adsabs/AstroCLIMB huggingface dataset:
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Simulated light curves for a WASP-43 b-like exoplanet using our panchromatic light-curve model EXPLOR. The top panel shows the white light curve convolved with the observational noise from JWST’s /Mid Infrared Instrument (MIRI), and the middle panel shows the same but convolved with the noise profile from Ariel. The bottom two panels show the underlying simulated spectra (in full resolution) at phases color marked in the white light curves (top and middle panels). Note that the top and middle panels are zoomed to illustrate the phase variations and eclipses, while the insets show the full light curve with the transit. Each data point corresponds to Δt = 7 mn integrations. By definition of the instruments, the JWST/MIRI phase curve covers λ ∈ [5, 12] μm, while the Ariel phase curve covers λ ∈ [0.5, 7.8] μm.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Simulated panchromatic light-curve observation of a WASP-43 b exoplanet with JWST/MIRI (top) for our Scenario 1. Middle: the corresponding best-fit solution from the EXPLOR atmospheric retrieval. Bottom: the residuals between the simulated observations and the best-fit solution, normalized by the observational uncertainties σ. The simulation is created with the same model as shown in Figure 1.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Simulated panchromatic light-curve observation of a WASP-43 b exoplanet with Ariel (top) for our Scenario 1. Middle: the corresponding best-fit solution from the EXPLOR atmospheric retrieval. Bottom: residuals between the simulated observations and the best-fit solution, normalized by the observational uncertainties σ. The simulation is created with the same model as shown in Figure 1.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Relationship between goodness of fit (R 2) and the range magnitude. When the range magnitude exceeds 0.1, the goodness of fit (R 2) value is greater than 0.99 and is represented by a red line. When the range magnitude falls between 0.03 and 0.1, the goodness of fit (R 2) surpasses a value calculated by formula 3, which is depicted by an orange line.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: The structure of the autoencoder neural network is shown. This structure contains the encoding structure and the decoding structure. The input of the network is a noise-added light curve of contact binary, and the output is a noise-free light curve. μ is set to 0, and the value of σ is sampled from the Poisson distribution in Figure 2.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Left: the light curve was interpolated to 4 points and then inverse interpolated back to 1000 points, calculating the standard deviation of residuals compared to the original light curve. The standard deviation of residuals is 0.2439. Right: This figure shows the error situation of this light curve when it is interpolated from 2 points to 200 points and then inverse interpolated back to 1000 points.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Top: TIC 388106759 is a nonvariable star with a noise standard deviation of 0.0013888. Bottom: noise distribution of 2230 targets similar to TIC 388106759.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: This figure depicts the situation where the error is less than 0.001 when 2707 light curves are interpolated to a certain number of points and then inverse interpolated back to 1000 points.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Left: the blue dots are the light curve generated by Phoebe with Gaussian noise added. The orange light curve is generated by the trained autoencoder model using the blue dots as inputs. Right: the distribution of the goodness of fit (R 2) between the 150,000 input light curves and the responding output light curves is shown.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: The distribution of parameters for contact binary stars is shown.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: (a) Velocities of primary component M and secondary component m in a coordinate system associated with the center of mass CM,  v    m   = −(M/m) v    M  , by conservation of momentum. (b) Velocities of primary component M and center of mass CM in a coordinate system associated with the secondary component.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: Violin plot for the dependence of the relative mean-square velocity σ/σ 0 on the SB1 fraction f in a square-root scale. The solid line is an approximation of the 50% quantile, the small-dashed line is an approximation of the 5% quantile, and the dashed line is an approximation of the 95% quantile.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: Distribution of the primary-component radial velocities in SB1 systems relative to the center of mass of the binary system in logarithmic scale.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: The surface density profile of NGC 2571, denoted by the solid black line. Dashed black lines show the confidence interval. The horizontal red line shows the mean field density. The smooth magenta line at the bottom right is a polynomial approximation of the surface density in the cluster corona.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: The plane passing through the primary component, containing the line of sight and perpendicular to the orbital plane. The angle i is an inclination of the line of sight to the orbital plane. ﹩{v}_{M}\cos \alpha \cos i﹩ is the desired projection of the velocity of the primary component onto the line of sight.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Panchromatic light-curve retrievals (ExPLOR) for an eclipse of a WASP-43 b-like planet when the data are scattered (top row) vs. unscattered (bottom row). A simulated spectro-temporal flux map convolved with a JWST/MIRI instrument model (left) serves as input to the retrievals. The retrieved best-fit maps obtained with EXPLOR (middle) and the residual maps (right) show the ability of the model to interpret such observations.