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15 results on '"Nemanja Jovanovic"'

1. Multiband Imaging of the HD 36546 Debris Disk: A Refined View from SCExAO/CHARIS*

Author

Kellen Lawson, Thayne Currie, John P. Wisniewski, Motohide Tamura, Jean-Charles Augereau, Timothy D. Brandt, Olivier Guyon, N. Jeremy Kasdin, Tyler D. Groff, Julien Lozi, Vincent Deo, Sebastien Vievard, Jeffrey Chilcote, Nemanja Jovanovic, Frantz Martinache, Nour Skaf, Thomas Henning, Gillian Knapp, Jungmi Kwon, Michael W. McElwain, Tae-Soo Pyo, Michael L. Sitko, Taichi Uyama, Kevin Wagner, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, National Astronomical Observatory of Japan (NAOJ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), University of California [Santa Barbara] (UCSB), University of California, Princeton University, NASA Goddard Space Flight Center (GSFC), National Astronomical Observatory of Japan, Subaru Telescope, 650 North A‘ohoku Place, Hilo, HI 96720, United States, University of Notre Dame [Indiana] (UND), California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, ISAS/JAXA, and NASA

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), 010309 optics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the first multi-wavelength (near-infrared; $1.1 - 2.4$ $\mu m$) imaging of HD 36546's debris disk, using the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). As a 3-10 Myr old star, HD 36546 presents a rare opportunity to study a debris disk at very early stages. SCExAO/CHARIS imagery resolves the disk over angular separations of $\rho \sim 0.25" - 1.0"$ (projected separations of $\rm{r_{proj}} \sim 25 - 101$ $\rm{au}$) and enables the first spectrophotometric analysis of the disk. The disk's brightness appears symmetric between its eastern and western extents and it exhibits slightly blue near-infrared colors on average (e.g. $J-K =-0.4\pm0.1$) $-$ suggesting copious sub-micron sized or highly porous grains. Through detailed modeling adopting a Hong scattering phase function (SPF), instead of the more common Henyey-Greenstein function, and using the differential evolution optimization algorithm, we provide an updated schematic of HD 36546's disk. The disk has a shallow radial dust density profile ($\alpha_{in} \approx 1.0$ and $\alpha_{out} \approx -1.5$), a fiducial radius of $r_0 \approx 82.7$ au, an inclination of $i \approx 79.1^\circ$, and a position angle of $\rm PA \approx 80.1^\circ$. Through spine tracing, we find a spine that is consistent with our modeling, but also with a "swept-back wing" geometry. Finally, we provide constraints on companions, including limiting a companion responsible for a marginal Hipparcos-Gaia acceleration to a projected separation of $\lesssim 0.2''$ and to a minimum mass of $\lesssim 11$ $\rm M_{Jup}$., Comment: 23 pages, 19 figures; corrected an error in the abstract, added a reference in Section 2

Published
2021
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2. Focal plane wavefront sensing on SUBARU/SCExAO

Author

Aurélie Montmerle-Bonnefois, Frédéric Cassaing, Nemanja Jovanovic, Laurent M. Mugnier, Alison Wong, Vincent Deo, Frans Snik, Sébastien Vievard, Coline Lopez, Michael J. Wilby, Barnaby Norris, Steven P. Bos, Thayne Currie, Christoph U. Keller, Mamadou N'Diaye, Jean-François Sauvage, Nour Skaf, Frantz Martinache, Olivier Guyon, Masen Lamb, Ananya Sahoo, Kelsey Miller, Julien Lozi, National Astronomical Observatory of Japan (NAOJ), Astrobiology Center of Nins, DTIS, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, California Institute of Technology (CALTECH), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], DOTA, ONERA, Université Paris Saclay [Châtillon], Schreiber, Laura, Schmidt, Dirk, and Vernet, Elise

Subjects
High contrast imaging, LOW WIND EFFECT, FOS: Physical sciences, 01 natural sciences, 010309 optics, [SPI]Engineering Sciences [physics], Optics, Wind effect, 0103 physical sciences, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Focal plane wavefront sensing, Physics, Wavefront, [PHYS]Physics [physics], [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], business.industry, CORONOGRAPHY, Detector, Spiders, SCEXAO, Cardinal point, CORONAGRAPHY, Adaptive optics systems, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Focal plane wavefront sensing is an elegant solution for wavefront sensing since near-focal images of any source taken by a detector show distortions in the presence of aberrations. Non-Common Path Aberrations and the Low Wind Effect both have the ability to limit the achievable contrast of the finest coronagraphs coupled with the best extreme adaptive optics systems. To correct for these aberrations, the Subaru Coronagraphic Extreme Adaptive Optics instrument hosts many focal plane wavefront sensors using detectors as close to the science detector as possible. We present seven of them and compare their implementation and efficiency on SCExAO. This work will be critical for wavefront sensing on next generation of extremely large telescopes that might present similar limitations., Comment: SPIE proceeding : Astronomical Telescopes + Instrumentation 2020. arXiv admin note: text overlap with arXiv:1912.10179

