First Light of the VLT Planet Finder SPHERE
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GEMINI PLANET IMAGER SPECTROSCOPY of the HR 8799 PLANETS C and D
The Astrophysical Journal Letters, 794:L15 (5pp), 2014 October 10 doi:10.1088/2041-8205/794/1/L15 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. GEMINI PLANET IMAGER SPECTROSCOPY OF THE HR 8799 PLANETS c AND d Patrick Ingraham1, Mark S. Marley2, Didier Saumon3, Christian Marois4, Bruce Macintosh1, Travis Barman5, Brian Bauman6, Adam Burrows7, Jeffrey K. Chilcote8, Robert J. De Rosa9,10, Daren Dillon11,Rene´ Doyon12, Jennifer Dunn4, Darren Erikson4, Michael P. Fitzgerald8, Donald Gavel11, Stephen J. Goodsell13, James R. Graham14, Markus Hartung13, Pascale Hibon13, Paul G. Kalas14, Quinn Konopacky15, James A. Larkin8, Jer´ omeˆ Maire15, Franck Marchis16, James McBride14, Max Millar-Blanchaer15, Katie M. Morzinski17,24, Andrew Norton11, Rebecca Oppenheimer18, Dave W. Palmer6, Jenny Patience9, Marshall D. Perrin19, Lisa A. Poyneer6, Laurent Pueyo19, Fredrik Rantakyro¨ 13, Naru Sadakuni13, Leslie Saddlemyer4, Dmitry Savransky20,Remi´ Soummer19, Anand Sivaramakrishnan19, Inseok Song21, Sandrine Thomas2,22, J. Kent Wallace23, Sloane J. Wiktorowicz11, and Schuyler G. Wolff19 1 Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 2 NASA Ames Research Center, Moffett Field, CA 94035, USA 3 Los Alamos National Laboratory, Los Alamos, NM 87545, USA 4 NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 5 Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721-0092, USA 6 Lawrence Livermore National Lab, -
The Formation Mechanism of Gas Giants on Wide Orbits
The Astrophysical Journal, 707:79–88, 2009 December 10 doi:10.1088/0004-637X/707/1/79 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS Sarah E. Dodson-Robinson1,4, Dimitri Veras2, Eric B. Ford2, and C. A. Beichman3 1 Astronomy Department, University of Texas, 1 University Station C1400, Austin, TX 78712, USA; [email protected] 2 Astronomy Department, University of Florida, 211 Bryant Space Sciences Center, Gainesville, FL 32111, USA 3 NASA Exoplanet Science Institute, California Institute of Technology, 770 S. Wilson Ave, Pasadena, CA 91125, USA Received 2009 July 29; accepted 2009 October 19; published 2009 November 18 ABSTRACT The recent discoveries of massive planets on ultra-wide orbits of HR 8799 and Fomalhaut present a new challenge for planet formation theorists. Our goal is to figure out which of three giant planet formation mechanisms— core accretion (with or without migration), scattering from the inner disk, or gravitational instability—could be responsible for Fomalhaut b, HR 8799 b, c and d, and similar planets discovered in the future. This paper presents the results of numerical experiments comparing the long-period planet formation efficiency of each possible mechanism in model A star, G star, and M star disks. First, a simple core accretion simulation shows that planet cores forming beyond 35 AU cannot reach critical mass, even under the most favorable conditions one can construct. Second, a set of N-body simulations demonstrates that planet–planet scattering does not create stable, wide-orbit systems such as HR 8799. -
