New binaries from the SHINE survey^⋆,⋆⋆

¹ INAF – Osservatorio Astronomico di Padova, Vicolo della Osservatorio 5, 35122 Padova, Italy
e-mail: mbonavit@ed.ac.uk
² Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
³ Institute for Astronomy, University of Edinburgh, EH9 3HJ Edinburgh, UK
⁴ Universitá degli studi di Padova, Dipartimento di Fisica ed Astronomia “Galileo Galilei”, Via G. Marzolo, 8, 35131 Padova, Italy
⁵ Núcleo de Astronomía, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile
⁶ Escuela de Ingeniería Industrial, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile
⁷ Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
⁸ Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
⁹ Department of Astronomy, Stockholm University, 10691 Stockholm, Sweden
¹⁰ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
¹¹ Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMI 3386 and Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
¹² Geneva Observatory, University of Geneva, Chemin Pegasi 51, 1290 Versoix, Switzerland
¹³ CRAL, CNRS, Université Lyon 1,Université de Lyon, ENS, 9 avenue Charles Andre, 69561 Saint Genis Laval, France
¹⁴ LESIA, Observatoire de Paris, Université PSL, Université de Paris, CNRS, Sorbonne Université, 5 place Jules Janssen, 92195 Meudon, France
¹⁵ Anton Pannekoek Institute for Astronomy, Science Park 9, 1098 XH Amsterdam, The Netherlands
¹⁶ Center for Space and Habitability, University of Bern, 3012 Bern, Switzerland
¹⁷ Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
¹⁸ Institute for Particle Physics and Astrophysics, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland
¹⁹ STAR Institute, University of Liège, Allée du Six Août 19c, 4000 Liège, Belgium
²⁰ INAF – Catania Astrophysical Observatory, Via S. Sofia 78, 95123 Catania, Italy
²¹ Univ. de Toulouse, CNRS, IRAP, 14 avenue Belin, 31400 Toulouse, France
²² European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching, German
²³ Université Côte d’Azur, OCA, CNRS, Lagrange, France
²⁴ Leiden Observatory, Leiden University, PO Box 9513 2300 RA Leiden, The Netherlands
²⁵ INAF – Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, Italy
²⁶ European Southern Observatory, Alonso de Còrdova 3107, Vitacura, Casilla, 19001 Santiago, Chile
²⁷ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
²⁸ Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile
²⁹ NOVA/UVA, Northern Virginia, USA
³⁰ European Space Agency (ESA), ESA Office, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
³¹ INAF – Osservatorio Astrofisico di Arcetri, Florence, Italy

Received: 6 February 2021
Accepted: 24 March 2021

Abstract

We present the multiple stellar systems observed within the SpHere INfrared survey for Exoplanet (SHINE). SHINE searched for sub-stellar companions to young stars using high contrast imaging. Although stars with known stellar companions within the SPHERE field of view (< 5.5 arcsec) were removed from the original target list, we detected additional stellar companions to 78 of the 463 SHINE targets observed so far. Twenty-seven per cent of the systems have three or more components. Given the heterogeneity of the sample in terms of observing conditions and strategy, tailored routines were used for data reduction and analysis, some of which were specifically designed for these datasets. We then combined SPHERE data with literature and archival data, TESS light curves, and Gaia parallaxes and proper motions for an accurate characterisation of the systems. Combining all data, we were able to constrain the orbits of 25 systems. We carefully assessed the completeness of our sample for separations between 50–500 mas (corresponding to periods of a few years to a few decades), taking into account the initial selection biases and recovering part of the systems excluded from the original list due to their multiplicity. This allowed us to compare the binary frequency for our sample with previous studies and highlight interesting trends in the mass ratio and period distribution. We also found that, when such an estimate was possible, the values of the masses derived from dynamical arguments were in good agreement with the model predictions. Stellar and orbital spins appear fairly well aligned for the 12 stars that have enough data, which favours a disk fragmentation origin. Our results highlight the importance of combining different techniques when tackling complex problems such as the formation of binaries and show how large samples can be useful for more than one purpose.