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KMT-2016-BLG-1397b: KMTNET-only Discovery of a Microlens Giant Planet

Zang, Weicheng and Hwang, Kyu-Ha and Kim, Hyoun-Woo and Gould, Andrew and Wang, Tianshu and Zhu, Wei and Mao, Shude and Albrow, Michael D. and Chung, Sun-Ju and Han, Cheongho and Jung, Youn Kil and Ryu, Yoon-Hyun and Shin, In-Gu and Shvartzvald, Yossi and Yee, Jennifer C. and Cha, Sang-Mok and Kim, Dong-Jin and Kim, Seung-Lee and Lee, Chung-Uk and Lee, Dong-Joo and Lee, Yongseok and Park, Byeong-Gon and Pogge, Richard W. (2018) KMT-2016-BLG-1397b: KMTNET-only Discovery of a Microlens Giant Planet. Astronomical Journal, 156 (5). Art. No. 236. ISSN 1538-3881. doi:10.3847/1538-3881/aae537.

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We report the discovery of a giant planet in the KMT-2016-BLG-1397 microlensing event, which was found by The Korea Microlensing Telescope Network alone. The timescale of this event is tE = 40.0 ± 0.5 days, and the mass ratio between the lens star and its companion is q = 0.016 ± 0.002. The planetary perturbation in the light curve is a smooth bump, resulting in the classical binary-lens/binary-source (2L1S/1L2S) degeneracy. We measure the V − I color of the (putative) two sources in the 1L2S model, and then effectively rule out the binary-source solution. The finite-source effect is marginally detected. Combined with the limits on the blend flux and the probability distribution of the source size normalized by the Einstein radius ρ, a Bayesian analysis yields the lens mass M_L = 0.45^(+0.33)_(-0.28) M⊙, at distance of D_L = 6.60^(+1.10)_(-1.30) kpc. Thus, the companion is a super-Jupiter of a mass m_p = 7.0^(+5.2)_(-4.3) M_J, at a projected separation r_⊥ = 5.1^(+1.5)_(-1.7) au, indicating that the planet is well beyond the snow line of the host star.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Zang, Weicheng0000-0001-6000-3463
Hwang, Kyu-Ha0000-0002-9241-4117
Kim, Hyoun-Woo0000-0001-8263-1006
Zhu, Wei0000-0003-4027-4711
Mao, Shude0000-0001-8317-2788
Albrow, Michael D.0000-0003-3316-4012
Chung, Sun-Ju0000-0001-6285-4528
Han, Cheongho0000-0002-2641-9964
Jung, Youn Kil0000-0002-0314-6000
Ryu, Yoon-Hyun0000-0001-9823-2907
Shin, In-Gu0000-0002-4355-9838
Shvartzvald, Yossi0000-0003-1525-5041
Yee, Jennifer C.0000-0001-9481-7123
Pogge, Richard W.0000-0003-1435-3053
Additional Information:© 2018 The American Astronomical Society. Received 2018 July 22; revised 2018 September 28; accepted 2018 September 28; published 2018 November 1. We thank Tianjun Gan and Chelsea Huang for discussions. This work was partly supported by the National Science Foundation of China (grant Nos. 11333003, 11390372, and 11761131004 to S.M.). 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. Work by W.Z., Y.K.J., and A.G. were supported by AST-1516842 from the US NSF. W.Z., I.G.S., and A.G. were supported by JPL grant 1500811. A.G. is supported from KASI grant 2016-1-832-01. A.G. received support from the European Research Council under the European Unions Seventh Framework Programme (FP 7) ERC Grant Agreement n. [321035]. Work by C.H. was supported by grant (2017R1A4A1015178) of the National Research Foundation of Korea.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
National Natural Science Foundation of China11333003
National Natural Science Foundation of China11390372
National Natural Science Foundation of China11761131004
Korea Astronomy and Space Science Institute (KASI)2016-1-832-01
European Research Council (ERC)321035
National Research Foundation of Korea2017R1A4A1015178
Issue or Number:5
Record Number:CaltechAUTHORS:20181101-105223492
Persistent URL:
Official Citation:Weicheng Zang et al 2018 AJ 156 236
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:90560
Deposited By: Tony Diaz
Deposited On:01 Nov 2018 18:09
Last Modified:16 Nov 2021 03:33

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