Han CUdalski AKim DJung YKLee CUBond IAChung SJGould AHwang KHKim HWRyu YHShin IGShvartzvald YZang WYee JCCha SMKim DJKim SLLee DJLee YPark BGPogge RWKim CHKim WTMróz PSzymański MKSkowron JPoleski RSoszyński IPietrukowicz PKozłowski SUlaczyk KRybicki KAIwanek PWrona MGromadzki MAbe FBarry RBennett DPBhattacharya ADonachie MFujii HFukui AItow YHirao YKirikawa RKondo ILi MCAMatsubara YMuraki YMiyazaki SRanc CRattenbury NJSatoh YShoji HSuematsu HSumi TSuzuki DTanaka YTristram PJYamakawa TYamawaki TYonehara AAlbrow, Michael2021-11-022021-11-022021Han C, Udalski A, Kim D, Jung YK, Lee CU, Bond IA, Albrow MD, Chung SJ, Gould A, Hwang KH, Kim HW, Ryu YH, Shin IG, Shvartzvald Y, Zang W, Yee JC, Cha SM, Kim DJ, Kim SL, Lee DJ, Lee Y, Park BG, Pogge RW, Kim CH, Kim WT, Mróz P, Szymański MK, Skowron J, Poleski R, Soszyński I, Pietrukowicz P, Kozłowski S, Ulaczyk K, Rybicki KA, Iwanek P, Wrona M, Gromadzki M, Abe F, Barry R, Bennett DP, Bhattacharya A, Donachie M, Fujii H, Fukui A, Itow Y, Hirao Y, Kirikawa R, Kondo I, Li MCA, Matsubara Y, Muraki Y, Miyazaki S, Ranc C, Rattenbury NJ, Satoh Y, Shoji H, Suematsu H, Sumi T, Suzuki D, Tanaka Y, Tristram PJ, Yamakawa T, Yamawaki T, Yonehara A (2021). KMT-2019-BLG-1715: Planetary microlensing event with three lens masses and two source stars. Astronomical Journal. 161(6). 270-270.0004-62561538-3881https://hdl.handle.net/10092/102831We investigate the gravitational microlensing event KMT-2019-BLG-1715, the light curve of which shows two short-term anomalies from a caustic-crossing binary-lensing light curve: one with a large deviation and the other with a small deviation. We identify five pairs of solutions, in which the anomalies are explained by adding an extra lens or source component in addition to the base binary-lens model. We resolve the degeneracies by applying a method in which the measured flux ratio between the first and second source stars is compared with the flux ratio deduced from the ratio of the source radii. Applying this method leaves a single pair of viable solutions, in both of which the major anomaly is generated by a planetary-mass third body of the lens, and the minor anomaly is generated by a faint second source. A Bayesian analysis indicates that the lens comprises three masses: a planet-mass object with ∼2.6 M and binary stars of K and M dwarfs lying in the galactic disk. We point out the possibility that the lens is the blend, and this can be verified by conducting high-resolution follow-up imaging for the resolution of the lens from the source. JenAll rights reserved unless otherwise statedastro-ph.EPastro-ph.GAastro-ph.SRJournal Article2021-06-170201 Astronomical and Space SciencesFields of Research::51 - Physical sciences::5101 - Astronomical sciences::510107 - Planetary science (excl. solar system and planetary geology)Fields of Research::51 - Physical sciences::5101 - Astronomical sciences::510109 - Stellar astronomy and planetary systemsFields of Research::51 - Physical sciences::5101 - Astronomical sciences::510108 - Solar physicshttp://doi.org/10.3847/1538-3881/abf4d0