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Orbiting a Binary SPHERE Characterisation of the HD 284149 System?

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Orbiting a Binary SPHERE Characterisation of the HD 284149 System? A&A 608, A106 (2017) Astronomy DOI: 10.1051/0004-6361/201731003 & c ESO 2017 Astrophysics Orbiting a binary SPHERE characterisation of the HD 284149 system? M. Bonavita1; 2, V. D’Orazi1, D. Mesa1, C. Fontanive2, S. Desidera1, S. Messina4, S. Daemgen3, R. Gratton1, A. Vigan5, M. Bonnefoy7, A. Zurlo5; 20, J. Antichi13; 1, H. Avenhaus3; 6; 16, A. Baruffolo1, J. L. Baudino19, J. L. Beuzit7, A. Boccaletti10, P. Bruno4, T. Buey10, M. Carbillet20, E. Cascone14, G. Chauvin7, R. U. Claudi1, V. De Caprio14, D. Fantinel1, G. Farisato1, M. Feldt6, R. Galicher10, E. Giro1, C. Gry5, J. Hagelberg7, S. Incorvaia15, M. Janson6; 9, M. Jaquet5, A. M. Lagrange7, M. Langlois5, J. Lannier7, H. Le Coroller5, L. Lessio1, R. Ligi5, A. L. Maire6, M. Meyer3; 18, F. Menard7; 8, C. Perrot10, S. Peretti12, C. Petit11, J. Ramos6, A. Roux7, B. Salasnich1, G. Salter5, M. Samland6, S. Scuderi4, J. Schlieder6; 17, M. Surez11, M. Turatto1, and L. Weber12 1 INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 2 Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK 3 Institute for Astronomy, ETH Zurich, Wolfgang-Pauli Strasse 27, 8093 Zurich, Switzerland 4 INAF–Osservatorio Astronomico di Catania, via Santa Sofia, 78 Catania, Italy 5 Aix Marseille Univ., CNRS, LAM, Laboratoire d’Astrophysique de Marseille, 13013 Marseille, France 6 Max-Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 7 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France 8 European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 9 Department of Astronomy, Stockholm University, AlbaNova University Center, 106 91 Stockholm, Sweden 10 LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 75013 Paris, France 11 ONERA (Office National d’Études et de Recherches Aérospatiales), BP 72, 92322 Châtillon, France 12 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland 13 INAF–Osservatorio Astrofisico di Arcetri, L.go E. Fermi 5, 50125 Firenze, Italy 14 INAF–Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 15 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, via E. Bassini 15, 20133 Milano, Italy 16 Universidad de Chile, Camino el Observatorio, 1515 Santiago, Chile 17 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 18 Department of Astronomy, University of Michigan, 1085 S. University, Ann Arbor, MI 48109, USA 19 Department of Physics, University of Oxford, Parks Rd, Oxford OX1 3PU, UK 20 Núcleo de Astronomía, Facultad de Ingeniería, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile Received 13 April 2017 / Accepted 18 July 2017 ABSTRACT Aims. In this paper we present the results of the SPHERE observation of the HD 284149 system, aimed at a more detailed characteri- sation of both the primary and its brown dwarf companion. Methods. We observed HD 284149 in the near-infrared with SPHERE, using the imaging mode (IRDIS+IFS) and the long-slit spectroscopy mode (IRDIS-LSS). The data were reduced using the dedicated SPHERE pipeline, and algorithms such as PCA and TLOCI were applied to reduce the speckle pattern. 00 Results. The IFS images revealed a previously unknown low-mass (∼0.16 M ) stellar companion (HD 294149 B) at ∼0.1 , compatible with previously observed radial velocity differences, as well as proper motion differences between Gaia and Tycho-2 measurements. The known brown dwarf companion (HD 284149 b) is clearly visible in the IRDIS images. This allowed us to refine both its pho- tometry and astrometry. The analysis of the medium resolution IRDIS long slit spectra also allowed a refinement of temperature and spectral type estimates. A full reassessment of the age and distance of the system was also performed, leading to more precise values of both mass and semi-major axis. Conclusions. As a result of this study, HD 284149 ABb therefore becomes the latest addition to the (short) list of brown dwarfs on wide circumbinary orbits, providing new evidence to support recent claims that object in such configuration occur with a similar frequency to wide companions to single stars. Key words. stars: individual: HD 284149 – brown dwarfs – binaries: visual – stars: rotation – techniques: high angular resolution ? The reduced spectrum is 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/qcat?J/A+A/608/A106 Article published by EDP Sciences A106, page 1 of 15 A&A 608, A106 (2017) 1. Introduction region (Daemgen et al. 2015). Together with several other tar- gets of the same survey, HD 284149 has been proposed to be Several new sub-stellar companions to nearby young stars have part of the so-called Taurus-Ext association (Luhman et al. 2017; been directly imaged in the last decade, spanning a wide range Kraus et al. 2017; Daemgen et al. 2015), a group of stars with of masses and separations (see e.g. Chauvin et al. 2005a,b; similar space position and kinematics of the Taurus star forming Marois et al. 2008, 2010; Lagrange et al. 2010; Biller et al. region but distinctly older ages. A dedicated age estimate was 2010; Carson et al. 2013; Delorme et al. 2013; Rameau et al. then performed for HD 284149 by Bonavita et al.