The Gemini Planet Imager: from science to design to construction

Macintosh, Bruce; Graham, James R.; Palmer, David; Doyon, René; Dunn, Jennifer; Gavel, Donald T.; Larkin, James E.; Oppenheimer, Ben R.; Saddlemyer, Les; Sivaramakrishnan, Anand; Wallace, J. Kent; Bauman, Brian; Erickson, Darren; Marois, Christian; Poyneer, Lisa; Soummer, Rémi

doi:10.1117/12.788083

Cited by 231 publications

(109 citation statements)

References 16 publications

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“…The findings presented herein are the result of more than 15 years of high-precision Doppler monitoring of nearby stars. Additional information will soon pour in from other surveys using techniques such as microlensing (e.g., Dong et al 2009;Gould et al 2010), astrometry (Boss et al 2009), transits (Borucki et al 2004;Barge et al 2008;Irwin et al 2009), and direct imaging (Claudi et al 2006;Artigau et al 2008;Macintosh et al 2008).…”

Section: Summary and Discussionmentioning

confidence: 99%

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Johnson¹,

Aller²,

Howard³

et al. 2010

PUBL ASTRON SOC PAC

767

824

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ABSTRACT. Correlations between stellar properties and the occurrence rate of exoplanets can be used to inform the target selection of future planet-search efforts and provide valuable clues about the planet-formation process. We analyze a sample of 1266 stars drawn from the California Planet Survey targets to determine the empirical functional form describing the likelihood of a star harboring a giant planet as a function of its mass and metallicity. Our stellar sample ranges from M dwarfs with masses as low as 0:2 M ⊙ to intermediate-mass subgiants with masses as high as 1:9 M ⊙ . In agreement with previous studies, our sample exhibits a planet-metallicity correlation at all stellar masses; the fraction of stars that harbor giant planets scales as f ∝ 10 1:2½Fe=H . We can rule out a flat metallicity relationship among our evolved stars (at 98% confidence), which argues that the high metallicities of stars with planets is not likely due to convective envelope "pollution." Our data also rule out a constant planet occurrence rate for ½Fe=H < 0, indicating that giant planets continue to become rarer at sub-Solar metallicities. We also find that planet occurrence increases with stellar mass (f ∝ M ⋆ ), characterized by a rise from 3% around M dwarfs (0:5 M ⊙ ) to 14% around A stars (2 M ⊙ ), at Solar metallicity. We argue that the correlation between stellar properties and giant planet occurrence is strong supporting evidence of the core-accretion model of planet formation.

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Section: Summary and Discussionmentioning

confidence: 99%

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Johnson¹,

Aller²,

Howard³

et al. 2010

PUBL ASTRON SOC PAC

767

824

View full text Add to dashboard Cite

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“…Then, using these simulated images, COFFEE perform the aberration estimation assuming a PSD following a 1/ν 2 power law (as described in Section 2.2). 2 2.28 nm RMS 4.09 nm RMS S φ k ∝ 1/ν 3 1.54 nm RMS 3.40 nm RMS Table 2. Comparison of COFFEE's estimation accuracy when the a priori knowledge on the aberration's PSD is not perfectly accurate.…”

Section: Sensitivity To the A Priori Assumption Accuracymentioning

confidence: 99%

“…The observation of an extremely faint object (the planet) very close to a bright source (the host star) requires the use of an extreme adaptive optics (XAO) system coupled with a high-contrast imaging technique such as coronagraphy. The current generation of instruments dedicated to exoplanets direct imaging (SPHERE on the VLT [1], GPI on Gemini South [2], Subaru SCExAO [3] and Palomar P1640 [4]) aim at detecting massive gaseous planets 10 −6 to 10 −7 times fainter than their host star. In the future, high-contrast imaging instruments on ground based or space based telescopes will perform observation of Earth-like planets, 10 −9 to 10 −10 times fainter than their host star.…”

