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Authordc.contributor.authorBonnefoy, M. 
Authordc.contributor.authorZurlo, A. 
Authordc.contributor.authorBaudino, J. L. 
Authordc.contributor.authorLucas, P. 
Authordc.contributor.authorMesa, D. 
Authordc.contributor.authorMaire, Anne-Lise 
Authordc.contributor.authorVigan, A. 
Authordc.contributor.authorGalicher, R. 
Authordc.contributor.authorHomeier, D. 
Authordc.contributor.authorMarocco, F. 
Authordc.contributor.authorGratton, R. 
Authordc.contributor.authorChauvin, G. 
Authordc.contributor.authorAllard, F. 
Authordc.contributor.authorDesidera, S. 
Authordc.contributor.authorKasper, M. 
Authordc.contributor.authorMoutou, C. 
Authordc.contributor.authorLagrange, Anne Marie 
Authordc.contributor.authorAntichi, J. 
Authordc.contributor.authorBaruffolo, A. 
Authordc.contributor.authorBaudrand, J. 
Authordc.contributor.authorBeuzit, J. -L. 
Authordc.contributor.authorBoccaletti, A. 
Authordc.contributor.authorCantalloube, F. 
Authordc.contributor.authorCarbillet, M. 
Authordc.contributor.authorCharton, J. 
Authordc.contributor.authorClaudi, R. U. 
Authordc.contributor.authorCostille, A. 
Authordc.contributor.authorDohlen, K. 
Authordc.contributor.authorDominik, C. 
Authordc.contributor.authorFantinel, D. 
Authordc.contributor.authorFeautrier, P. 
Authordc.contributor.authorFeldt, M. 
Authordc.contributor.authorFusco, T. 
Authordc.contributor.authorGigan, P. 
Authordc.contributor.authorGirard, J. H. 
Authordc.contributor.authorGluck, L. 
Authordc.contributor.authorGry, C. 
Authordc.contributor.authorHenning, Thomas 
Authordc.contributor.authorJanson, M. 
Authordc.contributor.authorLanglois, M. 
Authordc.contributor.authorMadec, F. 
Authordc.contributor.authorMagnard, Y. 
Authordc.contributor.authorMaurel, D. 
Authordc.contributor.authorMawet, D. 
Authordc.contributor.authorMeyer, M. R. 
Authordc.contributor.authorMilli, J. 
Authordc.contributor.authorMoeller-Nilsson, O. 
Authordc.contributor.authorMouillet, D. 
Authordc.contributor.authorPavlov, A. 
Authordc.contributor.authorPerret, D. 
Authordc.contributor.authorPujet, P. 
Authordc.contributor.authorQuanz, S. P. 
Authordc.contributor.authorRochat, S. 
Authordc.contributor.authorRousset, G. 
Authordc.contributor.authorRoux, A. 
Authordc.contributor.authorSalasnich, B. 
Authordc.contributor.authorSalter, G. 
Authordc.contributor.authorSauvage, Jean Francois 
Authordc.contributor.authorSchmid, H. M. 
Authordc.contributor.authorSevin, A. 
Authordc.contributor.authorSoenke, C. 
Authordc.contributor.authorStadler, E. 
Authordc.contributor.authorTuratto, M. 
Authordc.contributor.authorUdry, S. 
Authordc.contributor.authorVakili, F. 
Authordc.contributor.authorWahhaj, Z. 
Authordc.contributor.authorWildi, F. 
Admission datedc.date.accessioned2016-12-19T20:09:28Z
Available datedc.date.available2016-12-19T20:09:28Z
Publication datedc.date.issued2016-03
Cita de ítemdc.identifier.citationA&A 587, A58 (2016)es_ES
Identifierdc.identifier.issn1432-0746
Identifierdc.identifier.other10.1051/0004-6361/201526906
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/141974
Abstractdc.description.abstractContext. The system of four planets discovered around the intermediate-mass star HR8799 offers a unique opportunity to test planet formation theories at large orbital radii and to probe the physics and chemistry at play in the atmospheres of self-luminous young (similar to 30 Myr) planets. We recently obtained new photometry of the four planets and low-resolution (R similar to 30) spectra of HR8799 d and e with the SPHERE instrument (Paper III). Aims. In this paper (Paper IV), we aim to use these spectra and available photometry to determine how they compare to known objects, what the planet physical properties are, and how their atmospheres work. Methods. We compare the available spectra, photometry, and spectral energy distribution (SED) of the planets to field dwarfs and young companions. In addition, we use the extinction from corundum, silicate (enstatite and forsterite), or iron grains likely to form in the atmosphere of the planets to try to better understand empirically the peculiarity of their spectrophotometric properties. To conclude, we use three sets of atmospheric models (BT-SETTL14, Cloud-AE60, Exo-REM) to determine which ingredients are critically needed in the models to represent the SED of the objects, and to constrain their atmospheric parameters (T-eff, log g, M/H). Results. We find that HR8799d and e properties are well reproduced by those of L6-L8 dusty dwarfs discovered in the field, among which some are candidate members of young nearby associations. No known object reproduces well the properties of planets b and c. Nevertheless, we find that the spectra and WISE photometry of peculiar and/or young early-T dwarfs reddened by submicron grains made of corundum, iron, enstatite, or forsterite successfully reproduce the SED of these planets. Our analysis confirms that only the Exo-REM models with thick clouds fit (within 2 sigma) the whole set of spectrophotometric datapoints available for HR8799 d and e for T-eff = 1200 K, log g in the range 3.0-4.5, and M/H = +0.5. The models still fail to reproduce the SED of HR8799c and b. The determination of the metallicity, log g, and cloud thickness are degenerate. Conclusions. Our empirical analysis and atmospheric modelling show that an enhanced content in dust and decreased CIA of H-2 is certainly responsible for the deviation of the properties of the planet with respect to field dwarfs. The analysis suggests in addition that HR8799c and b have later spectral types than the two other planets, and therefore could both have lower masses.es_ES
Patrocinadordc.description.sponsorshipNucleus RC130007es_ES
Lenguagedc.language.isoenes_ES
Publisherdc.publisherEDP Sciences S.A.es_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Sourcedc.sourceAstronomy and Astrophysicses_ES
Keywordsdc.subjectinstrumentation: high angular resolutiones_ES
Keywordsdc.subjectstars: individual: HR8799es_ES
Keywordsdc.subjectplanets and satellites: atmosphereses_ES
Keywordsdc.subjectplanets and satellites: detectiones_ES
Keywordsdc.subjecttechniques: imaging spectroscopyes_ES
Keywordsdc.subjectplanets and satellites: fundamental parameterses_ES
Títulodc.titleFirst light of the VLT planet finder SPHERE IV. Physical and chemical properties of the planets around HR8799es_ES
Document typedc.typeArtículo de revista
Catalogueruchile.catalogadorcctes_ES
Indexationuchile.indexArtículo de publicación ISIes_ES


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Attribution-NonCommercial-NoDerivs 3.0 Chile
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile