adsabs/AstroCLIMB huggingface dataset:
Paper: ExoVista: A Suite of Planetary System Models for Exoplanet Studies
Authors: Christopher C. Stark
Figure caption: Illustration of the positions of several planets in a planetary system over a time span of 5 yr generated by exoVista. The inner planet (red) transits in front of the host star (black).
Paper: ExoVista: A Suite of Planetary System Models for Exoplanet Studies
Authors: Christopher C. Stark
Figure caption: Example stellar radial velocity information extracted from a planetary system model generated by exoVista. Stellar noise and activity are not included.
Paper: ExoVista: A Suite of Planetary System Models for Exoplanet Studies
Authors: Christopher C. Stark
Figure caption: Example TTV plot for a transiting planet generated by exoVista. The gravitational influence of other planets impacts the time of transit ingress.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Distribution of the instantaneous eccentricities of the final selected planet pairs at the beginning (dashed black) and end (solid green) of the stability run. Their similarity shows they are in statistical steady state. The gray background shows the initial combined eccentricity for all planet pairs, including those that went unstable and were excluded from the final selection. There is some stability sculpting, particularly at higher eccentricities, but many highly eccentric planet pairs remain. Distributions are shown for the (a) 3:1 and (b) 5:3 resonances.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The probability density of period ratios near the (a) 3:1 and (b) 5:3 mean-motion resonances. The nominal resonance value is marked with a dotted line. The instantaneous final and averaged final distributions are shown for the specified set of generated systems as described in Section 2.1. There is an excess of planet pairs due to the resonance seen in the instantaneous distribution (a result of stability sculpting), but the signal of interest is the narrow peak that is clearly revealed by time-averaging.
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: FO Aqr’s K2 power spectrum binned at 1.25 days with 0.25 day increments. The spin and orbital frequencies are seen at the highest powers throughout the observation. (T 0 ≈ 2144.0 BKJD).
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Several probability density functions with example parameters for the combined eccentricity of the planet pairs (e 1 + e 2). The combined beta distribution was derived numerically from samples taken in accordance with Kipping (2013) parameters and plotted using a Gaussian kernel-density estimate. Combined Rayleigh distributions for various scales were calculated analytically from Equation (3) and plotted for several samples scales: the best-fit value from Hadden & Lithwick (2014), σ = 0.018; the upper limit for 3:1 from this work, σ = 0.245; and the upper limit for 5:3 from this work, σ = 0.095.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Comparison of the posteriors of the fractional peak area of the (a) 3:1 and (b) 5:3 mean-motion resonances. The Kepler sample is in blue and the simulated combined beta distribution from Kipping (2013) sample in red. The median values are shown with a dashed line and the 68.2% percentile intervals with dotted lines. The Kepler sample is not consistent with the beta distribution, which was derived from radial velocity planets.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The cumulative distribution functions of the Kepler data (blue) along with the median model of the posteriors (black) and 10 samples with size equal to that of the Kepler data drawn from the median model (gray) for the (a) 3:1 and (b) 5:3 mean-motion resonances. The differences in the data and model can be explained by the small sample size of the Kepler data.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The cumulative distribution functions of the generated system set (magenta) along with the median model of the posteriors (black) and 100 sample draws from the MCMC posteriors (gray) for the (a) 3:1 and (b) 5:3 mean-motion resonances. The model is tightly fit to the data and shows a clear narrow peak at the resonance.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Comparison of the measured period ratio over time using exact osculating periods from an N-body simulation and the estimated osculating period ratio using the previous two transits at a given point in time to estimate the planet periods. The Pearson correlation coefficient is 0.834, indicating a highly linear correlation. Exact correlation is shown by the black line for reference. The comparison is done for twenty realizations of the K02261 that are consistent with the observed data, 10 of which show signs of libration in the resonant argument while the other 10 do not. Contours of the top 1% and 10% of the point density are shown to aid in interpreting the densest regions. The high correlation indicates that this estimation approach is a useful measurement of the period ratio changing over time directly from the transit times.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The period ratio over time for 20 sample systems of K02261 that are consistent with the observed TTVs. We use the libration or nonlibration in the resonant arguments of the 5:3 resonance to categorize the samples as resonant or nonresonant and extrapolate beyond the Kepler observational period (the time before the solid vertical line) to visualize the periodic behavior in this system. The horizontal lines show the average period ratio over the entire time for each system. The behavior of each individual system varies, but the resonant systems cluster much closer to the exact resonance over time, as expected.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Distribution of the instantaneous period ratio of the final selected planet pairs at the beginning (dashed black) and end (solid green) of the stability run. The gray background shows the initial period ratios in this range for all planet pairs, including those that went unstable and were excluded from the final selection. Distributions are shown for the (a) 3:1 and (b) 5:3 resonances, and the exact commensurabilities are shown with a dotted pink line.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Distribution of the instantaneous magnitude of the difference in the longitudes of the pericenter (such that 0 is aligned and π is antialigned) of the final selected planet pairs at the beginning (dashed black) and end (solid green) of the stability run. The gray background shows the initial magnitude of the difference in the longitudes of the pericenter for all planet pairs, including those that went unstable and were excluded from the final selection. Distributions are shown for the (a) 3:1 and (b) 5:3 resonances. Their agreement shows the phasing of the orbits in the input systems and the randomized phasing share the same distributions.