Please use this identifier to cite or link to this item: http://elar.urfu.ru/handle/10995/90209
Title: Discovery of a brown dwarf companion to the star HIP 64892
Authors: Cheetham, A.
Bonnefoy, M.
Desidera, S.
Langlois, M.
Vigan, A.
Schmidt, T.
Olofsson, J.
Chauvin, G.
Klahr, H.
Gratton, R.
D'Orazi, V.
Henning, T.
Janson, M.
Biller, B.
Peretti, S.
Hagelberg, J.
Ségransan, D.
Udry, S.
Mesa, D.
Sissa, E.
Kral, Q.
Schlieder, J.
Maire, A. -L.
Mordasini, C.
Menard, F.
Zurlo, A.
Beuzit, J. -L.
Feldt, M.
Mouillet, D.
Meyer, M.
Lagrange, A. -M.
Boccaletti, A.
Keppler, M.
Kopytova, T.
Ligi, R.
Rouan, D.
Le, Coroller, H.
Dominik, C.
Lagadec, E.
Turatto, M.
Abe, L.
Antichi, J.
Baruffolo, A.
Baudoz, P.
Blanchard, P.
Buey, T.
Carbillet, M.
Carle, M.
Cascone, E.
Claudi, R.
Costille, A.
Delboulbé, A.
De, Caprio, V.
Dohlen, K.
Fantinel, D.
Feautrier, P.
Fusco, T.
Giro, E.
Gluck, L.
Hubin, N.
Hugot, E.
Jaquet, M.
Kasper, M.
Llored, M.
Madec, F.
Magnard, Y.
Martinez, P.
Maurel, D.
Le, Mignant, D.
Möller-Nilsson, O.
Moulin, T.
Origné, A.
Pavlov, A.
Perret, D.
Petit, C.
Pragt, J.
Puget, P.
Rabou, P.
Ramos, J.
Rigal, F.
Rochat, S.
Roelfsema, R.
Rousset, G.
Roux, A.
Salasnich, B.
Sauvage, J. -F.
Sevin, A.
Soenke, C.
Stadler, E.
Suarez, M.
Weber, L.
Wildi, F.
Issue Date: 2018
Publisher: EDP Sciences
Citation: Discovery of a brown dwarf companion to the star HIP 64892 / A. Cheetham, M. Bonnefoy, S. Desidera, M. Langlois, et al. . — DOI 10.1051/0004-6361/201832650 // Astronomy and Astrophysics. — 2018. — Iss. 615. — A160.
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion (1.2705 ± 0.0023”) corresponds to a projected distance of 159 ± 12 AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its spectral energy distribution (SED) and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (<30 Myr), low surface gravity object with a spectral type of M9γ ± 1. From comparison with the BT-Settl atmospheric models we estimate an effective temperature of Teff = 2600 ± 100 K, and comparison of the companion photometry to the COND evolutionary models yields a mass of ∼29−37 MJ at the estimated age of 16+−157 Myr for the system. The star HIP 64892 is a rare example of an extreme-mass ratio system (q ∼ 0.01) and will be useful for testing models relating to the formation and evolution of such low-mass objects. © ESO 2018
Keywords: BROWN DWARFS
PLANETS
PLANETS AND SATELLITES: DETECTION
SATELLITES: ATMOSPHERES
STARS: INDIVIDUAL: HIP 64892
TECHNIQUES: HIGH ANGULAR RESOLUTION
PLANETS
SATELLITES
BROWN DWARFS
EFFECTIVE TEMPERATURE
EVOLUTIONARY MODELS
FORMATION AND EVOLUTIONS
PLANETS AND SATELLITES: DETECTIONS
SPECTRAL ENERGY DISTRIBUTION
STARS: INDIVIDUAL
TECHNIQUES: HIGH ANGULAR RESOLUTIONS
STARS
URI: http://elar.urfu.ru/handle/10995/90209
Access: info:eu-repo/semantics/openAccess
RSCI ID: 38634788
SCOPUS ID: 85055139238
WOS ID: 000440420500001
PURE ID: 7777957
ISSN: 0004-6361
DOI: 10.1051/0004-6361/201832650
metadata.dc.description.sponsorship: Ministerio de Ciencia e Innovación, MICINN
Science and Technology Facilities Council, STFC
National Science Foundation, NSF
National Aeronautics and Space Administration, NASA
ANR10 LABX56
Seventh Framework Programme, FP7: 312430, 2009-2012
Ministerio de Ciencia e Innovación, MICINN: AyA2011-24052
Istituto Nazionale di Astrofisica, INAF
RII3-Ct-2004-001566 for FP6 (2004-2008, 226604
Institut de Cardiologie de Montréal, ICM
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, SNSF
Science and Technology Facilities Council, STFC
Nova
National Centre of Competence in Research Robotics
Centre National de la Recherche Scientifique, CNRS
tive temperature for young objects with low surfaHR8799bce gravity from Labex OSUG@2020 (Investissements d’avenir – ANR10 LABX56). This publi- HR8799c Filippazzo et al. (2015), our spectral type constraints correspond cise distance measurement will come from theHR8799eGAIA parallax, itsoaajnoinetfpferocjteicvteoftethme pUenrivaetrusritey ooff MTefasfsa=ch2us6e0tt0s a±nd3t0h0e IKnf.rared Processing From the flux-calibrated LSS spectrum, we derived a syn-thetic absolute magnitude of MJ,2MASS = 9.37 ± 0.15 mag. Com- This publication makes use of VOSA,Kde1ve-lKop2edAurntdicelrethneumSpbaenri,shpaVgiretu7aloOf b1-2 servbiningatorytprojecthis witsupportedh the spectrfromthealSpanishtype ofMICINNM9 ±through1, wegrantcanAuseyA20t1he1- 2b4o0l5o2m. etric correction relations from Filippazzo et al. (2015) to Fig. 9. Colour-magnitude diagram comparing K1 absolute magnitudes R. G., R. C., S. D. acknowledge support from the “Progetti⊙ Premiali” funding and K1-K2 colours of a range of low-mass stellar and substellar ob- scheme of the Italian Ministry of Education, University, and Research. jects from the literature. Synthetic K1 and K2 fluxes were computed J. O. acknowledges financial support from ICM Núcleo Milenio de Formación fordictedeachtarKgS,e2tMfAroSmS absolutepublishedmagnispectra.tudeAnumberusing tofheyoungSpeXandspectrdustyum Planetaria, NPF. coQofm.pKTa.nWaicoAknnso2wo7Ablesdegrasevsefdanunwdianalog.itnhgSfrPoHmESTheRTEFCorrvesultingwiaitthhepIunbstvliitasulhtueeedofofKA-sbMtaronKndso,m2sMpye,AcCStrSaam=- wbe8rr.ie0dga2ed±dCeod0n.st1ool7itdhmaeteaddgiaGgcrraoanrmtr.e. sHpIoPn6d4s89t2oBafallulsmininaossiimtyilaorflolcoagti(oLn/tLo⊙P)Z= Te−l 2B.5a1nd±H0I.P1178d5e3x0Bu,sibnogththyeousnagmberomwenthdowda.rfs with late-M spectral types.We also compared the observed spectrum to the BT-Settl model grid (Baraffe et al. 2015) as a function of Teff, log g, and References radius R. We find a best-fit temperature and radius of Teff = work for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012), and grant number by the COND models for a 33 M object with an age of 16 Myr. Baehr, H., Klahr, H., & Kratter, K. M. 2017, ApJ, 848, 40 ThWis ewfoirnkdhtahsamt tahdee luoseggofvtahleuSePiHsEpRoEorDlyatcaoCnesnttrraei,njeodin,tlwy iotpheraatbedesbt-yfit Baraffe, I., Chabrier, G., Barman, T. S., Allard, F., & Hauschildt, P. H. 2003, OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), and Observatoire de Paris/LESIA (Paris) and supported by a grant from Labex OSUG@2020 (Investissements d’avenir – ANR10 LABX56). This publi- tures are generally narrow and fitting to the entire spectrum at Béjar, V. J. S., Zapatero Osorio, M. R., Pérez-Garrido, A., et al. 2008, ApJ, 673, is oa njocient mproajyecct oofmthpeliUcnaitveertshitiysomf Meaasssuarcehmuseetntst.anTdothienIvnefsratriegdatPerotcheisssi,nwg e L185 and Analysis Center/California Institute of Technology, funded by the National
Beiothhlienr, sRi.dCe. o20f0t7h,ein1A.4strµomnomteicllaul rSioccifeetyatoufretheinPdaicvifiidc uCaolnlfye.reTnhceeSYer–ieJs-, This publication makes use of VOSA, developed under the Spanish Virtual Ob-servatory project supported from the Spanish MICINN through grant AyA2011-24H05-2b. and spectrum yields log g = 3.5 ± 1.0, indicating that a lower Bonnefoy, M., Chauvin, G., Lagrange, A.-M., et al. 2014a, A&A, 562, A127 R. G., R. C., S. D. acknowledge support from the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research. Planetaria,NPF.J.O.acknowledgesfinancialsupportfromICMNúcleoMilenioA160de, pFaormaciónge 7 of 10
Q. K. acknowledges funding from STFC via the Institute of Astronomy, Cam-bridge Consolidated Grant.
Acknowledgements. This work has been carried out within the frame of the National Centre for Competence in Research “PlanetS” supported by the Swiss National Science Foundation (SNSF). SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Lab-oratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Obser-vatoire Astronomique de l’Université de Genève (Switzerland), ETH Zurich (Switzerland), NOVA (The Netherlands), ONERA (France), and ASTRON (The Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland), and NOVA (The Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Frame-work Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012), and grant number 312430 for FP7 (2013-2016). This work has made use of the SPHERE Data Centre, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), and Observatoire de Paris/LESIA (Paris) and supported by a grant from Labex OSUG@2020 (Investissements d’avenir – ANR10 LABX56). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported from the Spanish MICINN through grant AyA2011-24052. R.G., R.C., S.D. acknowledge support from the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research. J.O. acknowledges financial support from ICM Núcleo Milenio de Formación Planetaria, NPF. Q.K. acknowledges funding from STFC via the Institute of Astronomy, Cambridge Consolidated Grant.
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