OGLE-2018-BLG-1700L: Microlensing Planet in Binary Stellar System
Abstract
We report a planet in a binary that was discovered from the analysis of the microlensing event OGLE-2018-BLG-1700. We identify the triple nature of the lens from the fact that the anomaly pattern can be decomposed into two parts produced by two binary-lens events, in which one binary pair has a mass ratio of ~0.01 between the lens components and the other pair has a mass ratio of ~0.3. We find two sets of degenerate solutions, in which one solution has a projected separation between the primary and its stellar companion less than the angular Einstein radius θ_E (close solution), while the other solution has a separation greater than θ_E (wide solution). From the Bayesian analysis with the constraints of the event timescale and angular Einstein radius, we find that the planet has a mass of 4.4^(+3.0)_(−2.0) M_J and the stellar binary components have masses of 0.42^(+0.29)_(−0.19) M_⊙ and 0.12^(+0.08)_(−0.05) M_⊙, respectively, and the distance to the lens is D_L=7.6^(+1.2)_(−0.9) kpc. The planet is a circumstellar planet according to the wide solution, while it is a circumbinary planet according to the close solution.
Additional Information
© 2020 The American Astronomical Society. Received 2019 September 11; revised 2019 November 25; accepted 2019 November 29; published 2020 January 13. Work by C.H. was supported by the grants (2017R1A4A1015178 and 2019R1A2C2085965) of National Research Foundation of Korea. Work by A.G. was supported by US NSF grant AST-1516842 and by JPL grant 1500811. A.G. received support from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant Agreement No. [32103]. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI) and the data were obtained at three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. The MOA project is supported by JSPS KAKENHI grant No. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, JP17H02871, and JP16H06287. Y.M. acknowledges the support by the grant JP14002006. D.P.B., A.B., and C.R. were supported by NASA through grant NASA-80NSSC18K0274. 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. We acknowledge the high-speed Internet service (KREONET) provided by Korea Institute of Science and Technology Information (KISTI).Attached Files
Published - Han_2020_AJ_159_48.pdf
Submitted - 1909.04854.pdf
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Additional details
- Eprint ID
- 100676
- Resolver ID
- CaltechAUTHORS:20200113-111132037
- National Research Foundation of Korea
- 2017R1A4A1015178
- National Research Foundation of Korea
- 2019R1A2C2085965
- NSF
- AST-1516842
- JPL
- 1500811
- European Research Council (ERC)
- 32103
- National Science Centre (Poland)
- 2014/14/A/ST9/00121
- 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)
- JP17H02871
- Japan Society for the Promotion of Science (JSPS)
- JP16H06287
- Japan Society for the Promotion of Science (JSPS)
- JP14002006
- NASA
- 80NSSC18K0274
- NASA Postdoctoral Program
- Royal Society of New Zealand
- Created
-
2020-01-13Created from EPrint's datestamp field
- Updated
-
2021-11-16Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)