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dc.rights.license© ESO 2020-
dc.contributor.authorDamasso, D.-
dc.contributor.authorSozzetti, A-
dc.contributor.authorLovis, C.-
dc.contributor.authorBarros, S. C. C.-
dc.contributor.authorSousa, S. G.-
dc.contributor.authorDemangeon, O. D. S.-
dc.contributor.authorFaria, J. P.-
dc.contributor.authorLillo Box, J.-
dc.contributor.authorCristiani, S.-
dc.contributor.authorPepe, F.-
dc.contributor.authorRebolo, R.-
dc.contributor.authorSantos, N. C.-
dc.contributor.authorZapatero Osorio, M. R.-
dc.contributor.authorGonzález Hernández, J. I.-
dc.contributor.authorAmate, M.-
dc.contributor.authorPasquini, L.-
dc.contributor.authorZerbi, Filippo M.-
dc.contributor.authorAdibekyan, V.-
dc.contributor.authorAbreu, M.-
dc.contributor.authorAffolter, M.-
dc.contributor.authorAlibert, Y.-
dc.contributor.authorAliverti, M.-
dc.contributor.authorAllart, R.-
dc.contributor.authorAllende Prieto, C.-
dc.contributor.authorÁlvarez, D.-
dc.contributor.authorAlves, D.-
dc.contributor.authorÁvila, G.-
dc.contributor.authorBaldini, V.-
dc.contributor.authorBandy, T.-
dc.contributor.authorBenz, W.-
dc.contributor.authorBianco, A.-
dc.contributor.authorBorsa, F.-
dc.contributor.authorBossini, D.-
dc.contributor.authorBourrier, V.-
dc.contributor.authorBouchy, F.-
dc.contributor.authorBroeg, C.-
dc.contributor.authorCabral, A.-
dc.contributor.authorCalderone, G.-
dc.contributor.authorCirami, R.-
dc.contributor.authorCoelho, J.-
dc.contributor.authorConconi, P.-
dc.contributor.authorCoretti, I.-
dc.contributor.authorCumani, C.-
dc.contributor.authorCupani, G.-
dc.contributor.authorD´Odorico, V.-
dc.contributor.authorDeiries, S.-
dc.contributor.authorDekker, H.-
dc.contributor.authorDelabre, B.-
dc.contributor.authorDi Marcoantonio, P.-
dc.contributor.authorDumusque, X.-
dc.contributor.authorEhrenreich, D.-
dc.contributor.authorFigueira, P.-
dc.contributor.authorFragoso, A.-
dc.contributor.authorGenolet, L.-
dc.contributor.authorGenoni, M.-
dc.contributor.authorGénova Santos, R.-
dc.contributor.authorHughes, I.-
dc.contributor.authorIwert, O.-
dc.contributor.authorKerber, F.-
dc.contributor.authorKnudstrup, J.-
dc.contributor.authorLandoni, M.-
dc.contributor.authorLavie, B.-
dc.contributor.authorLizon, J. L.-
dc.contributor.authorLo Curto, G.-
dc.contributor.authorMaire, C.-
dc.contributor.authorMartins, C. J. A. P.-
dc.contributor.authorMégevand, D.-
dc.contributor.authorMehner, A.-
dc.contributor.authorMicela, G.-
dc.contributor.authorModigliani, A.-
dc.contributor.authorMolaro, P.-
dc.contributor.authorMonteiro, M. A.-
dc.contributor.authorMonteiro, M. J. P. F. G.-
dc.contributor.authorMoschetti, M.-
dc.contributor.authorMueller, E.-
dc.contributor.authorMurphy, M. T.-
dc.contributor.authorNunes, N.-
dc.contributor.authorOggioni, L.-
dc.contributor.authorOliveira, A.-
dc.contributor.authorOshagh, M.-
dc.contributor.authorPallé, E.-
dc.contributor.authorPariani, G.-
dc.contributor.authorPoretti, E.-
dc.contributor.authorRasilla, J. L.-
dc.contributor.authorRebordao, J.-
dc.contributor.authorRedaelli, E.-
dc.contributor.authorRiva, M.-
dc.contributor.authorSanta Tschudi, S.-
dc.contributor.authorSantin, P.-
dc.contributor.authorSantos, P.-
dc.contributor.authorSégransan, D.-
dc.contributor.authorSchmidt, T. M.-
dc.contributor.authorSegovia, A.-
dc.contributor.authorSosnowska, D.-
dc.contributor.authorSpanò, P.-
dc.contributor.authorSuárez Mascareño, A.-
dc.contributor.authorTabernero, H.-
dc.contributor.authorTenegi, F.-
dc.contributor.authorUdry, S.-
dc.contributor.authorZanutta, 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.accessioned2021-04-08T07:43:59Z-
dc.date.available2021-04-08T07:43:59Z-
dc.date.issued2020-10-01-
dc.identifier.citationAstronomy and Astrophysics 642: A31(2020)es
dc.identifier.issn0004-6361-
dc.identifier.otherhttps://www.aanda.org/articles/aa/full_html/2020/10/aa38416-20/aa38416-20.html-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/158-
dc.description.abstractContext. The bright star pi Men was chosen as the first target for a radial velocity follow-up to test the performance of ESPRESSO, the new high-resolution spectrograph at the European Southern Observatory's Very Large Telescope. The star hosts a multi-planet system (a transiting 4 M-circle plus planet at similar to 0.07 au and a sub-stellar companion on a similar to 2100-day eccentric orbit), which is particularly suitable for a precise multi-technique characterization. Aims. With the new ESPRESSO observations, which cover a time span of 200 days, we aim to improve the precision and accuracy of the planet parameters and search for additional low-mass companions. We also take advantage of the new photometric transits of pi Men c observed by TESS over a time span that overlaps with that of the ESPRESSO follow-up campaign. Methods. We analysed the enlarged spectroscopic and photometric datasets and compared the results to those in the literature. We further characterized the system by means of absolute astrometry with HIPPARCOS and Gaia. We used the high-resolution spectra of ESPRESSO for an independent determination of the stellar fundamental parameters. Results. We present a precise characterization of the planetary system around