The Gemini Planet Imager: integration and status

Macintosh, Bruce; Anthony, André; Atwood, Jennifer; Barriga, Nicolas A.; Bauman, Brian; Caputa, K.; Chilcote, J.; Dillon, Daren; Doyon, René; Dunn, Jennifer; Gavel, Donald T.; Galvez, Ramon; Goodsell, Stephen J.; Graham, James R.; Hartung, Markus; Isaacs, Joshua; Kerley, Dan; Konopacky, Quinn; Labrie, Kathleen; Larkin, James E.; Maire, Jérôme; Marois, Christian; Millar-Blanchaer, Max; Nunez, Arturo; Oppenheimer, Ben R.; Palmer, David; Pazder, John; Perrin, Marshall D.; Poyneer, Lisa; Quirez, Carlos; Rantakyrö, F.; Reshtov, Vlad; Saddlemyer, Leslie; Sadakuni, Naru; Savransky, Dmitry; Sivaramakrishnan, Anand; Smith, Malcolm J.; Soummer, Rémi; Thomas, Sandrine; Wallace, J. Kent; Weiss, Jason; Wiktorowicz, Sloane

doi:10.1117/12.926721

Cited by 30 publications

(14 citation statements)

References 6 publications

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“…First-Light Adaptive Optics Performance GPI was extensively characterized at the University of California, Santa Cruz, before shipping to Chile (34). In October 2013 it was attached to the bottom Cassegrain port of the Gemini South telescope.…”

Section: Design Of the Gemini Planet Imagermentioning

confidence: 99%

First light of the Gemini Planet Imager

Macintosh

Graham

Ingraham

et al. 2014

Proc. Natl. Acad. Sci. U.S.A.

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589

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The Gemini Planet Imager is a dedicated facility for directly imaging and spectroscopically characterizing extrasolar planets. It combines a very high-order adaptive optics system, a diffractionsuppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spatial resolution. Every aspect of the Gemini Planet Imager has been tuned for maximum sensitivity to faint planets near bright stars. During first-light observations, we achieved an estimated H band Strehl ratio of 0.89 and a 5-σ contrast of 10 6 at 0.75 arcseconds and 10 5 at 0.35 arcseconds. Observations of Beta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing. Beta Pictoris b is observed at a separation of 434 ± 6 milliarcseconds (mas) and position angle 211.8 ± 0.5°. Fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions. The planet orbits at a semimajor axis of 9:0 +0:8 −0:4 AU near the 3:2 resonance with the previously known 6-AU asteroidal belt and is aligned with the inner warped disk. The observations give a 4% probability of a transit of the planet in late 2017.high-contrast imaging | extreme adaptive optics | debris disks D irect imaging is a powerful complement to indirect exoplanet detection techniques. In direct imaging, the planet is spatially resolved from its star, allowing it to be independently studied. This capability opens up new regions of parameter space, including sensitivity to planets at >5 AU. It also allows spectroscopic analysis of the light emitted or reflected by the planet to determine its composition (1, 2) and astrometry to determine the full Keplerian orbital elements (3, 4).Imaging planets is extremely challenging-Jupiter is 10 9 times fainter than our sun in reflected visible light. Younger extrasolar planets are more favorable targets. During their formation, planets are heated by the release of gravitational potential energy. Depending on the exact formation process and initial conditions, a 4-Jupiter mass ðM J Þ planet at an age of 10 million years could have a luminosity between 10 −6 and 2 × 10 −5 L ⊙ (5), but this is still a formidable contrast ratio. To overcome this, astronomers combined large telescopes (to reduce the impact of diffraction), adaptive optics (to correct for phase errors induced by atmospheric turbulence), and sophisticated image processing (6, 7). This recipe in various combinations had achieved several notable successes (8-12). However, the rate of these discoveries remains low (13-15) in part because the number of suitable young stars in the solar neighborhood is low, and for all but the closest stars, such detection is limited to >20 AU, where planets may be relatively rare. To move beyond this limited sample, dedicated instruments are needed that are designed specifically for high-contrast imaging. One such instrument is the Gemini Planet Imager (GPI). GPI is a fully optimized high-con...

