Discovery of a warm, dusty giant planet around HIP 65426

Chauvin, G.G.ChauvinDESIDERA, SilvanoSilvanoDESIDERALagrange, A. -M.A. -M.LagrangeVigan, A.A.ViganGRATTON, RaffaeleRaffaeleGRATTONLanglois, M.M.LangloisBonnefoy, M.M.BonnefoyBeuzit, J. -L.J. -L.BeuzitFeldt, M.M.FeldtMouillet, D.D.MouilletMeyer, M.M.MeyerCheetham, A.A.CheethamBiller, B.B.BillerBoccaletti, A.A.BoccalettiD'Orazi, V.V.D'OraziGalicher, R.R.GalicherHagelberg, J.J.HagelbergMaire, A. -L.A. -L.MaireMESA, DINODINOMESAOlofsson, J.J.OlofssonSamland, M.M.SamlandSchmidt, T. O. B.T. O. B.SchmidtSissa, E.E.SissaBonavita, M.M.BonavitaCharnay, B.B.CharnayCudel, M.M.CudelDaemgen, S.S.DaemgenDelorme, P.P.DelormeJanin-Potiron, P.P.Janin-PotironJanson, M.M.JansonKeppler, M.M.KepplerLe Coroller, H.H.Le CorollerLIGI, ROXANNEROXANNELIGIMarleau, G. D.G. D.MarleauMESSINA, SergioSergioMESSINAMollière, P.P.MollièreMordasini, C.C.MordasiniMüller, A.A.MüllerPeretti, S.S.PerettiPerrot, C.C.PerrotRodet, L.L.RodetRouan, D.D.RouanZurlo, A.A.ZurloDominik, C.C.DominikHenning, T.T.HenningMenard, F.F.MenardSchmid, H. -M.H. -M.SchmidTURATTO, MassimoMassimoTURATTOUdry, S.S.UdryVakili, F.F.VakiliAbe, L.L.AbeAntichi, J.J.AntichiBARUFFOLO, AndreaAndreaBARUFFOLOBaudoz, P.P.BaudozBaudrand, J.J.BaudrandBlanchard, P.P.BlanchardBazzon, A.A.BazzonBuey, T.T.BueyCarbillet, M.M.CarbilletCarle, M.M.CarleCharton, J.J.ChartonCASCONE, EnricoEnricoCASCONECLAUDI, RiccardoRiccardoCLAUDICostille, A.A.CostilleDeboulbe, A.A.DeboulbeDe Caprio, V.V.De CaprioDohlen, K.K.DohlenFANTINEL, DanielaDanielaFANTINELFeautrier, P.P.FeautrierFusco, T.T.FuscoGigan, P.P.GiganGIRO, EnricoEnricoGIROGisler, D.D.GislerGluck, L.L.GluckHubin, N.N.HubinHugot, E.E.HugotJaquet, M.M.JaquetKasper, M.M.KasperMadec, F.F.MadecMagnard, Y.Y.MagnardMartinez, P.P.MartinezMaurel, D.D.MaurelLe Mignant, D.D.Le MignantMöller-Nilsson, O.O.Möller-NilssonLlored, M.M.LloredMoulin, T.T.MoulinOrigné, A.A.OrignéPavlov, A.A.PavlovPerret, D.D.PerretPetit, C.C.PetitPragt, J.J.PragtPuget, P.P.PugetRabou, P.P.RabouRamos, J.J.RamosRigal, R.R.RigalRochat, S.S.RochatRoelfsema, R.R.RoelfsemaRousset, G.G.RoussetRoux, A.A.RouxSALASNICH, BernardoBernardoSALASNICHSauvage, J. -F.J. -F.SauvageSevin, A.A.SevinSoenke, C.C.SoenkeStadler, E.E.StadlerSuarez, M.M.SuarezWeber, L.L.WeberWildi, F.F.WildiANTONIUCCI, SimoneSimoneANTONIUCCIAugereau, J. -C.J. -C.AugereauBaudino, J. -L.J. -L.BaudinoBrandner, W.W.BrandnerEngler, N.N.EnglerGirard, J.J.GirardGry, C.C.GryKral, Q.Q.KralKopytova, T.T.KopytovaLagadec, E.E.LagadecMilli, J.J.MilliMoutou, C.C.MoutouSchlieder, J.J.SchliederSzulágyi, J.J.SzulágyiThalmann, C.C.ThalmannWahhaj, Z.Z.Wahhaj2020-11-202020-11-2020170004-6361http://hdl.handle.net/20.500.12386/28462Aims: The SHINE program is a high-contrast near-infrared survey of 600 young, nearby stars aimed at searching for and characterizing new planetary systems using VLT/SPHERE's unprecedented high-contrast and high-angular-resolution imaging capabilities. It is also intended to place statistical constraints on the rate, mass and orbital distributions of the giant planet population at large orbits as a function of the stellar host mass and age to test planet-formation theories. Methods: We used the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE to acquire high-contrast coronagraphic differential near-infrared images and spectra of the young A2 star HIP 65426. It is a member of the 17 Myr old Lower Centaurus-Crux association. Results: At a separation of 830 mas (92 au projected) from the star, we detect a faint red companion. Multi-epoch observations confirm that it shares common proper motion with HIP 65426. Spectro-photometric measurements extracted with IFS and IRDIS between 0.95 and 2.2 μm indicate a warm, dusty atmosphere characteristic of young low-surface-gravity L5-L7 dwarfs. Hot-start evolutionary models predict a luminosity consistent with a 6-12 MJup, Teff = 1300-1600 K and R = 1.5 ± 0.1 RJup giant planet. Finally, the comparison with Exo-REM and PHOENIX BT-Settl synthetic atmosphere models gives consistent effective temperatures but with slightly higher surface gravity solutions of log (g) = 4.0-5.0 with smaller radii (1.0-1.3 RJup). Conclusions: Given its physical and spectral properties, HIP 65426 b occupies a rather unique placement in terms of age, mass, and spectral-type among the currently known imaged planets. It represents a particularly interesting case to study the presence of clouds as a function of particle size, composition, and location in the atmosphere, to search for signatures of non-equilibrium chemistry, and finally to test the theory of planet formation and evolution. Based on observations collected at La Silla and Paranal Observatory, ESO (Chile) Program ID: 097.C-0865 and 098.C-0209 (SPHERE).The planet spectrum is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/605/L9">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/605/L9STAMPAenDiscovery of a warm, dusty giant planet around HIP 65426Article10.1051/0004-6361/2017311522-s2.0-85029689672000412231200011https://www.aanda.org/articles/aa/abs/2017/09/aa31152-17/aa31152-17.html2017A&A...605L...9CFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation