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Physical properties of the WASP-67 planetary system from multi-colour photometry
Mancini, L1; Southworth, J2; Ciceri, S1; Novati, SC3,4; Dominik, M5; Henning, T1; Jorgensen, UG6,7; Korhonen, H6,7,8; Nikolov, N9; Alsubai, KA10; Bozza, V4,11; Bramich, DM12; D'Ago, G4,11; Jaimes, RF5,13; Galianni, P5; Gu SH(顾盛宏)14,15; Harpsoe, K6,7; Hinse, TC16; Hundertmark, M5; Juncher, D6,7; Kains, N17; Popovas, A6,7; Rabus, M1,18; Rahvar, S19; Skottfelt, J6,7; Snodgrass, C20; Street, R; Surdej, J; Tsapras, Y; Vilela, C2; Wang XB(王晓彬)14,15; Wertz, O
Source PublicationASTRONOMY & ASTROPHYSICS
2014-08
Volume568
DOI10.1051/0004-6361/201424106
Contribution Rank第14完成单位
Indexed BySCI ; EI
KeywordPlanetary Systems Stars: Fundamental Parameters Techniques: Photometric
Abstract

Context. The extrasolar planet WASP-67 b is the first hot Jupiter definitively known to undergo only partial eclipses. The lack of the second and third contact points in this planetary system makes it difficult to obtain accurate measurements of its physical parameters. 

Aims. By using new high precision photometric data we confirm that WASP-67 b shows grazing eclipses and compute accurate estimates of the physical properties of the planet and its parent star. 

Methods. We present high-quality. multi-colour, broad-band photometric observations comprising five light curves covering two transit events, obtained using two medium-class telescopes and the telescope defocusing technique. One transit was observed through a Bessel-R filter and the other simultaneously through filters similar to Sloan g ' r ' i ' z ' We modelled these data using,JKTEBOP. The physical parameters of the system were obtained from the analysis of these light curves and from published spectroscopic measurements. 

Results. All five of our light curves satisfy the criterion for being grazing eclipses. We revise the physical parameters of the whole WASP 67 system and, in particular. significantly improve the measurements of the planet's radius (R-b = 1.091 +/- 0.046 R-Jup) and density(rho(b) = 0.292 +/- 0.036 rho(Jup)), as compared to the values in the discovery paper (Rb = 1.4(-0.2)(+0.3) R-Jup and rho(b), = 0.16 +/- 0.08 rho(Jup)) The transit ephemeris was also substantially refined. We investigated the variation of the planet's radius as a function of the wavelength, using the simultaneous multi-band data finding that our measurements are consistent with a Oat spectrum to within the experimental uncertainties.

Funding ProjectDanish Natural Science Research Council (FNU) ; STFC in the form of an Advanced Fellowship ; European Union Seventh Framework Programme (FP7/2007-2013)[268421] ; FONDECYT postdoctoral fellowship [3120097] ; KASI grant[2014-1-400-06] ; European Commission under the Marie Curie Intra-European Fellowship Programme in FP7 ; National Natural Science Foundation of China[10873031] ; Chinese Academy of Sciences[KJCX2-YW-T24] ; Belgian National Fund for Scientific Research (FNRS) ; Communauté française de Belgique − Actions de recherche concertées – Académie universitaire Wallonie-Europe ; Qatar National Research Fund (a member of Qatar Foundation)[NPRP-09-476-1-7] ; NPRP grant from the Qatar National Research Fund[X-019-1-006]
Funding OrganizationDanish Natural Science Research Council (FNU) ; STFC in the form of an Advanced Fellowship ; European Union Seventh Framework Programme (FP7/2007-2013)[268421] ; FONDECYT postdoctoral fellowship [3120097] ; KASI grant[2014-1-400-06] ; European Commission under the Marie Curie Intra-European Fellowship Programme in FP7 ; National Natural Science Foundation of China[10873031] ; Chinese Academy of Sciences[KJCX2-YW-T24] ; Belgian National Fund for Scientific Research (FNRS) ; Communauté française de Belgique − Actions de recherche concertées – Académie universitaire Wallonie-Europe ; Qatar National Research Fund (a member of Qatar Foundation)[NPRP-09-476-1-7] ; NPRP grant from the Qatar National Research Fund[X-019-1-006]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherEDP SCIENCES S A
Publication Place17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN0004-6361
URL查看原文
WOS IDWOS:000341185900111
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordTRANSITING EXTRASOLAR PLANETS ; STELLAR EVOLUTION DATABASE ; HOT JUPITERS ; LIGHT CURVES ; MODELS ; ISOCHRONES ; RADIUS ; MASS ; ATMOSPHERES ; TELESCOPE
EI Accession Number20143700065295
EI KeywordsExtrasolar planets
EI Classification Number657.2Extraterrestrial Physics and Stellar Phenomena - 941.4Optical Variables Measurements
Citation statistics
Cited Times:17[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6799
Collection系外行星研究组
中国科学院天体结构与演化重点实验室
Corresponding AuthorMancini, L
Affiliation1.Max-Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
2.Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK
3.International Institute for Advanced Scientific Studies (IIASS), 84019 Vietri Sul Mare (SA), Italy
4.Department of Physics, University of Salerno, Via Giovanni Paolo II, 84084 Fisciano, Italy
5.SUPA, University of St Andrews, School of Physics & Astronomy, North Haugh, St Andrews, KY16 9SS, UK
6.Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100 Copenhagen Ø, Denmark
7.Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
8.Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
9.Astrophysics Group, University of Exeter, Stocker Road, EX4 4QL, Exeter, UK
10.Qatar Foundation, PO Box 5825, Doha, Qatar
11.Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Napoli, 80126 Napoli, Italy
12.Qatar Environment and Energy Research Institute, Qatar Foundation, Tornado Tower, Floor 19, PO Box 5825, Doha, Qatar
13.European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching bei München, Germany
14.Yunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, PR China
15.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011 Kunming, PR China
16.Korea Astronomy and Space Science Institute, Daejeon 305-348, Republic of Korea
17.Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
18.Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
19.Department of Physics, Sharif University of Technology, PO Box 11155-9161 Tehran, Iran
20.Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
Recommended Citation
GB/T 7714
Mancini, L,Southworth, J,Ciceri, S,et al. Physical properties of the WASP-67 planetary system from multi-colour photometry[J]. ASTRONOMY & ASTROPHYSICS,2014,568.
APA Mancini, L.,Southworth, J.,Ciceri, S.,Novati, SC.,Dominik, M.,...&Wertz, O.(2014).Physical properties of the WASP-67 planetary system from multi-colour photometry.ASTRONOMY & ASTROPHYSICS,568.
MLA Mancini, L,et al."Physical properties of the WASP-67 planetary system from multi-colour photometry".ASTRONOMY & ASTROPHYSICS 568(2014).
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