Published
2020
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3. SCExAO/CHARIS Direct Imaging Discovery of a 20 au Separation, Low-mass Ratio Brown Dwarf Companion to an Accelerating Sun-like Star *

Author

Trent J. Dupuy, John P. Wisniewski, Carol A. Grady, Vincent Deo, Gillian R. Knapp, Michael W. McElwain, Jungmi Kwon, Matthew Wahl, Daniel Michalik, Kevin Wagner, Masayuki Kuzuhara, Yunlin Zeng, Markus Janson, Sébastien Vievard, Kellen Lawson, Nemanja Jovanovic, Olivier Guyon, Yiting Li, Julien Lozi, Michael Letawsky, Taichi Uyama, Tyler D. Groff, Timothy D. Brandt, Ananya Sahoo, Jeffery Chilcote, Frantz Martinache, Thayne Currie, G. Mirek Brandt, Motohide Tamura, Christian Marois, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, National Astronomical Observatory of Japan (NAOJ), Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, University of Victoria [Canada] (UVIC), NASA, National Astronomical Observatory of Japan, Subaru Telescope, 650 North A‘ohoku Place, Hilo, HI 96720, United States, California Institute of Technology (CALTECH), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Institut de Mathématiques de Marseille (I2M), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, Photometry (optics), Observatory, 0103 physical sciences, direct imaging (387), 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), astronomical instrumentation (799), Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), astronomical techniques (1684), Astronomy and Astrophysics, brown dwarfs (185), Astrometry, Mass ratio, exoplanet detection methods (489), Exoplanet, coronagraphic imaging (313), astronomical optics (88), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, exoplanets (498), Low Mass, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the direct imaging discovery of a substellar companion to the nearby Sun-like star, HD 33632 Aa, at a projected separation of $\sim$ 20 au, obtained with SCExAO/CHARIS integral field spectroscopy complemented by Keck/NIRC2 thermal infrared imaging. The companion, HD 33632 Ab, induces a 10.5$\sigma$ astrometric acceleration on the star as detected with the $Gaia$ and $Hipparcos$ satellites. SCExAO/CHARIS $JHK$ (1.1--2.4 $\mu$m) spectra and Keck/NIRC2 $L_{\rm p}$ (3.78 $\mu$m) photometry are best matched by a field L/T transition object: an older, higher gravity, and less dusty counterpart to HR 8799 cde. Combining our astrometry with $Gaia/Hipparcos$ data and archival Lick Observatory radial-velocities, we measure a dynamical mass of 46.4 $\pm$ 8 $M_{\rm J}$ and an eccentricity of $e$ $, Comment: 11 pages, 3 figures, 2 tables; ApJ Letters in press. First discovery from SCExAO/CHARIS; first substellar companion discovered through direct imaging using Gaia for target selection

Published
2020
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4. Precision Photometric and Astrometric Calibration Using Alternating Satellite Speckles

Author

Nemanja Jovanovic, Ananya Sahoo, Julien Lozi, Tyler D. Groff, F. Martinache, Jeffery Chilcote, Timothy D. Brandt, Olivier Guyon, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, National Astronomical Observatory of Japan (NAOJ), National Astronomical Observatory of Japan, Subaru Telescope, 650 North A‘ohoku Place, Hilo, HI 96720, United States, California Institute of Technology (CALTECH), and NASA

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Deformable mirror, Photometry (optics), Speckle pattern, Optics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, Angular distance, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrometry, Image plane, Starlight, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, business
Abstract

