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The Gemini Planet Imager Exoplanet Survey : giant planet and brown dwarf demographics from 10 to 100 au
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dc.contributor.author | Nielsen, Eric L. | |
dc.contributor.author | De Rosa, Robert J. | |
dc.contributor.author | Macintosh, Bruce | |
dc.contributor.author | Wang, Jason J. | |
dc.contributor.author | Ruffio, Jean-Baptiste | |
dc.contributor.author | Chiang, Eugene | |
dc.contributor.author | Marley, Mark S. | |
dc.contributor.author | Saumon, Didier | |
dc.contributor.author | Savransky, Dmitry | |
dc.contributor.author | Ammons, S. Mark | |
dc.contributor.author | Bailey, Vanessa P. | |
dc.contributor.author | Barman, Travis | |
dc.contributor.author | Blain, Célia | |
dc.contributor.author | Bulger, Joanna | |
dc.contributor.author | Burrows, Adam | |
dc.contributor.author | Chilcote, Jeffrey | |
dc.contributor.author | Cotten, Tara | |
dc.contributor.author | Czekala, Ian | |
dc.contributor.author | Doyon, Rene | |
dc.contributor.author | Duchêne, Gaspard | |
dc.contributor.author | Esposito, Thomas M. | |
dc.contributor.author | Fabrycky, Daniel | |
dc.contributor.author | Fitzgerald, Michael P. | |
dc.contributor.author | Follette, Katherine B. | |
dc.contributor.author | Fortney, Jonathan J. | |
dc.contributor.author | Gerard, Benjamin L. | |
dc.contributor.author | Goodsell, Stephen J. | |
dc.contributor.author | Graham, James R. | |
dc.contributor.author | Greenbaum, Alexandra Z. | |
dc.contributor.author | Hibon, Pascale | |
dc.contributor.author | Hinkley, Sasha | |
dc.contributor.author | Hirsch, Lea A. | |
dc.contributor.author | Hom, Justin | |
dc.contributor.author | Hung, Li-Wei | |
dc.contributor.author | Dawson, Rebekah Ilene | |
dc.contributor.author | Ingraham, Patrick | |
dc.contributor.author | Kalas, Paul | |
dc.contributor.author | Konopacky, Quinn | |
dc.contributor.author | Larkin, James E. | |
dc.contributor.author | Lee, Eve J. | |
dc.contributor.author | Lin, Jonathan W. | |
dc.contributor.author | Maire, Jérôme | |
dc.contributor.author | Marchis, Franck | |
dc.contributor.author | Marois, Christian | |
dc.contributor.author | Metchev, Stanimir | |
dc.contributor.author | Millar-Blanchaer, Maxwell A. | |
dc.contributor.author | Morzinski, Katie M. | |
dc.contributor.author | Oppenheimer, Rebecca | |
dc.contributor.author | Palmer, David | |
dc.contributor.author | Patience, Jennifer | |
dc.contributor.author | Perrin, Marshall | |
dc.contributor.author | Poyneer, Lisa | |
dc.contributor.author | Pueyo, Laurent | |
dc.contributor.author | Rafikov, Roman R. | |
dc.contributor.author | Rajan, Abhijith | |
dc.contributor.author | Rameau, Julien | |
dc.contributor.author | Rantakyrö, Fredrik T. | |
dc.contributor.author | Ren, Bin | |
dc.contributor.author | Schneider, Adam C. | |
dc.contributor.author | Sivaramakrishnan, Anand | |
dc.contributor.author | Song, Inseok | |
dc.contributor.author | Soummer, Remi | |
dc.contributor.author | Tallis, Melisa | |
dc.contributor.author | Thomas, Sandrine | |
dc.contributor.author | Ward-Duong, Kimberly | |
dc.contributor.author | Wolff, Schuyler | |
dc.date.accessioned | 2024-02-14T16:30:05Z | |
dc.date.available | 2024-02-14T16:30:05Z | |
dc.date.issued | 2019-07-01 | |
dc.identifier | 295920721 | |
dc.identifier | 84267275-0b1d-47b6-be1e-8bb90bfc8646 | |
dc.identifier | 85071118271 | |
dc.identifier.citation | Nielsen , E L , De Rosa , R J , Macintosh , B , Wang , J J , Ruffio , J-B , Chiang , E , Marley , M S , Saumon , D , Savransky , D , Ammons , S M , Bailey , V P , Barman , T , Blain , C , Bulger , J , Burrows , A , Chilcote , J , Cotten , T , Czekala , I , Doyon , R , Duchêne , G , Esposito , T M , Fabrycky , D , Fitzgerald , M P , Follette , K B , Fortney , J J , Gerard , B L , Goodsell , S J , Graham , J R , Greenbaum , A Z , Hibon , P , Hinkley , S , Hirsch , L A , Hom , J , Hung , L-W , Dawson , R I , Ingraham , P , Kalas , P , Konopacky , Q , Larkin , J E , Lee , E J , Lin , J W , Maire , J , Marchis , F , Marois , C , Metchev , S , Millar-Blanchaer , M A , Morzinski , K M , Oppenheimer , R , Palmer , D , Patience , J , Perrin , M , Poyneer , L , Pueyo , L , Rafikov , R R , Rajan , A , Rameau , J , Rantakyrö , F T , Ren , B , Schneider , A C , Sivaramakrishnan , A , Song , I , Soummer , R , Tallis , M , Thomas , S , Ward-Duong , K & Wolff , S 2019 , ' The Gemini Planet Imager Exoplanet Survey : giant planet and brown dwarf demographics from 10 to 100 au ' , Astronomical Journal , vol. 158 , no. 1 , 13 . https://doi.org/10.3847/1538-3881/ab16e9 | en |
dc.identifier.issn | 0004-6256 | |
dc.identifier.other | BibCode: 2019AJ....158...13N | |
dc.identifier.other | ORCID: /0000-0002-1483-8811/work/146464271 | |
dc.identifier.uri | https://hdl.handle.net/10023/29240 | |
dc.description.abstract | We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M* > 1.5 M⊙ more likely to host planets with masses between 2 and 13MJup and semimajor axes of 3–100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M* > 1.5 M⊙) of the form d2N/(dm da) ∝ mα aβ, finding α = −2.4 ± 0.8 and β = −2.0 ± 0.5, and an integrated occurrence rate of 9+5-4% between 5–13MJup and 10–100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8+0.8-0.5% of stars hosting a brown dwarf companion between 13–80MJup and 10–100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ∼1 and 10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability. | |
dc.format.extent | 44 | |
dc.format.extent | 5626516 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomical Journal | en |
dc.subject | Instrumentation: adaptive optics | en |
dc.subject | Planetary systems | en |
dc.subject | Planets and satellites: detection | en |
dc.subject | QB Astronomy | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.title | The Gemini Planet Imager Exoplanet Survey : giant planet and brown dwarf demographics from 10 to 100 au | en |
dc.type | Journal article | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | 10.3847/1538-3881/ab16e9 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/1904.05358 | en |
dc.identifier.url | http://adsabs.harvard.edu/abs/2019AJ....158...13N | en |
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