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A&A 637, A9 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937239 & c O. Flasseur et al. 2020 Astrophysics PACO ASDI: an algorithm for exoplanet detection and characterization in direct imaging with integral field spectrographs Olivier Flasseur1, Loïc Denis1, Éric Thiébaut2, and Maud Langlois2 1 Université de Lyon, UJM-Saint-Etienne, CNRS, Institut d’Optique Graduate School, Laboratoire Hubert Curien UMR 5516, 42023 Saint-Etienne, France e-mail: [email protected] 2 Université de Lyon, Université Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR 5574, 69230 Saint-Genis-Laval, France e-mail: [email protected] Received 3 December 2019 / Accepted 6 March 2020 ABSTRACT Context. Exoplanet detection and characterization by direct imaging both rely on sophisticated instruments (adaptive optics and coro- nagraph) and adequate data processing methods. Angular and spectral differential imaging (ASDI) combines observations at different times and a range of wavelengths in order to separate the residual signal from the host star and the signal of interest corresponding to off-axis sources. Aims. Very high contrast detection is only possible with an accurate modeling of those two components, in particular of the back- ground due to stellar leakages of the host star masked out by the coronagraph. Beyond the detection of point-like sources in the field of view, it is also essential to characterize the detection in terms of statistical significance and astrometry and to estimate the source spectrum. Methods. We extend our recent method PACO, based on local learning of patch covariances, in order to capture the spectral and tem- poral fluctuations of background structures. -
Radial Velocity of Directly Imaged Planets Jean-Baptiste Ruffio, OSIRIS: Quinn M
Radial Velocity of directly imaged planets Jean-Baptiste Ruffio, OSIRIS: Quinn M. Konopacky, Travis Barman, Bruce Macintosh, Kielan K. Wilcomb, Robert J. De Rosa, Jason J. Wang, Ian Czekala, Christian Marois, KPIC: KPIC collaboration, Jason Wang, Evan Morris, Jacques Delorme, Dimitri Mawet, Andrew Skemer, Travis Barman. [email protected] Planetary radial velocity (RV) is one of the science drivers for high Youtube introduction link resolution spectroscopy of exoplanets. It can be used to better constrain the orbital architecture of stellar systems (e.g. eccentricity or obliquity), which can be related to the formation history of exoplanets. Ultimately, planetary RV will even allow the detection of exo-moons. Such measurements are however challenging due to the overwhelming starlight at the small separations corresponding to directly imaged planets. We present RV measurements of the four large gas giant planets orbiting the star HR 8799 (Fig. 1) using OSIRIS and the new KPIC instruments at Keck. Fig. 1: HR 8799 four-planet system from Marois et al. (2010) [1]. The orbital motion of the planets can be visualized here. Moderate resolution spectroscopy (R≈4,000) with OSIRIS/Keck The OSIRIS instrument at Keck has been used to detect molecules (CO and H2O) and characterize the atmosphere of HR 8799 b and c for more than a decade [2,3]. Despite the moderate resolution of the instrument (R≈4,000, K band), we showed that we could measure the RV of HR 8799 b and c with a combined precision of 0.5 km/s using a forward modeling approach. These measurements resolve the degeneracy in the 3D orientation of the system [4]. -
The LEECH Exoplanet Imaging Survey. Further Constraints on the Planet Architecture of the HR 8799 System?
A&A 576, A133 (2015) Astronomy DOI: 10.1051/0004-6361/201425185 & c ESO 2015 Astrophysics The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system? A.-L. Maire1, A. J. Skemer2;??, P. M. Hinz2, S. Desidera1, S. Esposito3, R. Gratton1, F. Marzari4, M. F. Skrutskie5, B. A. Biller6;7, D. Defrère2, V. P. Bailey2, J. M. Leisenring2, D. Apai2, M. Bonnefoy8;9;7, W. Brandner7, E. Buenzli7, R. U. Claudi1, L. M. Close2, J. R. Crepp10, R. J. De Rosa11;12, J. A. Eisner2, J. J. Fortney13, T. Henning7, K.-H. Hofmann14, T. G. Kopytova7;15, J. R. Males2;???, D. Mesa1, K. M. Morzinski2;???, A. Oza5, J. Patience11, E. Pinna3, A. Rajan11, D. Schertl14, J. E. Schlieder7;16;????, K. Y. L. Su2, A. Vaz2, K. Ward-Duong11, G. Weigelt14, and C. E. Woodward17 1 INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy e-mail: [email protected] 2 Steward Observatory, Department of Astronomy, University of Arizona, 993 North Cherry Avenue, Tucson, AZ 85721, USA 3 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy 4 Dipartimento di Fisica e Astronomia, Universitá di Padova, via F. Marzolo 8, 35131 Padova, Italy 5 Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA 6 Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 7 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 8 Université Grenoble Alpes, IPAG, 38000 Grenoble, France 9 CNRS, IPAG, 38000 Grenoble, France -
DIRECT DETECTION and ORBITAL ANALYSIS of the EXOPLANETS HR 8799 Bcd from ARCHIVAL 2005 KECK/NIRC2 DATA
The Astrophysical Journal Letters, 755:L34 (7pp), 2012 August 20 doi:10.1088/2041-8205/755/2/L34 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DIRECT DETECTION AND ORBITAL ANALYSIS OF THE EXOPLANETS HR 8799 bcd FROM ARCHIVAL 2005 KECK/NIRC2 DATA Thayne Currie1, Misato Fukagawa2, Christian Thalmann3, Soko Matsumura4, and Peter Plavchan5 1 NASA-Goddard Space Flight Center, Greenbelt, MD, USA 2 Department of Earth and Space Science, Graduate School of Science, Osaka University, Osaka, Japan 3 Astronomical Institute Anton Pannekoek, University of Amsterdam, 1090-GE, The Netherlands 4 Department of Astronomy, University of Maryland-College Park, MD 20742, USA 5 NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA, USA Received 2012 May 30; accepted 2012 July 5; published 2012 August 7 ABSTRACT We present previously unpublished 2005 July H-band coronagraphic data of the young, planet-hosting star HR 8799 from the newly released Keck/NIRC2 archive. Despite poor observing conditions, we detect three of the planets (HR 8799 bcd), two of them (HR 8799 bc) without advanced image processing. Comparing these data with previously published 1998–2011 astrometry and that from re-reduced 2010 October Keck data constrains the orbits of the planets. Analyzing the planets’ astrometry separately, HR 8799 d’s orbit is likely inclined at least 25◦ from face-on and the others may be on inclined orbits. For semimajor axis ratios consistent with a 4:2:1 mean-motion resonance, our analysis yields precise values for HR 8799 bcd’s orbital parameters and strictly constrains the planets’ eccentricities to be less than 0.18–0.3. -
Enrichment of the HR 8799 Planets by Minor Bodies and Dust Frantseva, K.; Mueller, M.; Pokorný, P.; Van Der Tak, F
University of Groningen Enrichment of the HR 8799 planets by minor bodies and dust Frantseva, K.; Mueller, M.; Pokorný, P.; van der Tak, F. F. S.; ten Kate, I. L. Published in: Astronomy and astrophysics DOI: 10.1051/0004-6361/201936783 IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2020 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Frantseva, K., Mueller, M., Pokorný, P., van der Tak, F. F. S., & ten Kate, I. L. (2020). Enrichment of the HR 8799 planets by minor bodies and dust. Astronomy and astrophysics, 638, [A50]. https://doi.org/10.1051/0004-6361/201936783 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. -
Direct Imaging of Exoplanets
