Franck Marchis

Franck Marchis

Mountain View, California, United States
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Publications

  • First light of the Gemini Planet imager.

    Proceedings of the National Academy of Sciences of the United States of America

    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 diffraction-suppressing 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…

    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 diffraction-suppressing 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 [Formula: see text] 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.

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  • An Adaptive Image Deconvolution Algorithm (AIDA) with Application to Multi-Frame and Three-Dimensional Data

    Journal of the Optical Society of America, A. 24:1580-1600

    We describe an adaptive image deconvolution algorithm (AIDA) for myopic deconvolution of multi-frame and three-dimensional data acquired through astronomical and microscopic imaging. AIDA is a reimplementation and extension of the MISTRAL method developed by Mugnier and co-workers and shown to yield object reconstructions with excellent edge preservation and photometric precision [J. Opt. Soc. Am. A21, 1841 (2004)]. Written in Numerical Python with calls to a robust constrained conjugate…

    We describe an adaptive image deconvolution algorithm (AIDA) for myopic deconvolution of multi-frame and three-dimensional data acquired through astronomical and microscopic imaging. AIDA is a reimplementation and extension of the MISTRAL method developed by Mugnier and co-workers and shown to yield object reconstructions with excellent edge preservation and photometric precision [J. Opt. Soc. Am. A21, 1841 (2004)]. Written in Numerical Python with calls to a robust constrained conjugate gradient method, AIDA has significantly improved run times over the original MISTRAL implementation. Included in AIDA is a scheme to automatically balance maximum-likelihood estimation and object regularization, which significantly decreases the amount of time and effort needed to generate satisfactory reconstructions. We validated AIDA using synthetic data spanning a broad range of signal-to-noise ratios and image types and demonstrated the algorithm to be effective for experimental data from adaptive optics-equipped telescope systems and wide-field microscopy.

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  • Shape, Size. And Multiplicity of Main-Belt Asteroids I. Keck Adaptive Optics Survey.

    Icarus (International Journal of Solar System Studies) 185:39-63

    This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an…

    This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × R(Hill) (1/4 × R(Hill)) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6-8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450-464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to ...

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  • A low density of 0.8 g cm-3 for the Trojan binary asteroid 617 Patroclus

    Nature

    The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter-Sun system (leading and following Jupiter by 60°). The asteroid 617Patroclus is the only known binary Trojan. The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680km, move around the system's centre of mass, describing a roughly circular orbit. Using this orbital information, combined…

    The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter-Sun system (leading and following Jupiter by 60°). The asteroid 617Patroclus is the only known binary Trojan. The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680km, move around the system's centre of mass, describing a roughly circular orbit. Using this orbital information, combined with thermal measurements to estimate the size of the components, we derive a very low density of 0.8 - 0.1 + 0.2gcm-3. The components of 617Patroclus are therefore very porous or composed mostly of water ice, suggesting that they could have been formed in the outer part of the Solar System.

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Projects

  • Artist Impression Sylvia Asteroid - SETI Institute Press Release

    Artist Impression Sylvia Asteroid and press-release for the SETI Institute and the W.M. Keck Observatory

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  • Kepler 62 - SETI Institute press-release

    Artist Impression / Illustration Kepler 62 System.

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  • SETI Instituto Twitter Account

    Translated tweets in spanish of @SETIInstitute.

    Other creators
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  • Adaptive Image Deconvolution Package (AIDA) Home Page

    development of a deconvolution algorithm to enhance the quality of images collected with adaptive optics systems, Hubble Space Telescope and fluorescence microscopy instruments

    Other creators
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  • First density measurement of a Trojan asteroid. The origin of 617 Patroclus-Menoetius

    -

    The Trojan population consists of two swarms of asteroidsfollowing the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter–Sun system (leading and following Jupiter by 60°).The asteroid 617 Patroclus is the only known binary Trojan.The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system’s centre of mass, describing a roughly circular orbit.
    Using this orbital information…

    The Trojan population consists of two swarms of asteroidsfollowing the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter–Sun system (leading and following Jupiter by 60°).The asteroid 617 Patroclus is the only known binary Trojan.The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system’s centre of mass, describing a roughly circular orbit.
    Using this orbital information, combined with thermal measurementsto estimate the size ofthe components, we derive a very low density of 0.8 +0.2−0.1 g cm−3.The components of 617 Patroclus are therefore very porous or composed mostly of water ice,suggesting that they could have been formed in the outer part of the Solar System

    Other creators
    • mike wong
    • Peter Wizinovich
    • Lynette Cook
    • Robert Sanders
    • David Le Mignant
    See project

Languages

  • French

    -

  • Spanish

    -

Organizations

  • VR2Planets

    Scientific Advisor

    - Present
  • PLANETS Foundation

    Scientific Advisor

    - Present

    Founded by a small international group of academic scientists, we aim to build a new class of optical telescope powerful enough to see continents on exoplanets like Proxima b. This new telescope can detect a wide range of biosignatures of simple and advanced life on several hundred exoplanets. Our members span the globe from from Canada, France, Germany, Japan, Mexico, and the United States. The PLANETS Foundation was formed with the mission of accelerating exolife studies while engaging the…

    Founded by a small international group of academic scientists, we aim to build a new class of optical telescope powerful enough to see continents on exoplanets like Proxima b. This new telescope can detect a wide range of biosignatures of simple and advanced life on several hundred exoplanets. Our members span the globe from from Canada, France, Germany, Japan, Mexico, and the United States. The PLANETS Foundation was formed with the mission of accelerating exolife studies while engaging the general public in finding life beyond Earth.

  • Union of Concerned Scientists

    Member

    - Present
  • American Astronomical Society

    Member

    - Present
  • American Geophysical Union

    Member

    - Present

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