Photometric and astrometric calibration of high-contrast images is essential for the characterization of companions at small angular separation from their stellar host. The main challenge to performing accurate relative photometry and astrometry of high-contrast companions with respect to the host star is that the central starlight cannot be directly used as a reference, as it is either blocked by a coronagraphic mask or saturating the detector. Our approach is to add fiducial incoherent faint copies of the host star in the image plane and alternate the pattern of these copies between exposures. Subtracting two frames with different calibration patterns removes measurement bias due to static and slowly varying incoherent speckle halo components, while ensuring that calibration references are inserted on each frame. Each calibration pattern is achieved by high-speed modulation of a pupil-plane deformable mirror to ensure incoherence. We implemented the technique on-sky on the Subaru Coronagraphic Extreme Adaptive Optics instrument with speckles which were of the order of 103 times fainter than the central host. The achieved relative photometric and astrometric measurement precisions for 10 s exposure were respectively 5% and 20 milliarcsecond. We also demonstrate, over a 540 s measurement span, that residual photometric and astrometric errors are uncorrelated in time, indicating that residual noise averages as the inverse square root of the number of exposures in longer time-series data sets.

Published
2020
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5. High-resolution Near-infrared Polarimetry and Submillimeter Imaging of FS Tau A: Possible Streamers in Misaligned Circumbinary Disk System

Author

Tae-Soo Pyo, Tomoyuki Kudo, Julien Lozi, Olivier Guyon, Ryuji Suzuki, Jungmi Kwon, Masanori Iye, Joseph C. Carson, Hiroshi Suto, Jeffrey Chilcote, Masahiko Hayashi, Takao Nakagawa, Nemanja Jovanovic, Thomas Henning, Christian Thalmann, M. Bonnefoy, Yutaka Hayano, Tetsuo Nishimura, Eugene Serabyn, Miki Ishii, Klaus W. Hodapp, Yang Yang, Tomonori Usuda, Ryo Kandori, Michael W. McElwain, Makoto Watanabe, Eiji Akiyama, Toru Yamada, Taichi Uyama, Masayuki Kuzuhara, Gillian R. Knapp, Nobuhiko Kusakabe, Evan A. Rich, Shoken M. Miyama, Markus Janson, Carol A. Grady, Saeko S. Hayashi, Wolfgang Brandner, Lyu Abe, Jun-Ichi Morino, Jun Hashimoto, Michihiro Takami, Thayne Currie, Timothy D. Brandt, Motohide Tamura, Markus Feldt, Miwa Goto, Naruhisa Takato, Jeremy Kasdin, Tyler D. Groff, Hideki Takami, Edwin L. Turner, John P. Wisniewski, Frantz Martinache, Satoshi Mayama, Ruobing Dong, Hiroshi Terada, Amaya Moro-Martin, Taro Matsuo, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Signal Processing Laboratory (SPL), Wuhan University [China], Hokkaido University [Sapporo, Japan], National Astronomical Observatory of Japan (NAOJ), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, NASA Goddard Space Flight Center (GSFC), California Institute of Technology (CALTECH), The University of Tokyo (UTokyo), Institut méditerranéen de biodiversité et d'écologie marine et continentale (IMBE), Avignon Université (AU)-Aix Marseille Université (AMU)-Institut de recherche pour le développement [IRD] : UMR237-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, and Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France

Subjects
010504 meteorology & atmospheric sciences, Polarimetry, FOS: Physical sciences, Binary number, Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Line (formation), Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Near-infrared spectroscopy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Wavelength, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Circumbinary planet, Astrophysics - Earth and Planetary Astrophysics
Abstract

We analyzed the young (2.8-Myr-old) binary system FS Tau A using near-infrared (H-band) high-contrast polarimetry data from Subaru/HiCIAO and sub-millimeter CO (J=2-1) line emission data from ALMA. Both the near-infrared and sub-millimeter observations reveal several clear structures extending to $\sim$240 AU from the stars. Based on these observations at different wavelengths, we report the following discoveries. One arm-like structure detected in the near-infrared band initially extends from the south of the binary with a subsequent turn to the northeast, corresponding to two bar-like structures detected in ALMA observations with an LSRK velocity of 1.19-5.64 km/s. Another feature detected in the near-infrared band extends initially from the north of the binary, relating to an arm-like structure detected in ALMA observations with an LSRK velocity of 8.17-16.43 km/s. From their shapes and velocities, we suggest that these structures can mostly be explained by two streamers that connect the outer circumbinary disk and the central binary components. These discoveries will be helpful for understanding the evolution of streamers and circumstellar disks in young binary systems., 20 pages, 11 figures, accepted for publication in The Astrophysical Journal

Published
2020
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6. Keck/NIRC2 L'-band Imaging of Jovian-mass Accreting Protoplanets around PDS 70

