The SPHERE infrared survey for exoplanets (SHINE). III. The demographics of young giant exoplanets below 300 au with SPHERE
Creators: name: Vigan, A.
name: Fontanive, C.
name: Meyer, M.
name: Biller, B.
name: Bonavita, M.
name: Feldt, M.
name: Desidera, S.
name: Marleau, G. -D.
name: Emsenhuber, A.
name: Galicher, R.
name: Rice, K.
name: Forgan, D.
name: Mordasini, C.
name: Gratton, R.
name: Coroller, H. Le
name: Maire, A. -L.
name: Cantalloube, F.
name: Chauvin, G.
name: Cheetham, A.
name: Hagelberg, J.
name: Lagrange, A. -M.
name: Langlois, M.
name: Bonnefoy, M.
name: Beuzit, J. -L.
name: Boccaletti, A.
name: D'Orazi, V.
name: Delorme, P.
name: Dominik, C.
name: Henning, Th.
name: Janson, M.
name: Lagadec, E.
name: Lazzoni, C.
name: Ligi, R.
name: Menard, F.
name: Mesa, D.
name: Messina, S.
name: Moutou, C.
name: Müller, A.
name: Perrot, C.
name: Samland, M.
name: Schmid, H. M.
name: Schmidt, T.
name: Sissa, E.
name: Turatto, M.
name: Udry, S.
name: Zurlo, A.
name: Abe, L.
name: Antichi, J.
name: Asensio-Torres, R.
name: Baruffolo, A.
name: Baudoz, P.
name: Baudrand, J.
name: Bazzon, A.
name: Blanchard, P.
name: Bohn, A. J.
name: Sevilla, S. Brown
name: Carbillet, M.
name: Carle, M.
name: Cascone, E.
name: Charton, J.
name: Claudi, R.
name: Costille, A.
name: De Caprio, V.
name: Delboulbé, A.
name: Dohlen, K.
name: Engler, N.
name: Fantinel, D.
name: Feautrier, P.
name: Fusco, T.
name: Gigan, P.
name: Girard, J. H.
name: Giro, E.
name: Gisler, D.
name: Gluck, L.
name: Gry, C.
name: Hubin, N.
name: Hugot, E.
name: Jaquet, M.
name: Kasper, M.
name: Mignant, D. Le
name: Llored, M.
name: Madec, F.
name: Magnard, Y.
name: Martinez, P.
name: Maurel, D.
name: Möller-Nilsson, O.
name: Mouillet, D.
name: Moulin, T.
name: Origné, A.
name: Pavlov, A.
name: Perret, D.
name: Petit, C.
name: Pragt, J.
name: Puget, P.
name: Rabou, P.
name: Ramos, J.
name: Rickman, E. L.
name: Rigal, F.
name: Rochat, S.
name: Roelfsema, R.
name: Rousset, G.
name: Roux, A.
name: Salasnich, B.
name: Sauvage, J. -F.
name: Sevin, A.
name: Soenke, C.
name: Stadler, E.
name: Suarez, M.
name: Wahhaj, Z.
name: Weber, L.
name: Wildi, F.
Publisher: name: arXiv
Year: 2020
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The SHINE project is a 500-star survey performed with SPHERE on the VLT 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 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. 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 MCMC 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.
description: 24 pages, 14 figures, 3 tables. Accepted for publication in A&amp;A