Section: Introductionmentioning

confidence: 99%

High-order myopic coronagraphic phase diversity (COFFEE) for wave-front control in high-contrast imaging systems

Paul¹,

Mugnier²,

Sauvage³

et al. 2013

Opt. Express

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Abstract:The estimation and compensation of quasi-static aberrations is mandatory to reach the ultimate performance of high-contrast imaging systems. COFFEE is a focal plane wave-front sensing method that consists in the extension of phase diversity to high-contrast imaging systems. Based on a Bayesian approach, it estimates the quasi-static aberrations from two focal plane images recorded from the scientific camera itself. In this paper, we present COFFEE's extension which allows an estimation of low and high order aberrations with nanometric precision for any coronagraphic device. The performance is evaluated by realistic simulations, performed in the SPHERE instrument framework. We develop a myopic estimation that allows us to take into account an imperfect knowledge on the used diversity phase. Lastly, we evaluate COFFEE's performance in a compensation process, to optimize the contrast on the detector, and show it allows one to reach the 10 −6 contrast required by SPHERE at a few resolution elements from the star. Notably, we present a non-linear energy minimization method which can be used to reach very high contrast levels (better than 10 7 in a SPHERE-like context).

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“…Following the science requirements for VLT/SPHERE and Gemini/GPI (Mesa et al 2011;Macintosh et al 2008) we use a residual stellar PSF of 10 −7 at a separation of 1 ′′ , and a read-noise of 10 electrons to simulate the ∼ 100 SNR J-band photometry (with added normally distributed noise of 1%, see below) for model B2 shown in the middle panel of Figure 8. We note that the high Strehl ratio provided by the Extreme AO (up to 80%) reduces the speckle noise to such low levels that the limiting factors for the detection of photometric variability will be the photometric precision, read noise and instrument stability.…”

Section: -M Class Telescopes With Next-generation Extreme Aomentioning

confidence: 99%

Mapping Directly Imaged Giant Exoplanets

Kostov

Apai

2012

ApJ

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With the increasing number of directly imaged giant exoplanets the current atmosphere models are often not capable of fully explaining the spectra and luminosity of the sources. A particularly challenging component of the atmosphere models is the formation and properties of condensate cloud layers, which fundamentally impact the energetics, opacity, and evolution of the planets.Here we present a suite of techniques that can be used to estimate the level of rotational modulations these planets may show. We propose that the timeresolved observations of such periodic photometric and spectroscopic variations of extrasolar planets due to their rotation can be used as a powerful tool to probe the heterogeneity of their optical surfaces. In this paper we develop simulations to explore the capabilities of current and next-generation ground-and space-based instruments for this technique. We address and discuss the following questions: a) what planet properties can be deduced from the light curve and/or spectra, and in particular can we determine rotation periods, spot-coverage, spot colors, spot spectra; b) what is the optimal configuration of instrument/wavelength/temporal sampling required for these measurements; and, c) can principal component analysis be used to invert the light curve and deduce the surface map of the planet.1 To whom correspondence should be addressed. Email: vkostov@pha.jhu.edu -2 -Our simulations describe the expected spectral differences between homogeneous (clear or cloudy) and patchy atmospheres, outline the significance of the dominant absorption features of H 2 O, CH 4 , and CO and provide a method to distinguish these two types of atmospheres. Assuming surfaces with and without clouds for most currently imaged planets the current models predict the largest variations in the J-band. Simulated photometry from current and future instruments is used to estimate the level of detectable photometric variations. We conclude that future instruments will be able to recover not only the rotation periods, cloud cover, cloud colors and spectra but even cloud evolution. We also show that a longitudinal map of the planet's atmosphere can be deduced from its disk-integrated light curves.

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The Gemini Planet Imager: from science to design to construction

Cited by 231 publications

References 16 publications

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

High-order myopic coronagraphic phase diversity (COFFEE) for wave-front control in high-contrast imaging systems

Mapping Directly Imaged Giant Exoplanets

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