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dc.contributor.authorCiceri, S.
dc.contributor.authorMancini, L.
dc.contributor.authorSouthworth, J.
dc.contributor.authorLendl, M.
dc.contributor.authorTregloan-Reed, J.
dc.contributor.authorBrahm, R.
dc.contributor.authorChen, G.
dc.contributor.authorD'Ago, G.
dc.contributor.authorDominik, Martin
dc.contributor.authorFiguera Jaimes, R.
dc.contributor.authorGalianni, P.
dc.contributor.authorHarpsøe, K.
dc.contributor.authorHinse, T. C.
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorJuncher, D.
dc.contributor.authorKorhonen, H.
dc.contributor.authorLiebig, C.
dc.contributor.authorRabus, M.
dc.contributor.authorBonomo, A. S.
dc.contributor.authorBott, K.
dc.contributor.authorHenning, Th
dc.contributor.authorJordán, A.
dc.contributor.authorSozzetti, A.
dc.contributor.authorAlsubai, K. A.
dc.contributor.authorAndersen, J. M.
dc.contributor.authorBajek, D.
dc.contributor.authorBozza, V.
dc.contributor.authorBramich, D. M.
dc.contributor.authorBrowne, P.
dc.contributor.authorCalchi Novati, S.
dc.contributor.authorDamerdji, Y.
dc.contributor.authorDiehl, C.
dc.contributor.authorElyiv, A.
dc.contributor.authorGiannini, E.
dc.contributor.authorGu, S-H.
dc.contributor.authorHundertmark, M.
dc.contributor.authorKains, N.
dc.contributor.authorPenny, M.
dc.contributor.authorPopovas, A.
dc.contributor.authorRahvar, S.
dc.contributor.authorScarpetta, G.
dc.contributor.authorSchmidt, R. W.
dc.contributor.authorSkottfelt, J.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSurdej, J.
dc.contributor.authorVilela, C.
dc.contributor.authorWang, X. B.
dc.contributor.authorWertz, O.
dc.identifier.citationCiceri , S , Mancini , L , Southworth , J , Lendl , M , Tregloan-Reed , J , Brahm , R , Chen , G , D'Ago , G , Dominik , M , Figuera Jaimes , R , Galianni , P , Harpsøe , K , Hinse , T C , Jørgensen , U G , Juncher , D , Korhonen , H , Liebig , C , Rabus , M , Bonomo , A S , Bott , K , Henning , T , Jordán , A , Sozzetti , A , Alsubai , K A , Andersen , J M , Bajek , D , Bozza , V , Bramich , D M , Browne , P , Calchi Novati , S , Damerdji , Y , Diehl , C , Elyiv , A , Giannini , E , Gu , S-H , Hundertmark , M , Kains , N , Penny , M , Popovas , A , Rahvar , S , Scarpetta , G , Schmidt , R W , Skottfelt , J , Snodgrass , C , Surdej , J , Vilela , C , Wang , X B & Wertz , O 2016 , ' Physical properties of the planetary systems WASP-45 and WASP-46 from simultaneous multiband photometry ' Monthly Notices of the Royal Astronomical Society , vol. 456 , no. 1 , pp. 990-1002 . DOI: 10.1093/mnras/stv2698en
dc.identifier.otherPURE: 241576484
dc.identifier.otherPURE UUID: 13ec4c9d-4f85-426d-93fb-83f48c756009
dc.identifier.otherScopus: 84959538333
dc.descriptionThis work was supported by KASI (Korea Astronomy and Space Science Institute) grants 2012-1-410-02 and 2013-9-400-00. ASB acknowledges support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). TCH acknowledges financial support from the Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Program. YD, AE, JSurdej and OW acknowledge support from the Communauté française de Belgique – Actions de recherche concertées – Académie Wallonie-Europe. SHG and XBW would like to thank the financial support from National Natural Science Foundation of China through grants nos. 10873031 and 11473066.en
dc.description.abstractAccurate measurements of the physical characteristics of a large number of exoplanets are useful to strongly constrain theoretical models of planet formation and evolution, which lead to the large variety of exoplanets and planetary-system configurations that have been observed. We present a study of the planetary systemsWASP-45 andWASP-46, both composed of a mainsequence star and a close-in hot Jupiter, based on 29 new high-quality light curves of transits events. In particular, one transit of WASP-45 b and four of WASP-46 b were simultaneously observed in four optical filters, while one transit of WASP-46 b was observed with the NTT obtaining a precision of 0.30 mmag with a cadence of roughly 3 min. We also obtained five new spectra of WASP-45 with the FEROS spectrograph. We improved by a factor of 4 the measurement of the radius of the planet WASP-45 b, and found that WASP-46 b is slightly less massive and smaller than previously reported. Both planets now have a more accurate measurement of the density (0.959 ± 0.077 ρJup instead of 0.64 ± 0.30 ρJup for WASP-45 b, and 1.103 ± 0.052 ρJup instead of 0.94 ± 0.11 ρJup for WASP-46 b). We tentatively detected radius variations with wavelength for both planets, in particular in the case of WASP-45 b we found a slightly larger absorption in the redder bands than in the bluer ones. No hints for the presence of an additional planetary companion in the two systems were found either from the photometric or radial velocity measurements.en
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2015 The Authors. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at
dc.subjectPlanets and satellites: fundamental parametersen
dc.subjectStars: fundamental parametersen
dc.subjectStars: individual: WASP-45en
dc.subjectStars: individual: WASP-46en
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectSpace and Planetary Scienceen
dc.subjectAstronomy and Astrophysicsen
dc.titlePhysical properties of the planetary systems WASP-45 and WASP-46 from simultaneous multiband photometryen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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