pi Men. The ESPRESSO radial velocities alone (37 nightly binned data with typical uncertainty of 10 cm s(-1)) allow for a precise retrieval of the Doppler signal induced by pi Men c. The residuals show a root mean square of 1.2 m s(-1), which is half that of the HARPS data; based on the residuals, we put limits on the presence of additional low-mass planets (e.g. we can exclude companions with a minimum mass less than similar to 2 M-circle plus within the orbit of pi Men c). We improve the ephemeris of pi Men c using 18 additional TESS transits, and, in combination with the astrometric measurements, we determine the inclination of the orbital plane of pi Men b with high precision (i(b) =45.8(-1.1)(+1.4) deg). This leads to precise measurement of its absolute mass m(b) = =14.1(-0.4)(+0.5) M-Jup, indicating that pi Men b can be classified as a brown dwarf. Conclusions. The pi Men system represents a nice example of the extreme precision radial velocities that can be obtained with ESPRESSO for bright targets. Our determination of the 3D architecture of the pi Men planetary system and the high relative misalignment of the planetary orbital planes put constraints on and challenge the theories of the formation and dynamical evolution of planetary systems. The accurate measurement of the mass of pi Men b contributes to make the brown dwarf desert a bit greener.es
dc.description.sponsorshipWe thank the referee Pierre Kervella for his comments that improved the contents of this work. M.D. acknowledges financial support from Progetto Premiale 2015 FRONTIERA (OB.FU. 1.05.06.11) funding scheme of the Italian Ministry of Education, University, and Research, and also acknowledge the computing centres of INAF -Osservatorio Astronomico di Trieste/Osservatorio Astrofisico di Catania, under the coordination of the CHIPP project, for the availability of computing resources and support. C.L. and F.P. would like to acknowledge the Swiss National Science Foundation (SNSF) for supporting research with ESPRESSO through the SNSF grants nr. 140649, 152721, 166227 and 184618. The ESPRESSO Instrument Project was partially funded through SNSF's FLARE Programme for large infrastructures. This work has been carried out in part within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This work was supported by FCT -Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987. S.C.C.B., V.Z.A., S.G.S. and J.P.S.F. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00650/2015/CP1273/CT0001, IF/00028/2014/CP1215/CT0002, DL 57/2016/CP1364/CT0005. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Funda cao para a Ciencia e Tecnologia (FCT). J.L.-B. has been funded by the Spanish State Research Agency (AEI) Projects No.ESP201787676-C5-1-R and No. MDM-2017-0737 Unidad de Excelencia "Maria de Maeztu"-Centro de Astrobiologia (INTA-CSIC). J.P.F. is supported in the form of a work contract funded by national funds through FCT with reference DL57/2016/CP1364/CT0005. V.B. acknowledges support by the Swiss National Science Foundation (SNSF) in the frame of the National Centre for Competence in Research "PlanetS". This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project Four Aces, grant agreement No 724427). R.R., C.A.P., J.I.G.H., A.S.M., and M.R.Z.O. acknowledge financial support from the Spanish Ministry of Science and Innovation (MICINN) projects AYA2017-86389-P and AYA2016-79425-C3-2-P. J.I.G.H. acknowledges financial support from the Spanish MICINN under the 2013 Ramon y Cajal program RYC-2013-14875. M.T.M. thanks the Australian Research Council for Future Fellowship grant FT180100194 which supported this work. Partial financial support from the agreement ASI-INAF n.2018-16-HH.0 is gratefully acknowledgded. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualization, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ches
dc.language.isoenges
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-87676-C5-1-R-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-86389-P/ES/ESPECTROSCOPIA DE ALTA RESOLUCION ORIENTADA AL ESTUDIO DE EXOTIERRAS Y LA FORMACION DE LA VIA LACTEA. EXPLOTACION CIENTIFICA DE ESPRESSO Y HORS/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-79425-C3-2-P/ES/ENANAS MARRONES Y PLANETAS AISLADOS Y COMO COMPAÑEROS DE ESTRELLAS/-
dc.relationinfo:eu-repo/grantAgreement/MINECO//RYC-2013-14875-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectTechniques: radial velocitieses
dc.subjectTechniques: photometrices
dc.subjectAstrometryes
dc.subjectPlanetary systemses
dc.subjectstars: individual:es
dc.subjectpi Menes
dc.titleA precise architecture characterization of the π Mensae planetary systemes
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcid0000-0003-0987-1593-
dc.identifier.doi10.1051/0004-6361/202038416-
dc.identifier.e-issn1432-0746-
dc.contributor.funderSwiss National Science Foundation (SNSF)-
dc.contributor.funderAgenzia Spaziale Italiana (ASI)-
dc.contributor.funderFundação para a Ciência e a Tecnologia (FCT)-
dc.contributor.funderAustralian Research Council (ARC)-
dc.contributor.funderIstituto Nazionale Astrofisica (INAF)-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/H2020/724427-
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