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Mikkel Nørup Lund

Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry

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  • L. Mancini, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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  • S. Ciceri, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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  • G. Chen, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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  • J. Tregloan-Reed, Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK
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  • J. J. Fortney, Department of Astronomy & Astrophysics, University of California, Santa Cruz, CA 95064, USA
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  • J. Southworth, Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK
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  • T. G. Tan, Perth Exoplanet Survey Telescope, Perth, Australia
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  • M. Burgdorf, HE Space Operations GmbH, Flughafenallee 24, D-28199 Bremen, Germany
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  • S. Calchi Novati, Department of Physics, University of Salerno, I-84084-Fisciano (SA), Italy
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  • M. Dominik, SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews KY16 9SS, UK
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  • X.-S. Fang, National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China
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  • F. Finet, Institut d'Astrophysique et de Géophysique, Université de Liège, B-4000 Liège, Belgium
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  • T. Gerner, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstraße 12-14, D-69120 Heidelberg, Germany
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  • S. Hardis, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, DK-2100 Copenhagen Ø, Denmark
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  • T. C. Hinse, Korea Astronomy and Space Science Institute, Daejeon 305-348, Republic of Korea
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  • U. G. Jørgensen, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, DK-2100 Copenhagen Ø, Denmark
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  • C. Liebig, SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews KY16 9SS, UK
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  • N. Nikolov, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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  • D. Ricci, Institut d'Astrophysique et de Géophysique, Université de Liège, B-4000 Liège, Belgium
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  • S. Schäfer, Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany
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  • F. Schönebeck, Zentrum für Astronomie, Universität Heidelberg, Mönchhofstraße 12-14, D-69120 Heidelberg, Germany
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  • Jesper Mirsa Skottfelt, Astrofysik og Planetforskning, Danmark
  • O. Wertz, Institut d'Astrophysique et de Géophysique, Université de Liège, B-4000 Liège, Belgium
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  • K. A. Alsubai, Qatar Foundation, PO Box 5825, Doha, Qatar
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  • V. Bozza, Department of Physics, University of Salerno, I-84084-Fisciano (SA), Italy
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  • P. Browne, National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China
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  • P. Dodds, SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews KY16 9SS, UK
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  • S.-H. Gu, National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China
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  • Kennet Bomann West Harpsøe, Niels Bohr Institutet - Afd., Danmark
  • Th. Henning, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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  • M. Hundertmark, SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews KY16 9SS, UK
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  • J. Jessen-Hansen
  • N. Kains, European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany
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  • E. Kerins, Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL, UK
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  • H. Kjeldsen
  • M. N. Lund
  • M. Lundkvist
  • N. Madhusudhan, Department of Physics and Department of Astronomy, Yale University, New Haven, CT 06511, USA
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  • M. Mathiasen, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, DK-2100 Copenhagen Ø, Denmark
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  • M. T. Penny, Department of Astronomy, Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA
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  • S. Prof, Department of Physics, Sharif University of Technology, P. O. Box 11155-9161 Tehran, Iran
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  • S. Rahvar, Department of Physics, Sharif University of Technology, P. O. Box 11155-9161 Tehran, Iran
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  • K. Sahu, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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  • G. Scarpetta, Department of Physics, University of Salerno, I-84084-Fisciano (SA), Italy
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  • C. Snodgrass, Max-Planck-Institute for Solar System Research, Max-Planck Str. 2, D-37191 Katlenburg-Lindau, Germany
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  • J. Surdej, Institut d'Astrophysique et de Géophysique, Université de Liège, B-4000 Liège, Belgium
We present new ground-based, multi-colour, broad-band photometric measurements of the physical parameters, transmission and emission spectra of the transiting extrasolar planet WASP-19b. The measurements are based on observations of eight transits and four occultations through a Gunn i filter using the 1.54-m Danish Telescope, 14 transits through an Rc filter at the Perth Exoplanet Survey Telescope (PEST) observatory and one transit observed simultaneously through four optical (Sloan g', r', i', z') and three near-infrared (J, H, K) filters, using the Gamma Ray Burst Optical and Near-Infrared Detector (GROND) instrument on the MPG/ESO 2.2-m telescope. The GROND optical light curves have a point-to-point scatter around the best-fitting model between 0.52 and 0.65 mmag rms. We use these new data to measure refined physical parameters for the system. We find the planet to be more bloated (Rb = 1.410 ± 0.017RJup; Mb = 1.139 ± 0.030MJup) and the system to be twice as old as initially thought. We also used published and archived data sets to study the transit timings, which do not depart from a linear ephemeris. We detected an anomaly in the GROND transit light curve which is compatible with a spot on the photosphere of the parent star. The starspot position, size, spot contrast and temperature were established. Using our new and published measurements, we assembled the planet's transmission spectrum over the 370-2350 nm wavelength range and its emission spectrum over the 750-8000 nm range. By comparing these data to theoretical models we investigated the theoretically predicted variation of the apparent radius of WASP-19b as a function of wavelength and studied the composition and thermal structure of its atmosphere. We conclude that: (i) there is no evidence for strong optical absorbers at low pressure, supporting the common idea that the planet's atmosphere lacks a dayside inversion; (ii) the temperature of the planet is not homogenized, because the high warming of its dayside causes the planet to be more efficient in re-radiating than redistributing energy to the night side; (iii) the planet seems to be outside of any current classification scheme.
OriginalsprogEngelsk
TidsskriftRoyal Astronomical Society. Monthly Notices
Vol/bind436
Nummer1
Sider (fra-til)2-18
Antal sider16
ISSN0035-8711
DOI
StatusUdgivet - 1 nov. 2013

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