GPI 2.0: upgrading the Gemini Planet Imager

Chilcote, Jeffrey; Konopacky, Quinn; Rosa, Robert J. De; Hamper, Randall; Macintosh, Bruce; Marois, Christian; Perrin, Marshall D.; Savransky, Dmitry; Soummer, Rémi; Véran, Jean-Pierre; Agapito, Guido; Aleman, Arlene; Ammons, Mark; Bonaglia, Marco; Boucher, Marc-André; Curliss, Maeve; Dunn, Jennifer; Esposito, Simone; Filion, Guillaume; Fitzsimmons, Joeleff; Kain, Isabel; Kerley, Dan; Landry, Jean-Thomas; Lardière, Olivier; Lemoine-Busserolle, Marie; Li, Duan; Limbach, Mary Anne; Madurowicz, Alex; Maire, Jérôme; N’Diaye, Mamadou; Nielsen, Eric L.; Poyneer, Lisa; Pueyo, Laurent; Summey, Kaitlyn; Thomas, Coleman

doi:10.1117/12.2562578

Cited by 12 publications

(6 citation statements)

References 34 publications

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“…For the first time, these instruments are designed from the beginning as fully integrated systems composed of starlight rejection devices (coronagraphs), wavefront controllers (adaptive optics and focal plane wavefront control) and post-processing techniques, all working with each others. For ground-based telescopes, the instruments will associate coronagraphy, extreme adaptive optics and focal plane wavefront control: SPHERE+ [221] and GPI2.0 [222]. These instruments will probe closer regions to the stars, where multiple exoplanets are expected to be.…”

Section: Discussionmentioning

confidence: 99%

Imaging exoplanets with coronagraphic instruments

Galicher¹,

Mazoyer²

2024

Comptes Rendus. Physique

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Exoplanetary science is a very active field of astronomy nowadays, with questions still opened such as how planetary systems form and evolve (occurrence, process), why such a diversity of exoplanets is observed (mass, radius, orbital parameters, temperature, composition), and what are the interactions between planets, circumstellar disk and their host star. Several complementary methods are used for the detection of exoplanets. Among these, imaging aims at the direct detection of the light reflected, scattered or emitted by exoplanets and circumstellar disks. This allows their spectral and polarimetric characterization. Such imaging remains challenging because of the large luminosity ratio (10 4 -10 10 ) and the small angular separation (fraction of an arcsecond) between the star and its environment. Over the past two decades, numerous techniques, including coronagraphy, have been developed to make exoplanet imaging a reality.This paper gives a broad overview of the subsystems that make up a coronagraphic instrument for imaging exoplanetary systems. It is especially intended for non-specialists or newcomers in the field. We explain the principle of coronagraphy and propose a formalism to understand their behavior. We discuss the impact of wavefront aberrations on the performance of coronagraphs and how they induce stellar speckles in the scientific image. Finally, we present instrumental and signal processing techniques used for on-sky minimization or a posteriori calibration of these speckles in order to improve the performance of coronagraphs.Résumé. L'exoplanétologie est un domaine très actif de l'astronomie moderne avec des questions encore ouvertes : comment les systèmes planétaires se forment-ils et évoluent-ils ; pourquoi une telle diversité d'exoplanètes est-elle observée (masse, rayon, paramètres orbitaux, température, composition) ; quelles sont les interactions entre les planètes, les disques circumstellaires et leur étoile hôte ? Plusieurs méthodes complémentaires sont utilisées pour la détection d'exoplanètes. Parmi celles-ci, l'imagerie permet la détection directe de la lumière réfléchie, diffusée ou émise par les exoplanètes et les disques circumstellaires. Ceci permet une caractérisation spectrale et polarimétrique. Obtenir une image d'exoplanète n'est cependant pas simple en raison du grand rapport de luminosité (10 4 -10 10 ) et de la faible séparation angulaire (fraction de seconde d'angle) entre l'étoile et son environnement. Depuis deux décennies, de nombreuses techniques, dont la coronographie, ont été développées pour faire de l'imagerie des exoplanètes une réalité.

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Section: Discussionmentioning

confidence: 99%

Imaging exoplanets with coronagraphic instruments

Galicher¹,

Mazoyer²

2024

Comptes Rendus. Physique

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“…Typically a large telescope is needed along with a coronagraph to block the diffracted star light while letting the light from around the star to pass. There are several groundbased observatories and instruments designed for this type of measurement: the Gemini Planet Imager [7,8], SPHERE [9], SCExAO [10,11], Project 1640 and the Stellar Double Coro nagraph [12,13], the Keck Planet Imager and Characterizer [14], and MagAOX [15].…”

Section: Direct Imagingmentioning

confidence: 99%

“…Titanium nitride was one of the first resistive superconductors with 𝑇 𝑐 < 10 K to be used in superconducting detectors [126]. By varying the relative percentage of nitrogen to titanium, the transition temperature can be tuned from 0.7 to 4.5 K. These films also can have very high internal quality factors >10 7 .…”

