Reference : Physical properties and transmission spectrum of the WASP-80 planetary system from mu...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/162006
Physical properties and transmission spectrum of the WASP-80 planetary system from multi-colour photometry
English
Mancini, L. [Max Planck Institute for Astronomy, Königstuhl 17, 69117, Heidelberg, Germany]
Southworth, J. [Astrophysics Group, Keele University, Keele, ST5 5BG, UK]
Ciceri, S. [Max Planck Institute for Astronomy, Königstuhl 17, 69117, Heidelberg, Germany]
Dominik, M. [SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews, KY16 9SS, UK]
Henning, Th [Max Planck Institute for Astronomy, Königstuhl 17, 69117, Heidelberg, Germany]
Jørgensen, U. G. [Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100, Copenhagen Ø, Denmark; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350, Copenhagen, Denmark]
Lanza, A. F. [INAF-Osservatorio Astrofisico di Catania, via S.Sofia 78, 95123, Catania, Italy]
Rabus, M. [Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile; Max Planck Institute for Astronomy, Königstuhl 17, 69117, Heidelberg, Germany]
Snodgrass, C. [Max-Planck-Institute for Solar System Research, Max-Planck Str. 2, 37191, Katlenburg-Lindau, Germany]
Vilela, C. [Astrophysics Group, Keele University, Keele, ST5 5BG, UK]
Alsubai, K. A. [Qatar Foundation, PO Box 5825, Doha, Qatar]
Bozza, V. [Dipartimento di Fisica "E.R. Caianiello", University of Salerno, via Giovanni Paolo II, 84084, Fisciano, Italy; Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Napoli, Italy]
Bramich, D. M. [Qatar Environment and Energy Research Institute, Qatar Foundation, Tornado Tower, Floor 19, PO Box 5825, Doha, Qatar]
Calchi Novati, S. [Istituto Internazionale per gli Alti Studi Scientifici (IIASS), 84019, Vietri Sul Mare, Italy; Dipartimento di Fisica "E.R. Caianiello", University of Salerno, via Giovanni Paolo II, 84084, Fisciano, Italy]
D'Ago, G. [Dipartimento di Fisica "E.R. Caianiello", University of Salerno, via Giovanni Paolo II, 84084, Fisciano, Italy; Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Napoli, Italy]
Figuera Jaimes, R. [European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748, Garching bei München, Germany; SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews, KY16 9SS, UK]
Galianni, P. [SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews, KY16 9SS, UK]
Gu, S.-H. [Yunnan Observatory, Chinese Academy of Sciences, 650011, Kunming, PR China; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011, Kunming, PR China]
Harpsøe, K. [Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100, Copenhagen Ø, Denmark; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350, Copenhagen, Denmark]
Hinse, T. [Korea Astronomy and Space Science Institute, 305-348, Daejeon, Republic of Korea]
Hundertmark, M. [SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews, KY16 9SS, UK]
Juncher, D. [Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100, Copenhagen Ø, Denmark; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350, Copenhagen, Denmark]
Kains, N. [European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748, Garching bei München, Germany]
Korhonen, H. [Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, 21500, Piikkiö, Finland; Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100, Copenhagen Ø, Denmark; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350, Copenhagen, Denmark]
Popovas, A. [Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100, Copenhagen Ø, Denmark; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350, Copenhagen, Denmark]
Rahvar, S. [Department of Physics, Sharif University of Technology, PO Box 11155-9161, Tehran, Iran; Perimeter Institute for Theoretical Physics, 31 Caroline St. N., Waterloo, N2L 2Y5, Canada]
Skottfelt, J. [Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100, Copenhagen Ø, Denmark; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350, Copenhagen, Denmark]
Street, R. [Las Cumbres Observatory Global Telescope Network, 6740B Cortona Drive, Goleta, CA, 93117, USA]
Surdej, Jean mailto [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO) >]
Tsapras, Y. [Las Cumbres Observatory Global Telescope Network, 6740B Cortona Drive, Goleta, CA, 93117, USA; School of Physics and Astronomy, Queen Mary University of London, Mile End Road, London, E1 4NS, UK]
Wang, X.-B. [Yunnan Observatory, Chinese Academy of Sciences, 650011, Kunming, PR China; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011, Kunming, PR China]
Wertz, O. [Institut d'Astrophysique et de Géophysique, Université de Liège, 4000, Liège, Belgium)]
1-Feb-2014
Astronomy and Astrophysics
EDP Sciences
562
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] Astrophysics - Earth and Planetary Astrophysics ; planetary systems ; stars: fundamental parameters ; stars: individual: ; WASP-80 ; techniques: photometric
[en] WASP-80 is one of only two systems known to contain a hot Jupiter which transits its M-dwarf host star. We present eight light curves of one transit event, obtained simultaneously using two defocussed telescopes. These data were taken through the Bessell I, Sloan g'r'i'z' and near-infrared JHK passbands. We use our data to search for opacity-induced changes in the planetary radius, but find that all values agree with each other. Our data are therefore consistent with a flat transmission spectrum to within the observational uncertainties. We also measure an activity index of the host star of log R '[SUB]HK[/SUB] = -4.495, meaning that WASP-80 A shows strong chromospheric activity. The non-detection of starspots implies that, if they exist, they must be small and symmetrically distributed on the stellar surface. We model all available optical transit light curves and obtain improved physical properties and orbital ephemerides for the system. Full Table 2 is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/562/A126">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/562/A126</A>
Researchers ; Professionals
http://hdl.handle.net/2268/162006
also: http://hdl.handle.net/2268/218278
10.1051/0004-6361/201323265
http://esoads.eso.org/abs/2014A%26A...562A.126M

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