Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/239
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dc.rights.license© ESO 2020-
dc.contributor.authorCarleo, I.-
dc.contributor.authorMalavolta, L.-
dc.contributor.authorLanza, A. F.-
dc.contributor.authorDamasso, M.-
dc.contributor.authorDesidera, S.-
dc.contributor.authorBorsa, F.-
dc.contributor.authorMallonn, M.-
dc.contributor.authorPinamonti, M.-
dc.contributor.authorGratton, R.-
dc.contributor.authorAlei, E.-
dc.contributor.authorBenatti, S.-
dc.contributor.authorMancini, L.-
dc.contributor.authorMaldonado, J.-
dc.contributor.authorBiazzo, K.-
dc.contributor.authorEsposito, M.-
dc.contributor.authorFrustagli, G.-
dc.contributor.authorGonzález Álvarez, E.-
dc.contributor.authorMicela, G.-
dc.contributor.authorScandariato, G.-
dc.contributor.authorSozzatti, A.-
dc.contributor.authorAffer, L.-
dc.contributor.authorBignamini, A.-
dc.contributor.authorBonomo, A. S.-
dc.contributor.authorClaudi, R.-
dc.contributor.authorCosentino, R.-
dc.contributor.authorCovino, E.-
dc.contributor.authorFiorenzano, A. F. M.-
dc.contributor.authorGiacobbe, P.-
dc.contributor.authorHarutyunyan, A.-
dc.contributor.authorLeto, G.-
dc.contributor.authorMaggio, A.-
dc.contributor.authorMolinari, E.-
dc.contributor.authorNascimbeni, V.-
dc.contributor.authorPagano, I.-
dc.contributor.authorPedani, M.-
dc.contributor.authorPiotto, G.-
dc.contributor.authorPoretti, E.-
dc.contributor.authorRainer, M.-
dc.contributor.authorRedfield, S.-
dc.contributor.authorBaffa, C.-
dc.contributor.authorBaruffolo, A.-
dc.contributor.authorBuschschacher, N.-
dc.contributor.authorBilloti, V.-
dc.contributor.authorCecconi, M.-
dc.contributor.authorFalcini, G.-
dc.contributor.authorFantinel, D.-
dc.contributor.authorFini, L.-
dc.contributor.authorGalli, A.-
dc.contributor.authorGhedina, A.-
dc.contributor.authorGhinassi, F.-
dc.contributor.authorGiani, E.-
dc.contributor.authorGonzález, C.-
dc.contributor.authorGonzález, M.-
dc.contributor.authorGuerra, J.-
dc.contributor.authorHernández Díaz, M.-
dc.contributor.authorHernández, N.-
dc.contributor.authorLuzzolino, M.-
dc.contributor.authorLodi, M.-
dc.contributor.authorOliva, E.-
dc.contributor.authorOriglia, L.-
dc.contributor.authorPérez Ventura, H.-
dc.contributor.authorPuglisi, A.-
dc.contributor.authorRiverol, C.-
dc.contributor.authorRiverol, L.-
dc.contributor.authorSan Juan, J.-
dc.contributor.authorSanna, N.-
dc.contributor.authorScuderi, S.-
dc.contributor.authorSeemann, U.-
dc.contributor.authorSozzi, M.-
dc.contributor.authorTozzi, P.-
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.accessioned2021-04-12T10:09:14Z-
dc.date.available2021-04-12T10:09:14Z-
dc.date.issued2020-05-29-
dc.identifier.citationAstronomy and Astrophysics 638: A5(2020)es
dc.identifier.issn0004-6361-
dc.identifier.otherhttps://www.aanda.org/articles/aa/abs/2020/06/aa37369-19/aa37369-19.html-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/239-
dc.descriptionPhotometry, RV, and time series are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/638/A5 Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated by the Fundación Galileo Galilei (FGG) of the Istituto Nazionale di Astrofisica (INAF) at the Observatorio del Roque de los Muchachos (La Palma, Canary Islands, Spain). Partly based on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC.es
dc.description.abstractContext. The existence of hot Jupiters is still not well understood. Two main channels are thought to be responsible for their current location: a smooth planet migration through the protoplanetary disk or the circularization of an initial highly eccentric orbit by tidal dissipation leading to a strong decrease in the semimajor axis. Different formation scenarios result in different observable effects, such as orbital parameters (obliquity and eccentricity) or frequency of planets at different stellar ages. Aims. In the context of the GAPS Young Objects project, we are carrying out a radial velocity survey with the aim of searching and characterizing young hot-Jupiter planets. Our purpose is to put constraints on evolutionary models and establish statistical properties, such as the frequency of these planets from a homogeneous sample. Methods. Since young stars are in general magnetically very active, we performed multi-band (visible and near-infrared) spectroscopy with simultaneous GIANO-B + HARPS-N (GIARPS) observing mode at TNG. This helps in dealing with stellar activity and distinguishing the nature of radial velocity variations: stellar activity will introduce a wavelength-dependent radial velocity amplitude, whereas a Keplerian signal is achromatic. As a pilot study, we present here the cases of two known hot Jupiters orbiting young stars: HD 285507 b and AD Leo b. Results. Our analysis of simultaneous high-precision GIARPS spectroscopic data confirms the Keplerian nature of the variation in the HD 285507 radial velocities and refines the orbital parameters of the hot Jupiter, obtaining an eccentricity consistent with a circular orbit. Instead, our analysis does not confirm the signal previously attributed to a planet orbiting AD Leo. This demonstrates the power of the multi-band spectroscopic technique when observing active stars.es
dc.description.sponsorshipThe authors acknowledge support by INAF/WOW and INAF/FRONTIERA through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research. P.G. acknowledges financial support from the Italian Space Agency (ASI) under contract 2014-025-R.1.2015 to INAF. M.P. gratefully acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement No. 313014 (ETAEARTH); 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.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectInstrumentation: spectrographses
dc.subjectPlanetary systemses
dc.subjectTechniques: spectroscopices
dc.subjectStars: activityes
dc.subjectTechniques: radial velocitieses
dc.titleThe GAPS Programme at TNG XXI. A GIARPS case study of known young planetary candidates: confirmation of HD 285507 b and refutation of AD Leonis bes
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidClaudi, R. [0000-0001-7707-5105]-
dc.contributor.orcidLeto, G. [0000-0002-0040-5011]-
dc.contributor.orcidPiotto, G. [0000-0002-9937-6387]-
dc.contributor.orcidBonomo, A. S. [0000-0002-6177-198X]-
dc.contributor.orcidSozzetti, A. [0000-0002-7504-365X]-
dc.contributor.orcidBiazzo, K. [0000-0002-1892-2180]-
dc.contributor.orcidGhedina, A. [0000-0003-4702-5152]-
dc.contributor.orcidDamasso, M. [0000-0001-9984-4278]-
dc.contributor.orcidCosentino, R. [0000-0003-1784-1431]-
dc.identifier.doi10.1051/0004-6361/201937369-
dc.identifier.e-issn1432-0746-
dc.contributor.funderAgenzia Spaziale Italiana (ASI)-
dc.contributor.funderEuropean Commission (EC)-
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-
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/FP7/313014-
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