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WEIRD: Wide-orbit Exoplanet Search with InfraRed Direct Imaging

Baron, Frédérique and Artigau, Étienne and Rameau, Julien and Lafrenière, David and Gagné, Jonathan and Malo, Lison and Albert, Loïc and Naud, Marie-Eve and Doyon, René and Janson, Markus and Delorme, Philippe and Beichman, Charles (2018) WEIRD: Wide-orbit Exoplanet Search with InfraRed Direct Imaging. Astronomical Journal, 156 (3). Art. No. 137. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20180830-145509367

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Abstract

We report results from the Wide-orbit Exoplanet search with InfraRed Direct imaging, or WEIRD, a survey designed to search for Jupiter-like companions on very wide orbits (1000–5000 au) around young stars (<120 Myr) that are known members of moving groups in the solar neighborhood (<70 pc). Companions that share the same age, distance, and metallicity as their host while being on large enough orbits to be studied as "isolated" objects make prime targets for spectroscopic observations, and they are valuable benchmark objects for exoplanet atmosphere models. The search strategy is based on deep imaging in multiple bands across the near-infrared domain. For all 177 objects of our sample, z_(ab)', J, [3.6], and [4.5] images were obtained with CFHT/MegaCam, GEMINI/GMOS, CFHT/WIRCam, GEMINI/Flamingos-2, and Spitzer/IRAC. Using this set of four images per target, we searched for sources with red z_(ab)' and [3.6]–[4.5] colors, typically reaching good completeness down to 2 M_(Jup) companions, while going down to 1 M_(Jup) for some targets, at separations of 1000–5000 au. The search yielded four candidate companions with the expected colors, but they were all rejected through follow-up proper motion observations. Our results constrain the occurrence of 1–13 M_(Jup) planetary-mass companions on orbits with a semimajor axis between 1000 and 5000 au at less than 0.03, with a 95% confidence level.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/aad599DOIArticle
https://arxiv.org/abs/1807.08799arXivDiscussion Paper
ORCID:
AuthorORCID
Baron, Frédérique0000-0002-5074-1128
Artigau, Étienne0000-0003-3506-5667
Rameau, Julien0000-0003-0029-0258
Lafrenière, David0000-0002-6780-4252
Gagné, Jonathan0000-0002-2592-9612
Albert, Loïc0000-0003-0475-9375
Naud, Marie-Eve0000-0003-1807-1598
Janson, Markus0000-0001-8345-593X
Beichman, Charles0000-0002-5627-5471
Additional Information:© 2018. The American Astronomical Society. Received 2018 May 30; revised 2018 July 19; accepted 2018 July 22; published 2018 August 30. Based on observations obtained at the Gemini Observatory through programs number GS-2014B-Q-2, GS-2015A-Q-71, GS-2015B-Q-57, GS-2016A-Q-69, GS-2016B-Q-33, GS-2017A-Q-58, and GS-2017B-Q-34. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). The authors would like to thank the anonymous referee for constructive comments and suggestions that improved the overall quality of the paper. This work was financially supported by the Fond de Recherche Québécois—Nature et Technologie(FRQNT; Québec). Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE) and the Los Alamos National Laboratory. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, particularly those participating in the Gaia Multilateral Agreement. Facilities: Gemini-South (Flamingos-2 - , GMOS-S) - , CFHT (WIRCam - , MegaCam) - , Spitzer (Irac). - Software: SExtractor (Bertin & Arnouts 1996), Scamp (Bertin 2010a), Swarp (Bertin 2010b), CFHT'S Elixir pipeline.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Fonds de recherche du Québec – Nature et technologies (FRQNT)UNSPECIFIED
NASANNX08AR22G
NSFAST-1238877
Gaia Multilateral AgreementUNSPECIFIED
Subject Keywords:planets and satellites: gaseous planets; planets and satellites: detection
Issue or Number:3
Record Number:CaltechAUTHORS:20180830-145509367
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180830-145509367
Official Citation:Frédérique Baron et al 2018 AJ 156 137
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:89323
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:30 Aug 2018 22:19
Last Modified:24 Feb 2020 10:30

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