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Section: Design Of the Gemini Planet Imagermentioning

confidence: 99%

First light of the Gemini Planet Imager

Macintosh

Graham

Ingraham

et al. 2014

Proc. Natl. Acad. Sci. U.S.A.

Self Cite

589

412

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“…In the Solar System, the ice giants Uranus and Neptune, with core (here ice and rock) masses of ∼ 13−15 M ⊕ , argue for the latter possibility. Ongoing exoplanet imaging surveys and their successors (Hinz et al 2012;Macintosh et al 2012;Close et al 2014) will help discriminate among the various planet formation pathways in the outskirts of protoplanetary disks.…”

Section: Equation Of Statementioning

confidence: 99%

On the Minimum Core Mass for Giant Planet Formation at Wide Separations

Piso

Youdin

2014

ApJ

226

270

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In the core accretion hypothesis, giant planets form by gas accretion onto solid protoplanetary cores. The minimum (or critical) core mass to form a gas giant is typically quoted as 10M ⊕ . The actual value depends on several factors: the location in the protoplanetary disk, atmospheric opacity, and the accretion rate of solids. Motivated by ongoing direct imaging searches for giant planets, this study investigates core mass requirements in the outer disk. To determine the fastest allowed rates of gas accretion, we consider solid cores that no longer accrete planetesimals, as this would heat the gaseous envelope. Our spherical, two-layer atmospheric cooling model includes an inner convective region and an outer radiative zone that matches onto the disk. We determine the minimum core mass for a giant planet to form within a typical disk lifetime of 3 Myr. The minimum core mass declines with disk radius, from ∼8.5M ⊕ at 5 AU to ∼3.5M ⊕ at 100 AU, with standard interstellar grain opacities. Lower temperatures in the outer disk explain this trend, while variations in disk density are less influential. At all distances, a lower dust opacity or higher mean molecular weight reduces the critical core mass. Our non-self-gravitating, analytic cooling model reveals that self-gravity significantly affects early atmospheric evolution, starting when the atmosphere is only ∼10% as massive as the core.

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“…Yet, since the initial promising discoveries of Fomalhaut b 1 and HR8799 b,c,d,e 2 less than 10 years ago, the number of newly imaged planetary mass objects with HCI has not exceeded a dozen. This is in spite of the recent commissioning of several secondgeneration so-called "planet-imager" instruments, including the Gemini Planet Imager (GPI), 3 the Spectro-Polarimetric High contrast Exoplanet Research (SPHERE) instrument, 4 and the Subaru Extreme-Adaptive Optics (SCExAO) facility. 5,6 These near-infrared (NIR) HCI instruments incorporate the latest Adaptive Optics (AO) systems to correct for the atmospheric turbulences, to reach the extreme AO regime with Strehl ratio in excess of 0.8.…”

Section: Introductionmentioning

confidence: 99%

SLM-based digital adaptive coronagraphy: current status and capabilities

Kühn

Patapis

et al. 2018

Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III

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Active coronagraphy is deemed to play a key role for the next generation of high-contrast instruments, notably in order to deal with large segmented mirrors that might exhibit time-dependent pupil merit function, caused by missing or defective segments. To this purpose, we recently introduced a new technological framework called digital adaptive coronagraphy (DAC), making use of liquid-crystal spatial light modulators (SLMs) display panels operating as active focal-plane phase mask coronagraphs. Here, we first review the latest contrast performance, measured in laboratory conditions with monochromatic visible light, and describe a few potential pathways to improve SLM coronagraphic nulling in the future. We then unveil a few unique capabilities of SLM-based DAC that were recently, or are currently in the process of being, demonstrated in our laboratory, including NCPA wavefront sensing, aperture-matched adaptive phase masks, coronagraphic nulling of multiple star systems, and coherent differential imaging (CDI).

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The Gemini Planet Imager: integration and status

Cited by 30 publications

References 6 publications

First light of the Gemini Planet Imager

First light of the Gemini Planet Imager

On the Minimum Core Mass for Giant Planet Formation at Wide Separations

SLM-based digital adaptive coronagraphy: current status and capabilities

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