Two Jupiter-mass Planets Discovered by the KMTNet Survey in 2017

Creators: Shin, I.-G.; Ryu, Y.-H.; Yee, J. C.; Gould, A.; Albrow, M. D.; Chung, S.-J.; Han, C.; Hwang, K.-H.; Jung, Y. K.; Shvartzvald, Y.; Zang, W.; Lee, C.-U.; Cha, S.-M.; Kim, D.-J.; Kim, H.-W.; Kim, S.-L.; Lee, Y.; Lee, D.-J.; Park, B.-G.; Pogge, R. W.

Abstract

We report two microlensing events, KMT-2017-BLG-1038 and KMT-2017-BLG-1146 that are caused by planetary systems. These events were discovered by KMTNet survey observations from the 2017 bulge season. The discovered systems consist of a planet and host star with mass ratios, 5.3^(+0.2)_(−0.4)×10^(−3) and 2.0^(+0.6)_(−0.1)×10^(−3), respectively. Based on a Bayesian analysis assuming a Galactic model without stellar remnant hosts, we find that the planet, KMT-2017-BLG-1038Lb, is a super Jupiter-mass planet (M_p = 2.04^(+2.02)_(−1.15)M_J) orbiting a mid-M dwarf host (M_h = 0.37^(+0.36)_(−0.20)M⊙) that is located at 6.01^(+1.27)_(−1.72) kpc toward the Galactic bulge. The other planet, KMT-2017-BLG-1146Lb, is a sub Jupiter-mass planet (M_p = 0.71^(+0.80)_(−0.42)M_J) orbiting a mid-M dwarf host (M_h = 0.33^(+0.36)_(−0.20)M⊙) at a distance toward the Galactic bulge of 6.50^(+1.38)_(−2.00) kpc. Both are potentially gaseous planets that are beyond their hosts' snow lines. These typical microlensing planets will be routinely discovered by second-generation microlensing surveys, rapidly increasing the number of detections.

Additional Information

© 2019 The American Astronomical Society. Received 2018 November 29; revised 2019 February 7; accepted 2019 February 16; published 2019 March 18. 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Work by I.G.S. and A.G. was supported by JPL grant 1500811. A.G. acknowledges the support from NSF grant AST-1516842. A.G. received support from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant Agreement No. [321035]. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea.

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