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A Gas Giant Planet in the OGLE-2006-BLG-284L Stellar Binary System

Bennett, David P. and Udalski, Andrzej and Bond, Ian A. and Abe, Fumio and Barry, Richard K. and Bhattacharya, Aparna and Donachie, Martin and Fujii, Hirosane and Fukui, Akihiko and Hirao, Yuki and Itow, Yoshitaka and Kawasaki, Kohei and Kirikawa, Rintaro and Kondo, Iona and Koshimoto, Naoki and Alex Li, Man Cheung and Matsubara, Yutaka and Miyazaki, Shota and Muraki, Yasushi and Ranc, Clément and Rattenbury, Nicholas J. and Satoh, Yuki and Shoji, Hikaru and Sumi, Takahiro and Suzuki, Daisuke and Tanaka, Yuzuru and Tristram, Paul J. and Yamawaki, Tsubasa and Yonehara, Atsunori and Mróz, Przemek and Poleski, Radek and Szymański, Michał K. and Soszyński, Igor and Wyrzykowski, Łukasz and Ulaczyk, Krzysztof (2020) A Gas Giant Planet in the OGLE-2006-BLG-284L Stellar Binary System. Astronomical Journal, 160 (2). Art. No. 72. ISSN 1538-3881. doi:10.3847/1538-3881/ab9cb9. https://resolver.caltech.edu/CaltechAUTHORS:20200720-131329686

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Abstract

We present the analysis of microlensing event OGLE-2006-BLG-284, which has a lens system that consists of two stars and a gas giant planet with a mass ratio of q_p = (1.26 ± 0.19) × 10⁻³ to the primary. The mass ratio of the two stars is q_s = 0.289 ± 0.011, and their projected separation is s_s = 2.1 ± 0.7 au, while the projected separation of the planet from the primary is s_p = 2.2 ± 0.8 au. For this lens system to have stable orbits, the three-dimensional separation of either the primary and secondary stars or the planet and primary star must be much larger than the projected separations. Since we do not know which is the case, the system could include either a circumbinary or a circumstellar planet. Because there is no measurement of the microlensing parallax effect or lens system brightness, we can only make a rough Bayesian estimate of the lens system masses and brightness. We find host star and planet masses of, M_(L1) = 0.35^(+0.30)_(−0.20) M⊙, M_(L2) = 0.10^(+0.09)_(−0.06) M⊙, and m_p = 144^(+126)_(−82) M⊕, and the K-band magnitude of the combined brightness of the host stars is K_L = 19.7^(+0.7)_(−1.0). The separation between the lens and source system will be ~90 mas in mid-2020, so it should be possible to detect the host system with follow-up adaptive optics or Hubble Space Telescope observations.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ab9cb9DOIArticle
https://arxiv.org/abs/2005.07199arXivDiscussion Paper
ORCID:
AuthorORCID
Bennett, David P.0000-0001-8043-8413
Udalski, Andrzej0000-0001-5207-5619
Barry, Richard K.0000-0003-4916-0892
Fukui, Akihiko0000-0002-4909-5763
Itow, Yoshitaka0000-0002-8198-1968
Kondo, Iona0000-0002-3401-1029
Koshimoto, Naoki0000-0003-2302-9562
Miyazaki, Shota0000-0001-9818-1513
Ranc, Clément0000-0003-2388-4534
Rattenbury, Nicholas J.0000-0001-5069-319X
Suzuki, Daisuke0000-0002-5843-9433
Mróz, Przemek0000-0001-7016-1692
Szymański, Michał K.0000-0002-0548-8995
Soszyński, Igor0000-0002-7777-0842
Ulaczyk, Krzysztof0000-0001-6364-408X
Additional Information:© 2020 The American Astronomical Society. Received 2020 May 5; revised 2020 June 3; accepted 2020 June 12; published 2020 July 17. D.P.B., A.B., and C.R. were supported by NASA through grant NASA-80NSSC18K0274. The MOA project is supported in Japan by JSPS KAKENHI grant Nos. JP17H02871, JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, and JP16H06287. The work by C.R. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA. N.J.R. is a Royal Society of New Zealand Rutherford Discovery Fellow. The OGLE Team thanks professors Marcin Kubiak and Grzegorz Pietrzyński for their contribution to the OGLE photometric data. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU.
Funders:
Funding AgencyGrant Number
NASA80NSSC18K0274
Japan Society for the Promotion of Science (JSPS)JP17H02871
Japan Society for the Promotion of Science (JSPS)JSPS24253004
Japan Society for the Promotion of Science (JSPS)JSPS26247023
Japan Society for the Promotion of Science (JSPS)JSPS23340064
Japan Society for the Promotion of Science (JSPS)JSPS15H00781
Japan Society for the Promotion of Science (JSPS)JP16H06287
NASA Postdoctoral ProgramUNSPECIFIED
Royal Society of New ZealandUNSPECIFIED
National Science Centre (Poland)MAESTRO 2014/14/A/ST9/00121
Subject Keywords:Triple lens microlensing ; Gravitational microlensing exoplanet detection ; Finite-source photometric effect ; Gravitational microlensing
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Triple lens microlensing (2137); Gravitational microlensing exoplanet detection (2147); Finite-source photometric effect (2142); Gravitational microlensing (672)
DOI:10.3847/1538-3881/ab9cb9
Record Number:CaltechAUTHORS:20200720-131329686
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200720-131329686
Official Citation:David P. Bennett et al 2020 AJ 160 72
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104456
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:20 Jul 2020 21:01
Last Modified:16 Nov 2021 18:31

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