KMT-2016-BLG-1397b: KMTNET-only Discovery of a Microlens Giant Planet
- Creators
- Zang, Weicheng
- Hwang, Kyu-Ha
- Kim, Hyoun-Woo
- Gould, Andrew
- Wang, Tianshu
- Zhu, Wei
- Mao, Shude
- Albrow, Michael D.
- Chung, Sun-Ju
- Han, Cheongho
- Jung, Youn Kil
- Ryu, Yoon-Hyun
- Shin, In-Gu
- Shvartzvald, Yossi
- Yee, Jennifer C.
- Cha, Sang-Mok
- Kim, Dong-Jin
- Kim, Seung-Lee
- Lee, Chung-Uk
- Lee, Dong-Joo
- Lee, Yongseok
- Park, Byeong-Gon
- Pogge, Richard W.
Abstract
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.
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.Attached Files
Published - Zang_2018_AJ_156_236.pdf
Accepted Version - 1810.10792.pdf
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Additional details
- Eprint ID
- 90560
- Resolver ID
- CaltechAUTHORS:20181101-105223492
- 11333003
- National Natural Science Foundation of China
- 11390372
- National Natural Science Foundation of China
- 11761131004
- National Natural Science Foundation of China
- AST-1516842
- NSF
- 1500811
- JPL
- 2016-1-832-01
- Korea Astronomy and Space Science Institute (KASI)
- 321035
- European Research Council (ERC)
- 2017R1A4A1015178
- National Research Foundation of Korea
- Created
-
2018-11-01Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)