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Corner plots (left: unscattered input; middle: combination of five independently scattered inputs) from the EXPLOR (black) and the TAUREX (blue) retrievals obtained for the 1.5D (i.e., spatially varying atmosphere) JWST eclipse examples, and retrieved T–p structure (right) for the unscattered case. Similar results to the 1D case shown in Figure 5 are found but the EXPLOR retrieval is allowed to perform eclipse mapping while the TAUREX retrieval is 1D. The retrieval TAUREX T–p profile can only obtain an average of the dayside and hot-spot profiles, but it is reassuring to find that no significant bias is introduced in this case. By design, the EXPLOR retrieval accounts for 3D biases in eclipse and transit (as described in, e.g., Feng et al. 2016; Caldas et al. 2019; Taylor et al. 2020; MacDonald & Lewis 2022), allowing one to extract more realistic information from the data than transitional 1D retrievals.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Retrieved temperature structure for the WASP-43 b panchromatic phase-curve simulations. Left: JWST/MIRI simulation for Scenario 1. Middle: Ariel simulation for Scenario 1. Right: JWST/MIRI simulation for Scenario 2. The solid lines and shaded regions are the median and 1σ and 3σ regions, respectively, while the dashed lines are the true values from the forward model. In all three simulations, the panchromatic light-curve retrievals manage to infer the thermal structure of the planet for all three regions.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Full corner plot of the EXPLOR panchromatic light-curve retrieval for the WASP-43 b-like case for Scenario 2. The true values of this simulation are indicated by the red crosses. Note that the temperature parameters do not have “true” values per say as the location of the nodes is different in the forward and retrieval models. We therefore indicate the absolute temperature of the forward model profiles at the pressures set for the retrieved nodes.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Simulated panchromatic light-curve observation of a WASP-43 b exoplanet with JWST/MIRI (top) for our Scenario 2. Middle: corresponding best-fit solution from the EXPLOR atmospheric retrieval. Bottom: residuals between the simulated observations and the best-fit solution, normalized by the observational uncertainties σ.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Full corner plot of the EXPLOR panchromatic light-curve retrieval for the WASP-43 b-like case for Scenario 1. This shows simulations for JWST/MIRI (black) and Ariel (blue). The true values of this simulation are indicated by the red crosses.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: Orbit of the primary component M relative to the secondary component m. Π is the periastron. IA is the intersection point of the line-of-sight projection and the line of apsides. θ is the true anomaly.
Paper: Velocity Dispersion of the Open Cluster NGC 2571 by Radial Velocities and Proper Motions
Authors: Maxim V. Kulesh, Aleksandra E. Samirkhanova, Giovanni Carraro, Joao V. Sales-Silva, Roberto Capuzzo Dolcetta, Anton F. Seleznev
Figure caption: The left three-panel column reports the distributions of the tangential and radial velocities (black lines) together with their fit by Gaussian functions (red lines). The right three-panel column reports the distributions of the squared errors of velocities (black lines) and their fit by Equation (3) (red lines). Specifically, (a) distribution of the tangential velocities in the direction of the R.A., (b) distribution of their squared errors, (c) distribution of the tangential velocities in the direction of the decl., (d) distribution of their squared errors, (e) distribution of the radial velocities, and (f) distribution of their squared errors.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of MOA-2016-BLG-526 with the family of degenerate 2L1S s − models with the ﹩{\rm{\Delta }}\xi \mbox{--}{\mathrm{log}}_{10}(q)﹩ space. In the ﹩{\rm{\Delta }}\xi \mbox{--}{\mathrm{log}}_{10}(q)﹩ space (upper left panel), each color represents Δχ 2 ≤ n 2 from the best-fit χ 2 where n = 1 (red), 2 (yellow), 3 (green), 4 (light blue), 5 (blue), and 6 (purple), respectively.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of MOA-2016-BLG-526 with 2L1S solutions compared to the 1L1S models.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of MOA-2016-BLG-526 with the degenerate 2L1S s + models and the ﹩{\rm{\Delta }}\xi \mbox{--}{\mathrm{log}}_{10}(q)﹩ space. The color scheme of the ﹩{\rm{\Delta }}\xi \mbox{--}{\mathrm{log}}_{10}(q)﹩ space is identical to that of Figure 5.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: APRX test of OGLE-2016-BLG-1598. The upper two panels show the cumulative Δχ 2 plot between the APRX and STD models with the light curve. The lower three panels show APRX contours obtained using all data (left), OGLE only (middle), and KMTC only (right), respectively.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of OGLE-2016-BLG-1598 with 2L1S and 1L1S models. We also present caustic geometries of the 2L1S models.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of OGLE-2016-BLG-1800 with both 2L1S solutions compared to the 1L1S models.
Paper: Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Subprime Field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Cheongho Han, Hongjing Yang, Andrew Gould, Chung-Uk Lee, Andrzej Udalski, Takahiro Sumi, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of KMT-2016-BLG-2321 with the 2L1S solutions compared to the 1L1S models.