, Les; Sivaramakrishnan, Anand; Veran, Jean-Pierre; Wallace, Kent (2007). "Ground-Based Direct Detection of Exoplanets with the Gemini Planet Imager (GPI)". arXiv:0704.1454 [astro-ph].
Bruce Macintosh; James Graham; David Palmer; Rene Doyon; Don Gavel; James Larkin; Ben Oppenheimer; Leslie Saddlemyer; J. Kent Wallace; Brian Bauman; Julia Evans; Darren Erikson; Katie Morzinski; Donald Phillion; Lisa Poyneer; Anand Sivaramakrishnan; Remi Soummer; Simon Thibault; Jean-Pierre Veran (June 2006). "The Gemini Planet Imager". Proceedings of SPIE. Astronomical Telescopes. 6272: 62720L–62720L–12. Bibcode:2006SPIE.6272E..0LM. doi:10.1117/12.672430. OSTI 898473. S2CID 123044593.

[1] Macintosh et al. (2006), p. 1.

[gpi_site-2] "GPI: Gemini Planet Imager". Retrieved 2010-03-07.

[3] Graham et al. (2007), p 2.

[4] S. R. Soummer; et al. (2009). Shaklan, Stuart B. (ed.). "The Gemini Planet Imager coronagraph testbed". Proc. SPIE 7440 Techniques and Instrumentation for Detection of Exoplanets IV. Techniques and Instrumentation for Detection of Exoplanets IV. 7440: 74400R. Bibcode:2009SPIE.7440E..0RS. doi:10.1117/12.826700. S2CID 122904075.

[5] Macintosh et al. (2006), p. 3.

[mac2-6] Macintosh et al. (2006), p. 2.

[Stanford_University-7] Bjorn, Carey. "Astronomers discover 'young Jupiter' exoplanet". ScienceDaily. Stanford University. Retrieved 17 August 2015.

[8] "GPI 2.0". Retrieved 7 January 2024.