Author

Nemanja Jovanovic, Sam Ragland, Dimitri Mawet, Olivier Absil, Jacques Robert Delorme, Mikael Karlsson, Jonathan P. Williams, Keith Matthews, François Ménard, Michael C. Liu, Henry Ngo, Andrea M. Ghez, Aïssa Jolivet, Charlotte Z. Bond, Elsa Huby, Bin Ren, Peter Wizinowich, Pontus Forsberg, Scott Lilley, Rebecca Jensen-Clem, Eugene Serabyn, Tiffany Meshkat, Garreth Ruane, Robert J. De Rosa, Denis Defrere, Peter Gao, Ed Wetherell, Ernesto Vargas Catalan, Maxwell A. Millar-Blanchaer, Elodie Choquet, Christophe Pinte, Jason J. Wang, Gilles Orban de Xivry, Carlos Alvarez, Sylvain Cetre, Mark Chun, Ji Wang, Christoph Baranec, Marie Ygouf, Nicole Wallack, Donald N. B. Hall, Barry Zuckerman, Gaspard Duchêne, Sivan Ginzburg, Olivier Guyon, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016)

Subjects
010504 meteorology & atmospheric sciences, DUST, Astrophysics, 01 natural sciences, Orbit determination, Exoplanet formation, RADIATIVE-TRANSFER, Planet, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, TEMPERATURE, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Radius, OPTICAL-PROPERTIES, Astrophysics - Solar and Stellar Astrophysics, Physical Sciences, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, ATMOSPHERES, Coronagraphic imaging, BROWN DWARFS, OPACITIES, Astrophysics::High Energy Astrophysical Phenomena, MODELS, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Jovian, EXTRASOLAR GIANT PLANETS, Photometry (optics), 0103 physical sciences, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Photosphere, Science & Technology, Exoplanet dynamics, EARLY EVOLUTION, Astronomy and Astrophysics, Planetary system, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Protoplanet, Exoplanet atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present $L$'-band imaging of the PDS 70 planetary system with Keck/NIRC2 using the new infrared pyramid wavefront sensor. We detected both PDS 70 b and c in our images, as well as the front rim of the circumstellar disk. After subtracting off a model of the disk, we measured the astrometry and photometry of both planets. Placing priors based on the dynamics of the system, we estimated PDS 70 b to have a semi-major axis of $20^{+3}_{-4}$~au and PDS 70 c to have a semi-major axis of $34^{+12}_{-6}$~au (95\% credible interval). We fit the spectral energy distribution (SED) of both planets. For PDS 70 b, we were able to place better constraints on the red half of its SED than previous studies and inferred the radius of the photosphere to be 2-3~$R_{Jup}$. The SED of PDS 70 c is less well constrained, with a range of total luminosities spanning an order of magnitude. With our inferred radii and luminosities, we used evolutionary models of accreting protoplanets to derive a mass of PDS 70 b between 2 and 4 $M_{\textrm{Jup}}$ and a mean mass accretion rate between $3 \times 10^{-7}$ and $8 \times 10^{-7}~M_{\textrm{Jup}}/\textrm{yr}$. For PDS 70 c, we computed a mass between 1 and 3 $M_{\textrm{Jup}}$ and mean mass accretion rate between $1 \times 10^{-7}$ and $5 \times~10^{-7} M_{\textrm{Jup}}/\textrm{yr}$. The mass accretion rates imply dust accretion timescales short enough to hide strong molecular absorption features in both planets' SEDs., Comment: 20 pages, 5 figures, Accepted to AJ. Updated author list from original version. Fixed equation typo

Published
2020
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7. Visible and Near-infrared Laboratory Demonstration of a Simplified Pyramid Wavefront Sensor

Author

Shane Jacobson, Olivier Guyon, Frantz Martinache, Julien Lozi, Nemanja Jovanovic, Mark Chun, Sean Goebel, National Astronomical Observatory of Japan (NAOJ), Département Sciences de la Fabrication et Logistique (SFL-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-CMP-GC, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Engineering, 010504 meteorology & atmospheric sciences, business.industry, FOS: Physical sciences, Astronomy and Astrophysics, High contrast imaging, Wavefront sensor, 01 natural sciences, Astronomical instrumentation, Contingency Fund, Space and Planetary Science, 0103 physical sciences, Pyramid, Astrophysics - Instrumentation and Methods for Astrophysics, Adaptive optics, Subaru Telescope, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Remote sensing
Abstract

