Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/122
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dc.rights.license© ESO 2020-
dc.contributor.authorHidalgo, D.-
dc.contributor.authorPallé, E.-
dc.contributor.authorAlonso, R.-
dc.contributor.authorGandolfi, D.-
dc.contributor.authorFridlund, M.-
dc.contributor.authorNowak, G.-
dc.contributor.authorLuque, R.-
dc.contributor.authorHirano, T.-
dc.contributor.authorJustesen, A. B.-
dc.contributor.authorCochran, W. D.-
dc.contributor.authorBarragán, O.-
dc.contributor.authorSpina, L.-
dc.contributor.authorRodler, F.-
dc.contributor.authorAlbrecht, S.-
dc.contributor.authorAnderson, D.-
dc.contributor.authorAmado, P. J.-
dc.contributor.authorBryant, E.-
dc.contributor.authorCaballero, J. A.-
dc.contributor.authorCabrera, J.-
dc.contributor.authorCsizmadia, Sz.-
dc.contributor.authorDai, F.-
dc.contributor.authorDe Leon, J.-
dc.contributor.authorDeeg, H. J.-
dc.contributor.authorEigmuller, Ph.-
dc.contributor.authorEndl, M.-
dc.contributor.authorErikson, A.-
dc.contributor.authorEsposito, M.-
dc.contributor.authorFigueira, P.-
dc.contributor.authorGeorgieva, I.-
dc.contributor.authorGrziwa, S.-
dc.contributor.authorGuenther, E. W.-
dc.contributor.authorHatzes, A. P.-
dc.contributor.authorHjorth, M.-
dc.contributor.authorHoeijmakers, H. J.-
dc.contributor.authorKabath, P.-
dc.contributor.authorKorth, J.-
dc.contributor.authorKuzuhara, M.-
dc.contributor.authorLafarga, M.-
dc.contributor.authorLampón, M.-
dc.contributor.authorLeao, I. C.-
dc.contributor.authorLivingston, J.-
dc.contributor.authorMathur, S.-
dc.contributor.authorMontañés Rodríguez, P.-
dc.contributor.authorMorales, J. C.-
dc.contributor.authorMurgas Alcaino, F.-
dc.contributor.authorNagel, E.-
dc.contributor.authorNarita, N.-
dc.contributor.authorNielsen, L. D.-
dc.contributor.authorPatzold, M.-
dc.contributor.authorPersson, C. M.-
dc.contributor.authorPrieto Arranz, J.-
dc.contributor.authorQuirrenbach, A.-
dc.contributor.authorRauer, H.-
dc.contributor.authorRedfield, S.-
dc.contributor.authorReiners, A.-
dc.contributor.authorRibas, I.-
dc.contributor.authorSmith, A. M. S.-
dc.contributor.authorSubjak, J.-
dc.contributor.authorVan Eylen, V.-
dc.contributor.authorWilson, P. A.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.date.accessioned2021-03-24T08:30:22Z-
dc.date.available2021-03-24T08:30:22Z-
dc.date.issued2020-04-24-
dc.identifier.citationAstronomy & Astrophysics 636: A89 (2020)es
dc.identifier.issn0004-6361-
dc.identifier.otherhttps://www.aanda.org/articles/aa/abs/2020/04/aa37080-19/aa37080-19.html-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/122-
dc.description.abstractWe report the discovery of a new planetary system with three transiting planets, one super-Earth and two sub-Neptunes, that orbit EPIC 249893012, a G8 IV-V evolved star ( M ? = 1.05 0.05 M fi, R ? = 1.71 0.04 R fi, Te ff = 5430 85 K). The star is just leaving the main sequence. We combined K2 photometry with IRCS adaptive-optics imaging and HARPS, HARPS-N, and CARMENES highprecision radial velocity measurements to confirm the planetary system, determine the stellar parameters, and measure radii, masses, and densities of the three planets. With an orbital period of 3:5949+0:0007 0:0007 days, a mass of 8:75+1:09 1:08 M , and a radius of 1:95+0:09 0:08 R , the inner planet b is compatible with nickel-iron core and a silicate mantle ( b = 6:39+1:19 1:04 g cm 3). Planets c and d with orbital periods of 15:624+0:001 0:001 and 35:747+0:005 0:005 days, respectively, have masses and radii of 14:67+1;84 1:89 M and 3:67+0:17 0:14 R and 10:18+2:46 2:42 M and 3:94+0:13 0:12 R , respectively, yielding a mean density of 1:62+0:30 0:29 and 0:91+0:25 0:23 g cm 3, respectively. The radius of planet b lies in the transition region between rocky and gaseous planets, but its density is consistent with a rocky composition. Its semimajor axis and the corresponding photoevaporation levels to which the planet has been exposed might explain its measured density today. In contrast, the densities and semimajor axes of planets c and d suggest a very thick atmosphere. The singularity of this system, which orbits a slightly evolved star that is just leaving the main sequence, makes it a good candidate for a deeper study from a dynamical point of view.es
dc.description.sponsorshipD.H. acknowledges the Spanish Ministry of Economy and Competitiveness (MINECO) for the financial support under the FPI programme BES-2015-075200. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through project ESP2016-80435-C2-2-R. This work is partly supported by JSPS KAKENHI Grant Numbers JP18H01265 and JP18H05439, and JST PRESTO Grant Number JPMJPR1775. This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions. S.M. acknowledges support from the Spanish Ministry under the Ramon y Cajal fellowship number RYC-2015-17697. H.J.D. and G.N. acknowledge support by grant ESP2017-87676-C5-4-R of the Spanish Secretary of State for R&D&i (MINECO). Sz.Cs., M.E., S.G., A.P.H., J.K., K.W.F.L., M.P. and H.R. acknowledge support by DFG grants PA525/18-1, PA525/19-1, PA525/20-1, HA3279/12-1 and RA714/14-1 within the DFG Schwerpunkt SPP 1992, "Exploring the Diversity of Extrasolar Planets". I.C.L. acknowledges CNPq, CAPES, and FAPERN Brazilian agencies. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has made use of data from the European Space Agency (ESA) mission Gaia12, processed by the Gaia Data Processing and Analysis Consortium (DPAC13). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper has made use of data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.language.isoenges
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2016-80435-C2-2-R/ES/HACIA LA CARACTERIZACION DE ATMOSFERAS PLANETARIAS Y LA BUSQUEDA DE VIDA: CHEOPS, CARMENES, PLATO, ARIEL Y HIRES/-
dc.relationinfo:eu-repo/grantAgreement/MINECO//RYC-2015-17697-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-87676-C5-4-R-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectPlanetary systemses
dc.subjectPlanets and satellites: detectiones
dc.subjectPlanets and satellites: fundamental parameterses
dc.subjectTechniques: photometrices
dc.subjectTechniques: radial velocitieses
dc.titleThree planets transiting the evolved star EPIC 249893012: A hot 8.8-M super-Earth and two warm 14.7 and 10.2-M sub-Neptuneses
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidHidalgo, D. [0000-0002-7340-6963]-
dc.identifier.doi10.1051/0004-6361/201937080-
dc.identifier.e-issn1432-0746-
dc.contributor.funderMinisterio de Economía y Competitividad (MINECO)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderDeutsche Forschungsgemeinschaft (DFG)-
dc.contributor.funderJapan Science and Technology Agency (JST)-
dc.description.peerreviewedPeer reviewes
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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