(2014), using 2013; Bailey et al. 2014; Bonavita et al. 2014; Gauza et al. 2015; +25 several youth indicators, leading to an adopted age of 25−10 Myr. Stone et al. 2016; Wagner et al. 2016). These objects, some They therefore finally estimated the mass of HD 284149 b to be of which have masses near and below 15MJup (see e.g. +18 32−14 MJup. From the available photometry they were able to in- Marois et al. 2008, 2010; Lagrange et al. 2010; Rameau et al. fer a spectral type between M8 and L1 and an effective tem- 2013; Bailey et al. 2014; Currie et al. 2014; Macintosh et al. +95 perature of 2537−182 K, but no spectroscopic characterisation 2015; Naud et al. 2014; Artigau et al. 2015; Bowler et al. 2017), has been performed up to now, leaving these estimates highly may represent the bottom end of the stellar companion mass uncertain. function as well as the top end of the planet population, Here we present the result of the observations of HD 284149 though both scenarios pose challenges to conventional formation performed with SPHERE, aimed at a precise characterisation of models. the whole system. Section 2 contains a detailed description of On one hand, the binary star formation process (e.g. the observations and data reduction while an update to the stel- Bate et al. 2003) rarely predicts such low mass ratios. On the lar characteristics given the new information available, includ- other hand, the standard core accretion model would struggle to ing those coming from the Gaia mission, is given in Sect. 3. The form super-Jupiter planets at >50 AU. Even though the alter- results are described and discussed in Sect. 4 and include the native gravitational instability (GI) model might become more description of a newly discovered close stellar companion, an plausible at large separations (see Meru & Bate 2010), espe- update of the astrometry of the known wide brown dwarf com- cially around more massive stars with larger disks, it is still panion and the comparison with the models of the medium res- unclear whether or not such an hypothesis is correct (see e.g. olution spectra obtained with the IRDIS LSS mode. Janson et al. 2012). Some of the most recent GI models (see e.g. Forgan & Rice 2013; Forgan et al. 2015) seem to suggest that the most likely 2. Observations and data reduction outcome of such formation process is a large fraction of rela- HD 284149 was observed with SPHERE in IRDIFS mode on tively massive objects at large semi-major axis. Such a popula- 2015-10-25 and with IRDIFS_EXT mode on 2015-11-27 as part tion would be easily detectable with direct imaging, and the lack of the SpHere INfrared survey for Exoplanet (SHINE) GTO of detections can be used to place strong constraints on how fre- campaign. The second epoch observations were taken without quently disk fragmentation occurs (see e.g. Vigan et al. 2017). coronagraph to confirm a faint candidate that was imaged for the An in-depth characterisation of the few known members of first time very close to the edge of the coronagraphic mask in the this population is therefore highly desirable, but the lack of first observation. In order to take full advantage of the angular multi-wavelength spectroscopy and photometry make precise differential imaging technique (ADI, see Marois et al. 2006a), characterisation of these systems quite challenging, leading to for both epochs the target was observed in pupil-stabilised mode poorly constrained values of some fundamental properties such to allow the rotation of the field of view. The reduction of as mass, radius and effective temperature. New dedicated instru- all the IRDIS and IFS data sets was performed through the ments, which allow both precise multi band photometry and low SPHERE Data Center (DC) using the SPHERE Data Reduction and medium resolution spectroscopy, are now becoming avail- and Handling (DRH) automated pipeline (Pavlov et al. 2008). able and allow a better characterisation of low mass companions. In the case of the IFS data, the DRH pipeline is complemented SPHERE (Beuzit et al. 2008), the new planet finder mounted at with additional routines that allow for an improved wavelength the VLT, is one of those. calibration as well as for a correction of both coherent and in- SPHERE includes three scientific modules: IFS (Claudi et al.
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