Wavefront sensing and control are important for enabling one of the key advantages of using large apertures, namely higher angular resolutions. Pyramid wavefront sensors are becoming commonplace in new instrument designs owing to their superior sensitivity. However, one remaining roadblock to their widespread use is the fabrication of the pyramidal optic. This complex optic is challenging to fabricate due to the pyramid tip, where four planes need to intersect in a single point. Thus far, only a handful of these have been produced due to the low yields and long lead times. To address this, we present an alternative implementation of the pyramid wavefront sensor that relies on two roof prisms instead. Such prisms are easy and inexpensive to source. We demonstrate the successful operation of the roof prism pyramid wavefront sensor on a 8-m class telescope, at visible and near infrared wavelengths ---for the first time using a SAPHIRA HgCdTe detector without modulation for a laboratory demonstration---, and elucidate how this sensor can be used more widely on wavefront control test benches and instruments., Comment: Accepted for publication in PASP, 7 pages, 9 figures, 1 table

Published
2019
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8. Measurements of Speckle Lifetimes in Near-infrared Extreme Adaptive Optics Images for Optimizing Focal Plane Wavefront Control

Author

Nemanja Jovanovic, Sean B. Goebel, Olivier Guyon, Julien Lozi, F. Martinache, Donald N. B. Hall, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Wavefront, business.industry, Near-infrared spectroscopy, Astronomy and Astrophysics, 01 natural sciences, 010309 optics, Methods statistical, Speckle pattern, Cardinal point, Optics, Space and Planetary Science, 0103 physical sciences, Adaptive optics, business, Subaru Telescope, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract

NSF [AST 1106391]; NASA Roses APRA award [NNX 13AC14G]; JSPS [23340051, 26220704, 23103002]; Astrobiology Center (ABC) of the National Institutes of Natural Sciences, Japan; Subaru Telescope; ERC [CoG 683029]

Published
2018
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9. Review of high-contrast imaging systems for current and future ground- and space-based telescopes I: coronagraph design methods and optical performance metrics

Author

Neil Zimmerman, Jeffrey Jewell, Frans Snik, Ewan S. Douglas, A. J. Riggs, R. Galicher, Matthew A. Kenworthy, Mamadou N'Diaye, Nemanja Jovanovic, Johan Mazoyer, Mathilde Beaulieu, Jeff Kuhn, Kevin Fogarty, Marie Ygouf, Eric Cady, Laurent Pueyo, Christoph U. Keller, Garreth Ruane, Olivier Absil, Michael J. Wilby, J. Kent Wallace, Sebastiaan Y. Haffert, David S. Doelman, Brunella Carlomagno, Emiel H. Por, Kelsey Miller, Olivier Guyon, Dan Sirbu, Pierre Baudoz, Justin Knight, Alexis Carlotti, Elsa Huby, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lystrup, Makenzie, MacEwen, Howard A., Fazio, Giovanni G., Batalha, Natalie, Siegler, Nicholas, Tong, Edward C., PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Computer science, Optical instrument, media_common.quotation_subject, FOS: Physical sciences, Context (language use), 01 natural sciences, law.invention, 010309 optics, law, 0103 physical sciences, Instrumentation (computer programming), Function (engineering), Design methods, 010303 astronomy & astrophysics, Coronagraph, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, media_common, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Exoplanet, Starlight, Systems engineering, Noise (video), Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Optimal Optical Coronagraph (OOC) Workshop at the Lorentz Center in September 2017 in Leiden, the Netherlands gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this first installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of design methods and optical performance metrics developed for coronagraph instruments. The design and optimization of coronagraphs for future telescopes has progressed rapidly over the past several years in the context of space mission studies for Exo-C, WFIRST, HabEx, and LUVOIR as well as ground-based telescopes. Design tools have been developed at several institutions to optimize a variety of coronagraph mask types. We aim to give a broad overview of the approaches used, examples of their utility, and provide the optimization tools to the community. Though it is clear that the basic function of coronagraphs is to suppress starlight while maintaining light from off-axis sources, our community lacks a general set of standard performance metrics that apply to both detecting and characterizing exoplanets. The attendees of the OOC workshop agreed that it would benefit our community to clearly define quantities for comparing the performance of coronagraph designs and systems. Therefore, we also present a set of metrics that may be applied to theoretical designs, testbeds, and deployed instruments. We show how these quantities may be used to easily relate the basic properties of the optical instrument to the detection significance of the given point source in the presence of realistic noise., To appear in Proceedings of the SPIE, vol. 10698

Published
2018
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10. Review of high-contrast imaging systems for current and future ground-based and space-based telescopes: Part II. Common path wavefront sensing/control and coherent differential imaging

Author

Kevin Fogarty, Eric Cady, Elsa Huby, Pierre Baudoz, Matthew A. Kenworthy, Laurent Pueyo, Michael Bottom, Mamadou N'Diaye, Brunella Carlomagno, Christoph U. Keller, Olivier Absil, Mathilde Beaulieu, Justin Knight, Michael J. Wilby, J. Kent Wallace, Garreth Ruane, Alexis Carlotti, A. J. Eldorado Riggs, Raphaël Galicher, Olivier Guyon, Nemanja Jovanovic, Kelsey Miller, Frans Snik, Emiel H. Por, Sebastiaan Y. Haffert, Marie Ygouf, Dan Sirbu, Johan Mazoyer, David S. Doelman, Jonas Kühn, Jeffrey Jewell, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Close, Laird M., Schreiber, Laura, and Schmidt, Dirk

Subjects
Wavefront, Computer science, 01 natural sciences, Exoplanet, Bridge (nautical), Field (computer science), law.invention, 010309 optics, law, 0103 physical sciences, Reflection (physics), Electronic engineering, Terrestrial planet, Instrumentation (computer programming), Differential (infinitesimal), Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Coronagraph, ComputingMilieux_MISCELLANEOUS
Abstract

The Optimal Optical Coronagraph (OOC) Workshop held at the Lorentz Center in September 2017 in Leiden, the Netherlands, gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this second installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of common path wavefront sensing/control and Coherent Differential Imaging techniques, highlight the latest results, and expose their relative strengths and weaknesses. We layout critical milestones for the field with the aim of enhancing future ground/space based high contrast imaging platforms. Techniques like these will help to bridge the daunting contrast gap required to image a terrestrial planet in the zone where it can retain liquid water, in reflected light around a G type star from space.

Published
2018
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11. A Demonstration of a Versatile Low-order Wavefront Sensor Tested on Multiple Coronographs

Author

Garima Singh, Olivier Guyon, Pierre Baudoz, Nemanja Jovanovic, Frantz Martinache, Tomoyuki Kudo, Julien Lozi, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Subaru Telescope, National Astronomical Observatory of Japan (NAOJ), Département Sciences de la Fabrication et Logistique (SFL-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), and Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-CMP-GC

Subjects
Physics, Wavefront, [PHYS]Physics [physics], Lyot stop, business.industry, Zernike polynomials, Astronomy and Astrophysics, Wavefront sensor, 01 natural sciences, Deformable mirror, law.invention, Starlight, 010309 optics, symbols.namesake, Optics, Space and Planetary Science, law, 0103 physical sciences, symbols, business, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Coronagraph, ComputingMilieux_MISCELLANEOUS
Abstract

Detecting faint companions in close proximity to stars is one of the major goals of current/planned ground- and space-based high-contrast imaging instruments. High-performance coronagraphs can suppress the diffraction features and gain access to companions at small angular separation. However, the uncontrolled pointing errors degrade the coronagraphic performance by leaking starlight around the coronagraphic focal-plane mask, preventing the detection of companions at small separations. A Lyot-stop low-order wavefront sensor (LLOWFS) was therefore introduced to calibrate and measure these aberrations for focal-plane phase mask coronagraphs. This sensor quantifies the variations in wavefront error decomposed into a few Zernike modes by reimaging the diffracted starlight rejected by a reflective Lyot stop. The technique was tested with several coronagraphs on the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system at the Subaru Telescope. The wavefront was decomposed into 15 and 35 Zernike modes with an occulting and focal-plane phase mask coronagraph, respectively, which were used to drive a closed-loop correction in the laboratory. Using a 2000-actuator deformable mirror, a closed-loop pointing stability between 10−3–10^(−4) λ/D was achieved in the laboratory in H-band, with sub nanometer residuals for the other Zernike modes (Noll index >4). On-sky, the low-order control of 10+ Zernike modes for the phase-induced amplitude apodization and the vector vortex coronagraphs was demonstrated, with a closed-loop pointing stability of 10^(-4) λ /D under good seeing and 10^(-3) λ/D under moderate seeing conditions readily achievable.

