CaltechAUTHORS
Published November 2018 | Version Published + Accepted Version
Journal Article Open

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

Creators

  • 1. ROR icon Tsinghua University
  • 2. ROR icon Korea Astronomy and Space Science Institute
  • 3. ROR icon The Ohio State University
  • 4. ROR icon Max Planck Institute for Astronomy
  • 5. ROR icon Canadian Institute for Theoretical Astrophysics
  • 6. ROR icon National Astronomical Observatories
  • 7. ROR icon University of Manchester
  • 8. ROR icon University of Canterbury
  • 9. ROR icon Korea University of Science and Technology
  • 10. ROR icon Chungbuk National University
  • 11. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 12. ROR icon Infrared Processing and Analysis Center
  • 13. ROR icon Kyung Hee University

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

Files

1810.10792.pdf

Files (2.7 MB)

Name Size
md5:0c89a281782a96cfd3001a155e1f8eaf
1.1 MB Preview Download
md5:4538aa164b83583f0154228f3402c5c1
1.6 MB Preview Download

Additional details

Identifiers

Eprint ID
90560
Resolver ID
CaltechAUTHORS:20181101-105223492

Related works

Describes
https://arxiv.org/abs/1810.10792 (URL)

Funding

National Natural Science Foundation of China
11333003
National Natural Science Foundation of China
11390372
National Natural Science Foundation of China
11761131004
NSF
AST-1516842
JPL
1500811
Korea Astronomy and Space Science Institute (KASI)
2016-1-832-01
European Research Council (ERC)
321035
National Research Foundation of Korea
2017R1A4A1015178

Dates

Created
2018-11-01
Created from EPrint's datestamp field
Updated
2021-11-16
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
Infrared Processing and Analysis Center (IPAC)