1/11/2024 0 Comments Dex white pages tucsonUsing our population model and restricting our sample to FGK stars, we derive a frequency of 5.7 −2.8 +3.8%, consistent with predictions from the parametric model. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1–75 M Jup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are 23.0 −9.7 +13.5, 5.8 −2.8 +4.7, and 12.6 −7.1 +12.9% for BA, FGK, and M stars, respectively. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Based on the results obtained for each star and on the 13 detections in the sample, we use a Markov chain Monte Carlo tool to compare our observations to two different types of models. For this purpose, we adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 M Jup and semimajor axes between 5 and 300 au. Here we present an initial statistical analysis for a subsample of 150 stars spanning spectral types from B to M that are representative of the full SHINE sample. The SpHere INfrared Exoplanet (SHINE) project is a 500-star survey performed with SPHERE on the Very Large Telescope for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. NOVA Optical Infrared Instrumentation Group, Núcleo Milenio Formación Planetaria – NPF, Universidad de Valparaíso, Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, INAF – Osservatorio Astronomico di Capodimonte, Núcleo de Astronomía, Facultad de Ingeniería y Ciencias, Universidad Diego Portales,Įscuela de Ingeniería Industrial, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, INAF – Osservatorio Astronomico di Brera, Geneva Observatory, University of Geneva, ONERA (Office National dEtudes et de Recherches Arospatiales), INAF – Catania Astrophysical Observatory, STAR Institute, University of Liège, Allée du Six Août 19c,Ĭentre for Exoplanet Science, University of Edinburgh,ĭepartment of Astronomy, Stockholm University,ĬRAL, CNRS, Université Lyon 1, Université de Lyon, ENS, Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMI 3386 and Departamento de Astronomía, Universidad de Chile, LESIA, Observatoire de Paris, Université PSL, Université de Paris, CNRS, Sorbonne Université, Lunar and Planetary Laboratory, University of Arizona 1629 E. Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, University of Edinburgh,Ĭentre for Exoplanet Science, SUPA, School of Physics & Astronomy, University of St Andrews, Institute for Astronomy, University of Edinburgh, Institute for Particle Physics and Astrophysics, INAF – Osservatorio Astronomico di Padova,ĭepartment of Astronomy, University of Michigan, Wildi 23Į-mail: for Space and Habitability, University of Bern,
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