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Distribution of the instantaneous magnitude of the difference in the arguments of the pericenter (such that 0 is aligned and π is antialigned) of the final selected planet pairs at the beginning (dashed black) and end (solid green) of the stability run. The gray background shows the initial magnitude of the difference in the arguments of the pericenter for all planet pairs, including those that went unstable and were excluded from the final selection. Distributions are shown for the (a) 3:1 and (b) 5:3 resonances.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The period ratio over time for K02261 estimated from transit time data from Rowe et al. (2015). Black points are calculated from the given transit times, and errors are the standard deviation of 1000 transit time realizations drawn using the uncertainty on the TTVs. The uncertainty from observations is too large to reveal any structure in the behavior of the period ratio over time.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Distribution of the instantaneous mutual inclination of the final selected planet pairs at the beginning (dashed black) and end (solid green) of the stability run. The gray background shows the initial mutual inclinations for all planet pairs, including those that went unstable and were excluded from the final selection. Distributions are shown for the (a) 3:1 and (b) 5:3 resonances.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Cumulative fraction of the logarithm of the mass ratio of the planets to the star for the generated population of planet pairs (solid coral) and for planet pairs in the Kepler sample (dashed blue) for the (a) 3:1 and (b) 5:3 resonances.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Distribution of the inner planet’s period for the generated population of planet pairs (solid coral) and for planet pairs in the Kepler sample (dashed blue) for the (a) 3:1 and (b) 5:3 resonances.
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Caustic topologies for all six events. For the first four, the degenerate pairs have identical topologies. In each case, for the “inner” topology, the source passes between the central caustic and the two triangular caustics associated with the minor image (opposite side of host from the planet). The “dip” is due to a magnification trough that runs along the planet-host axis, between these caustics. For the “outer” topology, these caustics have merged with the central caustic to form a resonant caustic. The “dip” is then due to the magnification trough that extends out from between these two wings of the resulting resonant caustic. For OGLE-2018-BLG-0977, the source intersects the triangular caustics, so there is no degeneracy. For KMT-2019-BLG-0953, there is only an “outer” solution. See Section 3.7.2.
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: CMDs for each of the six q < 2 × 10−4 planets reported here. The source positions (blue) and clump-giant centroids (red) are shown for all events. For KMT-2019-BLG-0253, the baseline object (green) and blended light (magenta) are also shown. Photometry is in the calibrated OGLE-III system for all except OGLE-2018-BLG-0506 (lower left), which is in the KMTC41 pyDIA system.
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Light curve and models of KMT-2019-BLG-0253. The main evidence for the “inner” and “outer” planetary model (which are virtually identical) is the “dip” in KMTC data from Chile, near 8588.6. This dip is supported by contemporaneous OGLE data, also from Chile, and also by two points from KMTS in South Africa. The dip is the signature of a minor-image perturbation, passing either “inside” or “outside” the two triangular caustics associated with the minor image. See Figure 2.(The data used to create this figure are available.)
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Light curve and model of KMT-2019-BLG-0953. The KMTS and KMTC data show a low-amplitude dip ﹩8643.4\lesssim {\mathrm{HJD}}^{{\prime} }\lt 8643.9﹩, which is not much larger than the individual error bars, but because the event lies in a small region with very high cadence, there are >100 data points during this 12 hr interval. Eight OGLE points near the trough confirm the dip. The dip indicates that the source passed near, but not over, the minor image due to the host. See Figure 2.(The data used to create this figure are available.)
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Light curve and model of OGLE-2018-BLG-0977. The KMTS data near 8280.5 briefly rise and then sharply fall, which indicates entrance into the trough that threads the two minor-image triangular caustics, near (but not over) one of these caustics. The KMTA data near 8281.0 show a sharp decline, followed by flattening, consistent with an exit from the triangular caustic on the opposite side of the trough. The caustic topology diagram (Figure 2) confirms this qualitative light-curve analysis.(The data used to create this figure are available.)
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Light curve and models of OGLE-2018-BLG-0506. The main evidence for an anomaly comes from the dip at about 8224.7 as seen in 26 KMTC points. This is confirmed by two OGLE points. The caustic topology is the same as for KMT-2019-BLG-0253. See Figure 2.(The data used to create this figure are available.)
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Light curve and models of OGLE-2018-BLG-0516. The main evidence for an anomaly comes from the dip at about 8229.85. This is confirmed by two OGLE points. The KMTA and MOA data trace the end of the dip, while the KMTS data are consistent with the beginning of the dip. The caustic topology is the same as for KMT-2019-BLG-0253 and OGLE-2018-BLG-0506. See Figure 2.(The data used to create this figure are available.)
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Light curve and models of OGLE-2019-BLG-1492. The main evidence for the anomaly comes from the dip in KMTC data at about 8764.65, which is confirmed by two OGLE points. It is also supported by the post-dip “ridge” in KMTS data at about 8665.25. The caustic topology is the same as for KMT-2019-BLG-0253, OGLE-2018-BLG-0506, and OGLE-2018-BLG-0516. See Figure 2.(The data used to create this figure are available.)