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@@ Line 1: / Line 1: @@
+{{Short description|Imaging instrument for the Gemini South Telescope in Chile}}
-The '''Gemini Planet Imager''' (GPI) is a high contrast imaging instrument that was built for the [[Gemini Observatory|Gemini South Telescope]] in [[Chile]]. The instrument achieves high contrast at small angular separations, allowing for the direct imaging and integral field spectroscopy of [[extrasolar planet]]s around nearby [[star]]s.<ref>Macintosh ''et al.'' (2006), p. 1.</ref> The collaboration involved in planning and building the Gemini Planet imager includes the [[American Museum of Natural History]] (AMNH), [[Dunlap Institute]], [[Gemini Observatory]], [[Herzberg Institute of Astrophysics]] (HIA), [[Jet Propulsion Laboratory]], [[Lawrence Livermore National Lab]] (LLNL), [[Lowell Observatory]], [[SETI Institute]], The [[Space Telescope Science Institute]] (STSCI), the [[University of Montreal]], [[University of California, Berkeley]], [[University of California, Los Angeles]] (UCLA), [[University of California, Santa Cruz]] (UCSC), [[University of Georgia]].<ref name="gpi_site">{{cite web | url = http://planetimager.org/ | title = GPI: Gemini Planet Imager | accessdate = 2010-03-07}}</ref>
+The '''Gemini Planet Imager''' (GPI) is a high contrast imaging instrument that was built for the [[Gemini Observatory|Gemini South Telescope]] in [[Chile]]. The instrument achieves high contrast at small angular separations, allowing for the direct imaging and integral field spectroscopy of [[extrasolar planet]]s around nearby [[star]]s.<ref>Macintosh ''et al.'' (2006), p. 1.</ref> The collaboration involved in planning and building the Gemini Planet imager includes the [[American Museum of Natural History]] (AMNH), [[Dunlap Institute]], [[Gemini Observatory]], [[Herzberg Institute of Astrophysics]] (HIA), [[Jet Propulsion Laboratory]], [[Lawrence Livermore National Lab]] (LLNL), [[Lowell Observatory]], [[SETI Institute]], The [[Space Telescope Science Institute]] (STSCI), the [[University of Montreal]], [[University of California, Berkeley]], [[University of California, Los Angeles]] (UCLA), [[University of California, Santa Cruz]] (UCSC), [[University of Georgia]].<ref name="gpi_site">{{cite web | url = http://planetimager.org/ | title = GPI: Gemini Planet Imager | access-date = 2010-03-07}}</ref>
 [[File:Logo gpi.png|160px|thumb|right]]
@@ Line 8: / Line 9: @@
 The Gemini Planet Imager is being used at the Gemini South Telescope, located in [[Cerro Pachon]], [[Chile]]. It saw the [[First light (astronomy)|first light]] in November 2013, and entered regular operations in November 2014.<ref name="gpi_site"/> It is designed to directly detect young [[gas giant]]s via their [[thermal emission]]. It will operate at near-[[infrared astronomy|infrared]] [[wavelength]]s (Y - K bands), where planets will be reasonably bright, but thermal emission from the [[Earth]]'s [[atmosphere]] is not too strong.<ref>Graham ''et al.'' (2007), p 2.</ref>
-The system consist of multiple components, including a high-order adaptive optics system, a [[coronagraph]], a calibration interferometer, and an [[integral field spectrograph]]. The adaptive optics system, being built at LLNL, uses a [[MEMS]] [[deformable mirror]] from [[Boston Micromachines Corporation]] to correct [[wavefront]] errors induced by [[Astronomical seeing|motion of air in the atmosphere]] and the [[optics]] in the [[telescope]]. The coronagraph, being built at AMNH, blocks out the light from the star being observed, which is necessary in order to see a much dimmer companion. Before sending the GPI at Gemini South it was essential to test the coronagraph by reproducing the exact experimental conditions in which it was going to be used. [[Photon etc.]] [[tunable laser]] source was use for this matter and helped determine that at its efficiency peak of wavelength, the imager could detect a planet only slightly more massive than Jupiter around a 100-million-year-old Sun-like star.<ref>{{cite journal |author=S. R. Soummer |display-authors=etal |title= The Gemini Planet Imager coronagraph testbed|journal=Proc. SPIE 7440 Techniques and Instrumentation for Detection of Exoplanets IV |date=2009 | doi= 10.1117/12.826700}}</ref> The spectrograph, developed by UCLA and Montreal, images and takes [[spectrum|spectra]] of any detected companion to the star, with a [[spectral resolution|spectral resolving power]] of 34 - 83, depending on wavelength. The expected instrument performance will allow for detection of companions one ten millionth as bright as their hosts at angular separations of roughly 0.2-1 [[arcsecond]]s, down to an H band magnitude of 23.<ref>Macintosh ''et al.'' (2006), p. 3.</ref>