Direct Imaging of Exoplanets Techniques & Results Challenge 1: Large ratio between star and planet flux (Star/Planet) Reflected light from Jupiter ≈ 10–9 Stars are a billion times brighter… …than the planet …hidden in the glare. Challenge 2: Close proximity of planet to host star Direct Detections need contrast ratios of 10–9 to 10–10 At separations of 0.01 to 1 arcseconds Earth : ~10–10 separation = 0.1 arcseconds for a star at 10 parsecs Jupiter: ~10–9 separation = 0.5 arcseconds for a star at 10 parsecs 1 AU = 1 arcsec separation at 1 parsec Younger planets are hotter and they emit more radiated light. These are easier to detect. Adaptive Optics : An important component for any imaging instrument Atmospheric turbulence distorts stellar images making them much larger than point sources. This seeing image makes it impossible to detect nearby faint companions. Adaptive Optics (AO) The scientific and engineering discipline whereby the performance of an optical signal is improved by using information about the environment through which it passes AO Deals with the control of light in a real time closed loop and is a subset of active optics. Adaptive Optics: Systems operating below 1/10 Hz Active Optics: Systems operating above 1/10 Hz Example of an Adaptive Optics System: The Eye-Brain The brain interprets an image, determines its correction, and applies the correction either voluntarily of involuntarily Lens compression: Focus corrected mode Tracking an Object: Tilt mode optics system Iris opening and closing to intensity levels: Intensity control mode Eyes squinting: An aperture stop, spatial filter, and phase controlling mechanism The Ideal Telescope image of a star produced by ideal telescope where: • P(α) is the light intensity in the focal plane, as a function of angular coordinates α ; • λ is the wavelength of light; • D is the diameter of the telescope aperture; • J1 is the so-called Bessel function. -
GEMINI PLANET IMAGER SPECTROSCOPY of the HR 8799 PLANETS C and D
The Astrophysical Journal Letters, 794:L15 (5pp), 2014 October 10 doi:10.1088/2041-8205/794/1/L15 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. GEMINI PLANET IMAGER SPECTROSCOPY OF THE HR 8799 PLANETS c AND d Patrick Ingraham1, Mark S. Marley2, Didier Saumon3, Christian Marois4, Bruce Macintosh1, Travis Barman5, Brian Bauman6, Adam Burrows7, Jeffrey K. Chilcote8, Robert J. De Rosa9,10, Daren Dillon11,Rene´ Doyon12, Jennifer Dunn4, Darren Erikson4, Michael P. Fitzgerald8, Donald Gavel11, Stephen J. Goodsell13, James R. Graham14, Markus Hartung13, Pascale Hibon13, Paul G. Kalas14, Quinn Konopacky15, James A. Larkin8, Jer´ omeˆ Maire15, Franck Marchis16, James McBride14, Max Millar-Blanchaer15, Katie M. Morzinski17,24, Andrew Norton11, Rebecca Oppenheimer18, Dave W. Palmer6, Jenny Patience9, Marshall D. Perrin19, Lisa A. Poyneer6, Laurent Pueyo19, Fredrik Rantakyro¨ 13, Naru Sadakuni13, Leslie Saddlemyer4, Dmitry Savransky20,Remi´ Soummer19, Anand Sivaramakrishnan19, Inseok Song21, Sandrine Thomas2,22, J. Kent Wallace23, Sloane J. Wiktorowicz11, and Schuyler G. Wolff19 1 Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 2 NASA Ames Research Center, Moffett Field, CA 94035, USA 3 Los Alamos National Laboratory, Los Alamos, NM 87545, USA 4 NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 5 Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721-0092, USA 6 Lawrence Livermore National Lab, -
VLT/NACO Astrometry of the HR 8799 Planetary System⋆
A&A 528, A134 (2011) Astronomy DOI: 10.1051/0004-6361/201116493 & c ESO 2011 Astrophysics VLT/NACO astrometry of the HR 8799 planetary system L-band observations of the three outer planets C. Bergfors1,, W. Brandner1, M. Janson2,R.Köhler1,3, and T. Henning1 1 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 University of Toronto, Dept. of Astronomy, 50 St George Street, Toronto, ON, M5S 3H8, Canada 3 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl, 69117 Heidelberg, Germany Recieved 10 January 2011 / Accepted 16 February 2011 ABSTRACT Context. HR 8799 is so far the only directly imaged multiple exoplanet system. The orbital configuration would, if better known, provide