The SPHERE infrared survey for exoplanets (SHINE)

A Vigan ,J L Beuzit ,D Mesa ,V D’orazi ,M Turatto ,D Le Mignant ,Duncan Forgan ,Cyril Petit ,C Fontanive ,S Rochat ,Markus Janson ,Y Magnard ,M Jaquet ,R Roelfsema ,Beth Biller ,E Sissa ,André Müller ,M Feldt ,A L Maire ,D Perret ,N Hubin ,A J Bohn ,C Perrot ,C Lazzoni ,J Ramos ,K Døhlen ,A Roux ,A Zurlo ,J Charton ,Lyu Abe ,M Bonavita ,D Gisler ,O Möller-Nilsson ,Pierre Baudoz ,T O B Schmidt ,C Soenke ,S Brown Sevilla ,D Fantinel ,A Bazzon ,H M Schmid ,Th Henning ,Ken Rice ,C Moutou ,E Cascone ,L Glück ,J Baudrand ,R G Gratton ,A.-M Lagrange ,M Suárez ,R Galicher ,Rubén Asensio-Torres ,Vincenzo De Caprio ,J Pragt ,E Rickman ,J Antichi ,A Baruffolo ,F Cantalloube ,Arnaud Sevin ,S Udry ,P Puget ,R Claudi ,C Gry ,Bernardo Salasnich ,S Messina ,T Moulin ,P Gigan ,Eric Stadler ,L Weber ,M Langlois ,F Ménard ,M Llored ,H Le Coroller ,M Bonnefoy ,Marcel Carbillet ,C Dominik ,Patrick Rabou ,Thierry Fusco ,Philippe Feautrier ,S Desidera ,J Girard ,A Costille ,J.-F Sauvage ,D Mouillet ,P Martínez ,F Rigal ,E Lagadec ,G Chauvin ,F Madec ,Z Wahhaj ,G Rousset ,D Maurel ,Emmanuel Hugot ,Gabriel-Dominique Marleau ,A Pavlov ,Markus Kasper ,A Origné ,J Hagelberg ,P Blanchard ,N Engler ,P Delorme ,Michael Meyer ,Alexandre Emsenhuber ,M Carle ,E Giro ,M Samland ,R Ligi ,A Boccaletti ,A Cheetham ,Christoph Mordasini ,A Delboulbé ,F Wildi

doi:10.1051/0004-6361/202038107

Abstract

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. 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. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. 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. 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. 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. 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. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1–75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using 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. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies.

Highlights

In the past 20 yr, large-scale direct-imaging surveys for exoplanets have discovered approximately 60 substellar and planetarymass companions around young nearby stars
In this paper we present a first statistical analysis of the properties of the population of 1–75 MJup companions at orbital separations from 5–300 au based on the first 150 stars observed in the SpHere INfrared Exoplanet (SHINE) survey
Comparison to previous works The SHINE survey is certainly one of the deepest, and it is one of the first to open the low-mass regime at semimajor axes 5–50 au. This enables us to obtain quantitative statistical constraints in that range. It offers some overlap with the parameter space that has been explored by previous works, which have placed strong statistical constraints on the population of young giant planets on wide orbits

Summary

Introduction

In the past 20 yr, large-scale direct-imaging surveys for exoplanets have discovered approximately 60 substellar and planetarymass companions around young nearby stars (see, e.g., Wagner et al 2019). SHINE and GPIES have added three new exoplanet detections to the growing cohort of directly imaged objects (Macintosh et al 2015; Chauvin et al 2017; Keppler et al 2018) and several additional higher mass brown dwarfs (Konopacky et al 2016; Cheetham et al 2018). New exoplanet detections are just one goal of largescale direct-imaging surveys. These surveys provide key spectral and orbital characterization data for known exoplanets (e.g., De Rosa et al 2016; Samland et al 2017; Chauvin et al 2018; Wang et al 2018; Müller et al 2018; Cheetham et al 2019; Lagrange et al 2019; Maire et al 2019), and statistical constraints

Objectives

Results

Discussion

Conclusion