+The system consists of multiple components, including a high-order adaptive optics system, a [[coronagraph]], a calibration interferometer, and an [[integral field spectrograph]]. The adaptive optics system, being built at LLNL, uses a [[MEMS]] [[deformable mirror]] from [[Boston Micromachines Corporation]] to correct [[wavefront]] errors induced by [[Astronomical seeing|motion of air in the atmosphere]] and the [[optics]] in the [[telescope]]. The coronagraph, being built at AMNH, blocks out the light from the star being observed, which is necessary in order to see a much dimmer companion. Before sending the GPI at Gemini South it was essential to test the coronagraph by reproducing the exact experimental conditions in which it was going to be used. A [[Photon etc.]] [[tunable laser]] source was used for this and helped determine that, at its most efficient wavelength, the imager could detect a planet only slightly more massive than Jupiter around a 100-million-year-old Sun-like star.<ref>{{cite journal |author=S. R. Soummer |editor1-first=Stuart B. |editor1-last=Shaklan |display-authors=etal |title= The Gemini Planet Imager coronagraph testbed|journal=Proc. SPIE 7440 Techniques and Instrumentation for Detection of Exoplanets IV |series=Techniques and Instrumentation for Detection of Exoplanets IV |date=2009 |volume=7440 |pages=74400R | doi= 10.1117/12.826700|bibcode=2009SPIE.7440E..0RS |s2cid=122904075 }}</ref> The spectrograph, developed by UCLA and Montreal, images and takes [[spectrum|spectra]] of any detected companion to the star, with a [[spectral resolution|spectral resolving power]] of 34 - 83, depending on wavelength. The expected instrument performance will allow for detection of companions one ten millionth as bright as their hosts at angular separations of roughly 0.2-1 [[arcsecond]]s, down to an H band magnitude of 23.<ref>Macintosh ''et al.'' (2006), p. 3.</ref>
 ==Scientific goals==
-Present day [[methods of detecting extrasolar planets|searches for exoplanet]]s are insensitive to exoplanets located at the distances from their host star comparable to the [[Semi-major axis|semi-major axes]] of the gas giants in the [[Solar System]], greater than about 5 AU. Surveys using the [[radial velocity method]] require observing a star over at least one [[Orbital period|period]] of revolution, which is roughly 30 years for a planet at the distance of [[Saturn]]. Existing adaptive optics instruments become ineffective at small angular separations, limiting them to semi-major axes larger than about 30 [[astronomical unit]]s. The high contrast of the Gemini Planet Imager at small angular separations will allow it to detect gas giants with semi-major axes of 5-30 [[astronomical unit]]s.<ref name="mac2">Macintosh ''et al.'' (2006), p. 2.</ref>
+Present day [[methods of detecting extrasolar planets|searches for exoplanet]]s are insensitive to exoplanets located at the distances from their host star comparable to the [[Semi-major axis|semi-major axes]] of the gas giants in the [[Solar System]], greater than about 5 AU. Surveys using the [[radial velocity method]] require observing a star over at least one [[Orbital period|period]] of revolution, which is roughly 30 years for a planet at the distance of [[Saturn]]. Existing adaptive optics instruments become ineffective at small angular separations, limiting them to semi-major axes larger than about 30 [[astronomical unit]]s. The high contrast of the Gemini Planet Imager at small angular separations will allow it to detect gas giants with semi-major axes of 5–30 [[astronomical unit]]s.<ref name="mac2">Macintosh ''et al.'' (2006), p. 2.</ref>
-The Gemini Planet Imager will be most effective at detecting young gas giants, 1 Myr to 1 Gyr in age. The reason for this is that young planets retain heat from their formation, and only gradually cool. While a planet is still hot, it remains bright, and is thus more easily detected. This limits GPI to younger targets, but means that it will yield information about [[planet formation|how gas giants form]]. In particular, the spectrograph will allow determination of the [[temperature]] and [[surface gravity]], which yield information about the atmospheres and thermal evolution of gas giants.<ref name="mac2"/>
+The Gemini Planet Imager will be most effective at detecting young gas giants, one million to one billion years old. The reason for this is that young planets retain heat from their formation, and only gradually cool. While a planet is still hot, it remains bright, and is thus more easily detected. This limits GPI to younger targets, but means that it will yield information about [[planet formation|how gas giants form]]. In particular, the spectrograph will allow determination of the [[temperature]] and [[surface gravity]], which yield information about the atmospheres and thermal evolution of gas giants.<ref name="mac2"/>
