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dc.contributor.authorBonnefoy, M.
dc.contributor.authorMarleau, G.-D.
dc.contributor.authorGalicher, R.
dc.contributor.authorBeust, H.
dc.contributor.authorLagrange, A.-M.
dc.contributor.authorBaudino, J. -L.
dc.contributor.authorChauvin, G.
dc.contributor.authorBorgniet, S.
dc.contributor.authorMeunier, N.
dc.contributor.authorRameau, J.
dc.contributor.authorBoccaletti, A.
dc.contributor.authorCumming, A.
dc.contributor.authorHelling, C.
dc.contributor.authorHomeier, D.
dc.contributor.authorAllard, F.
dc.contributor.authorDelorme, P.
dc.identifier.citationBonnefoy , M , Marleau , G-D , Galicher , R , Beust , H , Lagrange , A-M , Baudino , J -L , Chauvin , G , Borgniet , S , Meunier , N , Rameau , J , Boccaletti , A , Cumming , A , Helling , C , Homeier , D , Allard , F & Delorme , P 2014 , ' Physical and orbital properties of Beta Pictoris b ' , Astronomy & Astrophysics , vol. 567 , L9 .
dc.identifier.otherPURE: 157156766
dc.identifier.otherPURE UUID: 5f8acc79-9d40-4c33-8356-d2005c42c856
dc.identifier.otherScopus: 84905495862
dc.identifier.otherWOS: 000341185300145
dc.descriptionM.B., G.C., A.M.L., J.R., H.B., F.A., and D.H. acknowledge financial support from the French National Research Agency (ANR) through project grant, ANR10- BLANC0504-01, ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01, and ANR- 2010-JCJC-0501-01. ChH and DH highlight EU financial support under FP7 by starting grant. J.L.B. Ph.D is funded by the LabEx Exploration Spatiale des Environnements Planétaires (ESEP) # 2011-LABX-030.en
dc.description.abstractThe intermediate-mass star Beta Pictoris is known to be surrounded by a structured edge-on debris disk within which a gas giant planet was discovered orbiting at 8-10 AU. The physical properties of Beta Pic b were previously inferred from broad- and narrow-band 0.9-4.8 microns photometry. We used commissioning data of the Gemini Planet Imager (GPI) to obtain new astrometry and a low-resolution (R∼35-39) J-band (1.12-1.35 microns) spectrum of the planet. We find that the planet has passed the quadrature. We constrain its semi-major axis to ≤10 AU (90 % prob.) with a peak at 8.9+0.4/-0.6 AU. The joint fit of the planet astrometry and the most recent radial velocity measurements of the star yields a planet's dynamical mass lower then 20 MJup (greater than 96 % prob.). The extracted spectrum of Beta Pic b is similar to those of young L1-1.5/+1 dwarfs. We use the spectral type estimate to revise the planet luminosity to log(L/Lsun)=-3.90±0.07. The 0.9-4.8 microns photometry and spectrum are reproduced for T eff=1650±150 K and a log g lower than 4.7 dex by 12 grids of PHOENIX-based and LESIA atmospheric models. If we adopt the most recent system age estimate (21±4 Myr), the bolometric luminosity and the constraints on the dynamical mass of Beta Pic b are only reproduced by warm- and hot-start tracks with initial entropies Si greater than 10.5 kB/baryon. Such initial conditions may result from an inefficient accretion shock and/or a planetesimal density at formation higher than in the classical core accretion model. Considering a younger age for the system or a conservative formation time for Beta Pic b does not change these conclusions.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2014. ESOen
dc.subjectTechniques: photometricen
dc.subjectTechniques: spectroscopicen
dc.subjectPlanetary systemsen
dc.subjectStars: individual: Beta-Picen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titlePhysical and orbital properties of Beta Pictoris ben
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.description.statusPeer revieweden

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