valuable insight into the formation and dynamical evolution of wide-orbit planetary systems. Aims. We present data which add to the astrometric monitoring of the planets HR 8799 b, c and d. We investigate how well the two simple cases of (i) a circular orbit and (ii) a face-on orbit fit the astrometric data for HR 8799 d over a total time baseline of ∼2 years. Methods. The HR 8799 planetary system was observed in L-band with NACO at VLT. Results. The results indicate that the orbit of HR 8799 d is inclined with respect to our line of sight, and suggest that the orbit is slightly eccentric or non-coplanar with the outer planets and debris disk. Key words. planetary systems – stars: individual: HR 8799 1. Introduction masses 7–10 MJ at projected separations 14.5, 24, 38 and 68 AU from the central star. -
A Possible Architecture of the Planetary System HR 8799
A&A 503, 247–258 (2009) Astronomy DOI: 10.1051/0004-6361/200912055 & c ESO 2009 Astrophysics A possible architecture of the planetary system HR 8799 M. Reidemeister, A. V. Krivov, T. O. B. Schmidt, S. Fiedler, S. Müller, T. Löhne, and R. Neuhäuser Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany e-mail: [email protected] Received 12 March 2009 / Accepted 20 May 2009 ABSTRACT HR 8799 is a nearby A-type star with a debris disk and three planetary candidates, which have been imaged directly. We undertake a coherent analysis of various observational data for all known components of the system, including the central star, imaged companions, and dust. Our goal is to elucidate the architecture and evolutionary status of the system. We try to further constrain the age and orientation of the system, the orbits and masses of the companions, and the location of dust. On the basis of the high luminosity of debris dust and dynamical constraints, we argue for a rather young system’s age of ∼<50 Myr. The system must be seen nearly, but not exactly, pole-on. Our analysis of the stellar rotational velocity yields an inclination of 13–30◦, whereas i ∼> 20◦ is needed for the system to be dynamically stable, which suggests a probable inclination range of 20–30◦. The spectral energy distribution, including the Spitzer/IRS spectrum in the mid-infrared as well as IRAS, ISO, JCMT, and IRAM observations, is naturally reproduced by two dust rings associated with two planetesimal belts. -
Modelling the Inner Debris Disc of HR 8799
Modelling the Inner Debris Disc of HR 8799 Bruna Contro1,2, Jonti Horner3,4, Rob Wittenmyer2,3,4, Jonathan P. Marshall2,4, T. C. Hinse5,6,3 1University of Sao Paulo State, Sao Paulo, Botucatu 18618-970, Brazil 2School of Physics, UNSW Australia, Sydney, New South Wales 2052, Australia 3Computational Engineering and Science Research Centre, University of Southern Queensland, Toowoomba, Queensland 4350, Australia 4Australian Centre for Astrobiology, UNSW Australia, Sydney, New South Wales 2052, Australia 5Korea Astronomy and Space Science Institute, 776 Daedukdae-ro, Yuseong-gu, Daejeon 305-348, Republic of Korea. 6Armagh Observatory, College Hill, Armagh BT61 9DG, UK Abstract: In many ways, the HR 8799 planetary system strongly resembles our own. It features four giant planets and two debris belts, analogues to the Asteroid and Edgeworth-Kuiper belts. Here, we present the results of dynamical simulations of HR8799’s inner debris belt, to study its structure and collisional environment. Our results suggest that HR 8799’s inner belt is highly structured, with gaps between regions of dynamical stability. The belt is likely constrained between sharp inner and outer edges, located at ~6 and ~8 au, respectively. Its inner edge coincides with a broad gap cleared by the 4:1 mean-motion resonance with HR 8799e. Within the belt, planetesimals are undergoing a process of collisional attrition like that observed in the Asteroid belt. However, whilst the mean collision velocity in the Asteroid belt exceeds 5 kms-1, the majority of collisions within HR 8799’s inner belt occur with velocities of order 1.2 kms-1, or less.