J/MNRAS/428/678ivo://CDS.VizieR/J/MNRAS/428/678doi:10.26093/cds/vizier.74280678CDSTurner J.D.Smart B.M.Hardegree-Ullman K.K.Carleton T.M.,Walker-Lafollette A.M.Crawford B.E.Smith C.-T.W.McGraw A.M.,Small L.C.Rocchetto M.Cunningham K.I.Towner A.P.M.Zellem R.,Robertson A.N.Guvenen B.C.Schwarz K.R.Hardegree-Ullman E.E.,Collura D.Henz T.N.Lejoly C.Richardson L.L.Weinand M.A.,Taylor J.M.Daugherty M.J.Wilson A.A.Austin C.L.2024-07-20T20:13:40Z2016-04-21T09:12:11ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starssolar-system-planetsccd-photometryWe observed nine primary transits of the hot Jpiter TrES-3b in several optical and near-UV photometric bands from 2009 June to 2012 April in an attempt to detect its magnetic field. Vidotto, Jardine and Helling suggest that the magnetic field of TrES-3b can be constrained if its near-UV light curve shows an early ingress compared to its optical light curve, while its egress remains unaffected. Predicted magnetic field strengths of Jupiter-like planets should range between 8G and 30G. Using these magnetic field values and an assumed B* of 100G, the Vidotto et al. method predicts a timing difference of 5-11min. We did not detect an early ingress in our three nights of near-UV observations, despite an average cadence of 68 s and an average photometric precision of 3.7mmag. However, we determined an upper limit of TrES-3b's magnetic field strength to range between 0.013 and 1.3G (for a 1-100G magnetic field strength range for the host star, TrES-3) using a timing difference of 138s derived from the Nyquist-Shannon sampling theorem. To verify our results of an abnormally small magnetic field strength for TrES-3b and to further constrain the techniques of Vidotto et al., we propose future observations of TrES-3b with other platforms capable of achieving a shorter near-UV cadence. We also present a refinement of the physical parameters of TrES-3b, an updated ephemeris and its first published near-UV light curve. We find that the near-UV planetary radius of Rp=1.386+0.248-0.144RJup is consistent with the planet's optical radius.2013MNRAS.428..678Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/428/678CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/AJ/136/267 : Six occultations of the exoplanet TrES-3 (Winn+, 2008)J/ApJ/691/1145 : Spectrophotometry of TrES-3 and TrES-4 (Sozzetti+, 2009)J/MNRAS/408/1494 : Planetary transits of TrES-2 and TrES-3 (Colon+, 2010)J/AJ/145/68 : Five new transit light curves of TrES-3 (Jiang+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/428/678https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/428/678http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/428/678https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/428/678https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/428/678http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/428/678GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/428/678/lcLight curves of TrES-3brecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFilt[UBVR J-CR] Filter (1)meta.id;instr.filtercharHJDHeliocentric Julian Date (HJD-2450000)dtime.epochdoubleFluxRelative fluxphot.flux;arith.ratiodouble