Section: Titanium Nitridementioning

confidence: 99%

Improving the Resolving Power of Ultraviolet to Near-Infrared Microwave Kinetic Inductance Detectors

Zobrist¹

2022

Springer Theses

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dark matter searches to biological imaging and astronomy. The performance of these de tectors often limits the achievable science goals for an application, so improvements to detector technologies can be transformative. This dissertation focuses on these detector enhancements, emphasizing the requirements for one particular application, exoplanet di rect imaging. However, the work done here remains broadly applicable to fields needing highly sensitive sensors in this wavelength range.Finding and studying the properties of exoplanets orbiting distant stars can tell us much about solar system dynamics and the formation of our own solar system. With sufficiently precise measurements we might also discover the presence of water or even biological processes on these planets. To achieve this goal, we need astronomical instrumentation ca pable of separating an exoplanet's light from its host star by directly imaging it. For many exoplanets, though, we receive at our telescope only roughly one photon for every billion from the star. Even worse, these two light sources often partially overlap because of the relative closeness of exoplanets to their stars and the diffraction limit set by the finite size xi of our telescope optics. Therefore, the extreme contrast ratio between the brightness of the star and planet sets the performance requirements for this kind of instrument.Carrying out this measurement with the traditional semiconductor based sensors can be difficult. They detect the intensity of light at each pixel and introduce excess noise into the system. However, superconducting sensors avoid this limitation because of their ex tra sensitivity. Each individual incident photon can be resolved making them essentially perfect photon counting detectors, which enables the detection of exoplanets with more challenging contrast ratios than detectable with conventional detectors. The system noise in a superconducting sensor, instead, determines how accurately the photon energy can be measured through the size of the detector response. Because of this extra energy measure ment capability these detectors do not need the complicated optical systems typically used to measure an exoplanet's atmospheric spectrum. The accuracy at which we can resolve these planetary spectra determines how much we can learn about a planet and, as such, is the principal metric for the performance of these devices.The Microwave Kinetic Inductance Detector (MKID) is unique among other supercon ducting technologies because it allows for the simple readout of tens to hundreds of thou sands of pixels, which is a requirement for when the exact location of an exoplanet is un known. This dissertation focuses on improving the spectral resolving power of MKIDs to make them the superior option for ultraviolet to nearinfrared measurements and, in partic ular, for exoplanet direct imaging. Chapters 1 and 2 discuss the significance of MKIDs as astronomical detectors and the relevant physics needed to understand their operation. In the following chapters, four sepa...

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“…The Gemini Planet Imager 10 is an integral field spectrograph and coronagraph that is in the process of being upgraded and moved from its current mount behind the Cassegrain focus of the 8.1m Gemini South Telescope to a similar position on the telescope's twin, Gemini North, as part of the instrument's upgrade process -GPI 2.0. 11 The APLC-Optimization toolkit was recently used to develop new apodizer and Lyot stop masks as part of the GPI 2.0 upgrade. 8,12 These updated apodizers were optimized to achieve better high-contrast imaging performance, such as deeper raw contrast at the IWA of the dark zone, and increased robustness to Lyot stop misalignments.…”

Section: Gpimentioning

confidence: 99%

APLC-optimization: an apodized pupil Lyot coronagraph design survey toolkit

Nickson¹,

Por²,

Nguyen³

et al. 2022

Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter Wave

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We present a publicly available software package developed for exploring apodized pupil Lyot coronagraph (APLC) solutions for various telescope architectures. In particular, the package optimizes the apodizer component of the APLC for a given focal-plane mask and Lyot stop geometry to meet a set of constraints (contrast, bandwidth etc.) on the coronagraph intensity in a given focal-plane region (i.e. dark zone). The package combines a high-contrast imaging simulation package (HCIPy 1 ) with a third-party mathematical optimizer (Gurobi) to compute the linearly optimized binary mask that maximizes transmission. We provide examples of the application of this toolkit to several different telescope geometries, including the Gemini Planet Imager (GPI) and the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed. Finally, we summarize the results of a preliminary design survey for the case of a ∼6 m aperture off-axis space telescope, as recommended by the 2020 NASA Decadal Survey, exploring APLC solutions for different segment sizes. We then use the Pair-based Analytical model for Segmented Telescope Imaging from Space (PASTIS) to perform a segmented wavefront error tolerancing analysis on these solutions.

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GPI 2.0: upgrading the Gemini Planet Imager

Cited by 12 publications

References 34 publications

Imaging exoplanets with coronagraphic instruments

Imaging exoplanets with coronagraphic instruments

Improving the Resolving Power of Ultraviolet to Near-Infrared Microwave Kinetic Inductance Detectors

APLC-optimization: an apodized pupil Lyot coronagraph design survey toolkit

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