Published
2017
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12. Efficient injection from large telescopes into single-mode fibres: Enabling the era of ultra-precision astronomy

Author

Naruhisa Takato, Barnaby Norris, Nemanja Jovanovic, Nick Cvetojevic, Thayne Currie, Christian Schwab, F. Martinache, Julien Lozi, Sergio G. Leon-Saval, Simon Gross, Olivier Guyon, D. Doughty, Subaru Telescope, National Astronomical Observatory of Japan (NAOJ), CUDOS and MQ Photonics, Macquarie University, Anglo-Australian Observatory (AAO), Sydney Institute for Astronomy (SIfA), The University of Sydney, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, Centre for Ultra-high bandwidth Devices for Optical Systems (CUDOS), and Australian National University (ANU)

Subjects
Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Bandwidth (signal processing), Single-mode optical fiber, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, 010309 optics, Space and Planetary Science, Research council, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Subaru Telescope, Ultra precision, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics - Optics, Optics (physics.optics)
Abstract

Photonic technologies offer numerous advantages for astronomical instruments such as spectrographs and interferometers owing to their small footprints and diverse range of functionalities. Operating at the diffraction-limit, it is notoriously difficult to efficiently couple such devices directly with large telescopes. We demonstrate that with careful control of both the non-ideal pupil geometry of a telescope and residual wavefront errors, efficient coupling with single-mode devices can indeed be realised. A fibre injection was built within the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument. Light was coupled into a single-mode fibre operating in the near-IR (J-H bands) which was downstream of the extreme adaptive optics system and the pupil apodising optics. A coupling efficiency of 86% of the theoretical maximum limit was achieved at 1550 nm for a diffraction-limited beam in the laboratory, and was linearly correlated with Strehl ratio. The coupling efficiency was constant to within 40% for 84% of the time and >50% for 41% of the time. The laboratory results allow us to forecast that extreme adaptive optics levels of correction (Strehl ratio >90% in H-band) would allow coupling of >67% (of the order of coupling to multimode fibres currently). For Strehl ratios, 15 pages, 16 figures, 1 table, published in A&A

Published
2017
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13. The SOPHIE search for northern extrasolar planets X. Detection and characterization of giant planets by the dozen

Author

Nicola Astudillo-Defru, Paul Wilson, O. Labrevoir, Alexandre Santerne, Luc Arnold, X. Delfosse, Nemanja Jovanovic, Simon Borgniet, Rodrigo F. Díaz, Guillaume Hébrard, X. Bonfils, Johannes Sahlmann, J. Gregorio, Guillaume Montagnier, J. Rey, Julien Lozi, A-M. Lagrange, Vincent Bourrier, Nuno C. Santos, Damien Ségransan, David Ehrenreich, T. Forveille, Arthur Vigan, Olivier Demangeon, C. Lovis, M. Vanhuysse, B. Courcol, Jacques Laskar, Magali Deleuil, Stéphane Udry, C. Moutou, Janis Hagelberg, Alexandre C. M. Correia, François Bouchy, Isabelle Boisse, Francesco Pepe, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), European Southern Observatory (ESO), Département RadioChimie et Procédés (DRCP), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universidade do Porto, Universidade do Porto-Universidade do Porto, Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidade do Porto [Porto], Departamento de Física e Astronomia [Porto], PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Canada-France-Hawaii Telescope Corporation, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], photometric [Techniques], Astronomy and Astrophysics, Planetary system, Exoplanet, Radial velocity, Stars, Planetary systems, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new radial velocity measurements of eight stars secured with the spectrograph SOPHIE at the 193-cm telescope of the Haute-Provence Observatory allowing the detection and characterization of new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes between 6.7 and 9.6; the planets have minimum masses M_p sin i between 0.4 to 3.8 M_Jup and orbital periods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD143105, HIP109600, HD35759, HIP109384, HD220842, and HD12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP65407, allows the discovery of two giant planets, just outside the 12:5 resonance in weak mutual interaction. The last star, HD141399, was already known to host a four-planetary system; our additional data and analyses allow new constraints to be put on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planetary systems. HD143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted despite this is not a transiting system. The giant planets HIP109600b, HIP109384b, and HD141399c are located in the habitable zone of their host star., Comment: 20 pages, 19 figures, 5 tables, accepted for publication in A&A

Published
2016
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14. On-Sky Demonstration of Low-Order Wavefront Sensing and Control with Focal Plane Phase Mask Coronagraphs

