Light curve of the microlensing event KMT-2018-BLG-1743. The inset shows the zoom-in view of the peak region. The two curves drawn over the data points are the model curves of the 1L1S (dotted) and the wide 2L2S (solid) solutions. The colors of the telescopes in the legend are chosen to match those of the data points in the light curve.

Contexts in source publication

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... Table 1, we present the data rescaling coefficients along with the time range and the number of data points, N data , for the individual data sets. Figure 1 shows the lensing light curve of KMT-2018-BLG-1743. Inspection of the light curve reveals three characteristics. ...

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... model curve (dotted curve) is drawn over the data points in Figure 1. The magnification at the peak of the light curve estimated from the 1L1S model is A peak ∼ 800. ...

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... the light curve exhibits an additional anomaly in the peak region as well as the anomaly in the wing. To better show this central deviation, we present the zoom-in view of the peak region in the inset of Figure 1. The central deviation is most evident for the two KMTS data points taken at the epochs of HJD ′ = 8249.430 ...

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... of the solution, both the primary and secondary source stars cross the caustic, and the caustic crossings of S 1 and S 2 explain the central and peripheral anomalies, respectively. The model curves and the residuals from the models of the wide and close solutions in the regions of the anomalies are shown in Figures 9 and 10, respectively. Despite the significant difference in the lens system configurations, it is found that both solutions result in similar fits to the data. ...

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... find that the models obtained under the 2L2S interpretation provide substantially better fits to the observed data than the other models based on the 2L1S and 3L1S interpretations. This can be seen in the middle panel of Figure 11, where we plot the cumulative distributions of the χ 2 difference relative to the 2L1S model, that is, ∆χ 2 = χ 2 2L1S − χ 2 , for the 3L1S and 2L2S (wide and close) models. We find that the fit of the wide (close) 2L2S model is better than the 3L1S and 2L1S models by ∆χ 2 = 90.8 ...

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... estimate the reddening and extinction corrected (de-reddened) source color and brightness, (V − I, I) 0 , we used the method of Yoo et al. (2004), in which the centroid of the red giant clump (RGC) in the CMD is used as a reference for calibration. Figure 12 shows the locations of S 1 and S 2 with respect to the RGC centroid (red dot) in the instrumental CMD of neighboring stars around the source constructed using the pyDIA photometry of the KMTC I-and V-band data. The pair of the filled blue and green dots denote the positions of S 1 and S 2 based on the wide 2L2S solution, and the pair of the empty dots indicate the positions based on the close 2L2S solution. ...

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... the events produced by the simulation, the posterior distributions of M and D L are obtained by constructing their distributions for events with t E and θ E values located within their ranges of uncertainty. Figure 13 shows the posterior distributions of the host mass M host ≡ M 1 (upper panel) and distance (lower panel) to the planetary lens system. In Table 6, we list the estimated values of M host , M planet ≡ M 2 , D L , and a ⊥ , where a ⊥ = sD L θ E is the physical projected separation between the planet and host. ...