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SHIN, I.-G. (Harvard-Smithsonian Center for Astrophysics ) ;  RYU, Y.-H. ( Korea Astronomy and Space Science Institute ) ;  UDALSKI, A. ( Warsaw University Observatory ) ;  ALBROW, M. ( Department of Physics and Astronomy, University of Canterbury ) ;  CHA, S.-M. ( Korea Astronomy and Space Science Institute ) ;  CHOI, J.-Y. ( Busan National Science Museum ) ;  CHUNG, S.-J. ( Korea Astronomy and Space Science Institute ) ;  HAN, C. ( Department of Physics, Chungbuk National University ) ;  HWANG, K.-H. ( Department of Physics, Chungbuk National University ) ;  JUNG, Y.K. ( Harvard-Smithsonian Center for Astrophysics ) ;  KIM, D.-J. ( Korea Astronomy and Space Science Institute ) ;  KIM, S.-L. ( Korea Astronomy and Space Science Institute ) ;  LEE, C.-U. ( Korea Astronomy and Space Science Institute ) ;  LEE, Y. ( Korea Astronomy and Space Science Institute ) ;  PARK, B.-G. ( Korea Astronomy and Space Science Institute ) ;  PARK, H. ( Busan National Science Museum ) ;  POGGE, R.W. ( Department of Astronomy Ohio State University ) ;  YEE, J.C. ( Harvard-Smithsonian Center for Astrophysics ) ;  PIETRUKOWICZ, P. ( Warsaw University Observatory ) ;  MROZ, P. ( Warsaw University Observatory ) ;  KOZLOWSKI, S. ( Warsaw University Observatory ) ;  POLESKI, R. ( Warsaw University Observatory ) ;  SKOWRON, J. ( Warsaw University Observatory ) ;  SOSZYNSKI, I. ( Warsaw University ) ;  SZYMANSKI, M.K. ULACZYK, K. WYRZYKOWSKI, L. PAWLAK, M. GOULD, A.

We report the characterization of a massive (mp = 3.9±1.4Mjup) microlensing planet (OGLE-2015-BLG-0954Lb) orbiting an M dwarf host (M = 0.33 ± 0.12M⊙) at a distance toward the Galactic bulge of $0.6^{+0.4}_{-0.2}kpc$, which is extremely nearby by microlensing standards. The planet-host projected separation is a⊥ ~ 1.2AU. The characterization was made possible by the wide-field (4 deg2) high cadence (Γ = 6 hr–1) monitoring of the Korea Microlensing Telescope Network (KMTNet), which had two of its three telescopes in commissioning operations at the time of the planetary anomaly. The source crossing time t* = 16 min is among the shortest ever published. The high-cadence, wide-field observations that are the hallmark of KMTNet are the only way to routinely capture such short crossings. High-cadence resolution of short caustic crossings will preferentially lead to mass and distance measurements for the lens. This is because the short crossing time typically implies a nearby lens, which enables the measurement of additional effects (bright lens and/or microlens parallax). When combined with the measured crossing time, these effects can yield planet/host masses and distance.

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