-In addition to its main goal of imaging exoplanets, GPI will be capable of studying [[protoplanetary disks]], [[transition disks]], and [[debris disks]] around young stars.  This may provide clues about [[planet formation]].  The technique used to image disks with this instrument is called polarization differential imaging.  Another science case is to study [[solar system]] objects at high spatial resolution and high [[Strehl ratio]].  Asteroids and their moons, the satellites of [[Jupiter]] and [[Saturn]], Uranus, and Neptune are all good targets for GPI.  The final ancillary science case is to study the mass loss from evolved stars via their outflow.
+In addition to its main goal of imaging exoplanets, GPI will be capable of studying [[protoplanetary disks]], [[transition disks]], and [[debris disks]] around young stars. This may provide clues about [[planet formation]]. The technique used to image disks with this instrument is called polarization differential imaging. Another science case is to study [[Solar System]] objects at high spatial resolution and high [[Strehl ratio]]. Asteroids and their moons, the satellites of [[Jupiter]] and [[Saturn]], and the planets Uranus and Neptune are all good targets for GPI. The final ancillary science case is to study the mass loss from evolved stars via their outflow.{{Citation needed|date=March 2019}}
-==Achivements==
+==Achievements==
-The planet 51 Eridani b, is the first exoplanet discovered by the Gemini Planet Imager. It is a million times fainter than its parent star and shows the strongest methane signature ever detected on an alien planet, which should yield additional clues as to how the planet formed.
+The planet [[51 Eridani b]] is the first exoplanet discovered by the Gemini Planet Imager. It is a million times fainter than its parent star and shows the second strongest [[methane]] signature ever detected on an alien planet (after only [[Gliese 504 b|GJ 504b]]), which should yield additional clues as to how the planet formed.<ref name="Stanford University">{{cite web|last1=Bjorn|first1=Carey|title=Astronomers discover 'young Jupiter' exoplanet|url=https://www.sciencedaily.com/releases/2015/08/150813142532.htm|website=ScienceDaily|publisher=[[Stanford University]]|access-date=17 August 2015}}</ref>
+==Evolution==
+In 2022, GPI was removed from the [[Gemini South]] telescope and shipped to the [[University of Notre Dame]] in Indiana to undergo a major upgrade of the whole system called GPI 2.0.<ref>{{cite web |title=GPI 2.0 |url=https://www.gemini.edu/instrumentation/future-instruments/gpi2 |access-date=7 January 2024}}</ref> GPI 2.0 will be installed on the [[Gemini North]] telescope and is expected to see first light in late 2024 or early 2025.
 ==Gallery==
@@ Line 27: / Line 31: @@
 ==References==
-{{reflist}}
+{{Reflist}}
 ==Bibliography==
-*{{cite journal | title = Ground-Based Direct Detection of Exoplanets with the Gemini Planet Imager (GPI) | author = Graham, James R.; Macintosh, Bruce; Doyon, Rene; Gavel, Don; Larkin, James; Levine, Marty; Oppenheimer, Ben; Palmer, David; Saddlemyer, Les; Sivaramakrishnan, Anand; Veran, Jean-Pierre; Wallace, Kent | journal = Eprint arXiv:0704.1454 | date = 2007 | bibcode = 2007arXiv0704.1454G | arxiv=0704.1454|url=http://arxiv.org/abs/0704.1454}}
+*{{cite arXiv | title = Ground-Based Direct Detection of Exoplanets with the Gemini Planet Imager (GPI) |author1=Graham, James R. |author2=Macintosh, Bruce |author3=Doyon, Rene |author4=Gavel, Don |author5=Larkin, James |author6=Levine, Marty |author7=Oppenheimer, Rebecca |author8=Palmer, David |author9=Saddlemyer, Les |author10=Sivaramakrishnan, Anand |author11=Veran, Jean-Pierre |author12=Wallace, Kent | date = 2007  |class=astro-ph |eprint=0704.1454}}
-*{{cite journal | authors=Bruce Macintosh, James Graham, David Palmer, Rene Doyon, Don Gavel, James Larkin, Ben Oppenheimer, Leslie Saddlemyer, J. Kent Wallace, Brian Bauman, Julia Evans, Darren Erikson, Katie Morzinski, Donald Phillion, Lisa Poyneer, Anand Sivaramakrishnan, Remi Soummer, Simon Thibault, Jean-Pierre Veran | title=The Gemini Planet Imager | journal=Proceedings of SPIE |date=June 2006 | volume=6272 | series=Astronomical Telescopes | pages=62720L-62720L-12 | doi=10.1117/12.672430 | url=http://adsabs.harvard.edu/abs/2006SPIE.6272E..18M | accessdate=18 April 2012}}
+*{{cite journal |author=Bruce Macintosh |author2=James Graham |author3=David Palmer |author4=Rene Doyon |author5=Don Gavel |author6=James Larkin |author7=Ben Oppenheimer |author8=Leslie Saddlemyer |author9=J. Kent Wallace |author10=Brian Bauman |author11=Julia Evans |author12=Darren Erikson |author13=Katie Morzinski |author14=Donald Phillion |author15=Lisa Poyneer |author16=Anand Sivaramakrishnan |author17=Remi Soummer |author18=Simon Thibault |author19=Jean-Pierre Veran | title=The Gemini Planet Imager | journal=Proceedings of SPIE |date=June 2006 | volume=6272 | series=Astronomical Telescopes | pages=62720L–62720L–12 | doi=10.1117/12.672430 | bibcode=2006SPIE.6272E..0LM | osti=898473 | s2cid=123044593 }}<!--| access-date=18 April 2012-->
 {{Exoplanet search projects}}
+{{Exoplanet}}
 [[Category:Telescope instruments]]