Author

Pierre Baudoz, Jonas Kühn, Olivier Guyon, Frantz Martinache, Tomoyuki Kudo, Julien Lozi, Eugene Serabyn, Nemanja Jovanovic, Garima Singh, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Palaiseau], ONERA-Université Paris Saclay (COmUE), Département Sciences de la Fabrication et Logistique (SFL-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-CMP-GC, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Stuttgart University, Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), NASA-California Institute of Technology (CALTECH), and Universität Stuttgart [Stuttgart]

Subjects
Zernike polynomials, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, symbols.namesake, Optics, law, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, Coronagraph, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Physics, Wavefront, [PHYS]Physics [physics], business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Wavefront sensor, Starlight, Cardinal point, Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Subaru Telescope, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The ability to characterize exoplanets by spectroscopy of their atmospheres requires direct imaging techniques to isolate planet signal from the bright stellar glare. One of the limitations with the direct detection of exoplanets, either with ground- or space-based coronagraphs, is pointing errors and other low-order wavefront aberrations. The coronagraphic detection sensitivity at the diffraction limit therefore depends on how well low-order aberrations upstream of the focal plane mask are corrected. To prevent starlight leakage at the inner working angle of a phase mask coronagraph, we have introduced a Lyot-based low-order wavefront sensor (LLOWFS), which senses aberrations using the rejected starlight diffracted at the Lyot plane. In this paper, we present the implementation, testing and results of LLOWFS on the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) at the Subaru Telescope. We have controlled thirty-five Zernike modes of a H-band vector vortex coronagraph in the laboratory and ten Zernike modes on sky with an integrator control law. We demonstrated a closed-loop pointing residual of 0.02 mas in the laboratory and 0.15 mas on sky for data sampled using the minimal 2-second exposure time of the science camera. We have also integrated the LLOWFS in the visible high-order control loop of SCExAO, which in closed-loop operation has validated the correction of the non-common path pointing errors between the infrared science channel and the visible wavefront sensing channel with pointing residual of 0.23 mas on sky., Comment: 12 pages, 15 figures, Accepted and scheduled for publication in September 2015 issue of the PASP

Published
2015
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15. Development and recent results from the Subaru coronagraphic extreme adaptive optics system

Author

Franck Marchis, Takayuki Kotani, Tomoyuki Kudo, Jonas Kuhn, Peter G. Tuthill, Guy Perrin, Gaspard Duchene, Elsa Huby, Olivier Lai, Naoshi Murakami, Christophe Clergeon, Garima Singh, F. Martinache, John H. White, Yutaka Hayano, O. Fumika, Sylvestre Lacour, Paul Stewart, Olivier Guyon, Barnaby Norris, Nemanja Jovanovic, Eugene Serabyn, Y. Minowa, Sébastien Vievard, K. Newman, Julien Woillez, Subaru Telescope, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Central Arizona College, Coolidge, Jet Propulsion Laboratory, California Institute of Technology (JPL), The Univ. of Sydney (Australia), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Hokkaido University, Gemini Observatory, SETI Institute (United States), Univ. of California, Berkeley (United States), and European Southern Observatory (Germany)

Subjects
Physics, Wavefront, Speckle pattern, Interferometry, Optics, Apodization, business.industry, Aperture masking interferometry, Wavefront sensor, business, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Deformable mirror
Abstract

International audience; The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is one of a handful of extreme adaptive optics systems set to come online in 2014. The extreme adaptive optics correction is realized by a combination of precise wavefront sensing via a non-modulated pyramid wavefront sensor and a 2000 element deformable mirror. This system has recently begun on-sky commissioning and was operated in closed loop for several minutes at a time with a loop speed of 800 Hz, on ~150 modes. Further suppression of quasi-static speckles is possible via a process called "speckle nulling" which can create a dark hole in a portion of the frame allowing for an enhancement in contrast, and has been successfully tested on-sky. In addition to the wavefront correction there are a suite of coronagraphs on board to null out the host star which include the phase induced amplitude apodization (PIAA), the vector vortex, 8 octant phase mask, 4 quadrant phase mask and shaped pupil versions which operate in the NIR (y-K bands). The PIAA and vector vortex will allow for high contrast imaging down to an angular separation of 1 lambda/D to be reached; a factor of 3 closer in than other extreme AO systems. Making use of the left over visible light not used by the wavefront sensor is VAMPIRES and FIRST. These modules are based on aperture masking interferometry and allow for sub-diffraction limited imaging with moderate contrasts of ~100-1000:1. Both modules have undergone initial testing on-sky and are set to be fully commissioned by the end of 2014.

Published
2014
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