adsabs/AstroCLIMB huggingface dataset:
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The minimum mass detectable at S/N = 5 as predicted from our contrast levels using the Marley et al. (2021) models. The blue line and points are from this work. The contrast curves reported by Thalmann et al. (2011; Subaru/IRCS), Vigan et al. (2015; SPHERE), and Pathak et al. (2021; VISIR) have been reanalyzed using the Bobcat models for spectra and evolution, incorporating a T eq correction as described in Section 4.1 with A  B  = 0.5. The shaded region encompasses the minimum-to-maximum mass across all sampled points at that radius. Points at 1 M J are likely overestimates, as that is the lower limit of the range of the model grid (shown as a cross-hatched region for out-of-bounds masses).
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The line labeled “this work, median” indicates the median contrast level for which we would detect a source at S/N = 5, taken over the contrast levels for all PAs at that separation. The variation of contrast with PA is captured by the shaded gray region on either side of the line. Left: the contrast levels as a function of separation in arcseconds with the Thalmann et al. (2011), Vigan et al. (2015), and Pathak et al. (2021) reported curves for comparison. Right: the contrast levels scaled into λ/D units to compare the inner working angle across wavelengths and telescopes more effectively. When scaled by the telescope diameter and wavelength, the ability of the gvAPP-180 coronagraph to work at extremely small inner working angles is apparent.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: S/N map of the final derotated focal plane. To calculate the detection map, the optimized mode fraction k for a particular location (ρ, θ) is taken from the optimization process and applied to reducing the original data without an injected companion. The resulting S/N, measured in λ/D-spaced apertures and computed with the correction from Mawet et al. (2014), is shown in this figure. We found no S/N ≥ 4 signals to report, and the lower S/N signals we inspected did not behave like a companion (moving with changing k, or disappearing) which points to a local maximum of the optimization process producing a spurious detection.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Visualization of the mass limit. This minimum mass is detectable when the separation is entirely in the plane of the sky; in other words, when the planet is experiencing the maximum irradiation for that projected separation. Since the irradiation depends on the actual separation, while the contrast limit depends on the projected separation, it is easier to interpret these results through completeness plots.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The masses detectable at a host-to-planet contrast of 10−5 and 5 × 10−6 are shown overlaid on a contour plot of planet absolute [3.95] mag predicted by the Bobcat models for t = 242 Myr and T eff = 9910 K for Sirius.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Contrast map of the faintest signal detectable at S/N = 5, expressed as a ratio to the host-star flux.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The minimum mass detectable at S/N = 5 as predicted from our contrast levels using the Marley et al. (2021) models, without irradiation (A  B  = 1.0). The blue line and points are from this work.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Visualization of the spatial distributions of hyperparameters found by the optimization process. (a) Distribution of the optimal modes fraction ﹩k/{k}_{\max }﹩ at each position scaled by 1/n, where n is the optimal number of frames to coadd from the n ∈ {1, 10, 50} values evaluated. (b) Spatial distribution the optimal number of frames to coadd n ∈ {1, 10, 50}. (c) Optimized amplitude of injected signal used to measure an S/N and compute the limiting amplitude where S/N = 5. Since injecting a signal with an amplitude much greater than the limit will cause us to overestimate the limit, we vary the amplitude in the optimization process as well as described in Section 3.6.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Minimum masses detectable at S/N = 5 at our contrast levels using the Marley et al. (2021) models when assuming a second epoch of planet formation at t = 141 Myr. The blue line and points are from this work. The contrast curves from the literature have also been reanalyzed using the Bobcat models for spectra and evolution, incorporating a T eq correction as described in Section 4.1. (Points at 1 M J are likely overestimates, as that is the limit of the model grid.)
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The fraction of planets in randomly drawn orbits around Sirius A that would be detectable in these observations and/or a past study of Sirius A, as a function of semimajor axis and mass. When combining the results of all four studies, at least one study would have detected a 9 M J planet in the 2.5–7 au range for 99% of trials.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The fraction of planets in randomly drawn orbits around Sirius A that would be detectable in these observations, as a function of semimajor axis and mass. (Note that the separation axis is scaled differently from that in Figure 14.)
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The fraction of planets formed in a hypothetical second period of formation at t = 141 Myr in randomly drawn orbits around Sirius A that would be detectable in these observations, as a function of semimajor axis and mass.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Minimum masses detectable at S/N = 5 at our contrast levels using the Marley et al. (2021) models assuming a second epoch of planet formation, without irradiation. The blue line and points are from this work.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Long-cadence (1800 s), unbinned transit observations of TOI-5375 in TESS Sectors 20 (top) and 26 (middle), and short-cadence (120 s) unbinned photometry from TESS Sector 40 (bottom). Variability in the host star’s light curve evolves throughout the different sectors, which we infer to be due to varying stellar spots. The periodicity of the spot-induced variability is tied to the rotation of the primary star. We also see flares due to stellar activity, which are masked out in our analysis.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Speckle contrast curve of TOI-5375 from the Sloan z’ filter using NESSI. The blue squares are 5σ contrast limits at each angular separation with a spline fit in red. The black plus signs are the extreme local maxima and the black dots are extreme local minima for the sensitivity limits. The data reveals no bright companions and no significant sources of dilution at separations from 0.″2 to 1.″2 from TOI-5375. The inset is the 4.″7 × 4.″7 NESSI speckle image centered on TOI-5375 in the z’ filter.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Top: light curve of RBO data of an exposure time of 240 s normalized and detrended using AstroImageJ. The MCMC model is overlaid with the blue shaded region indicating a 1σ deviation. Bottom: residuals of this model with a median value of 1528.52 ppm.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Top left: RV data points in black with the best-fitting joint fit model overlaid in blue. Bottom left: residuals from the best-fit model. Right: phase-folded RVs with the best-fitting joint fit model overlaid.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Representative example of TESS Sector 20 photometry along with a stellar rotation GP kernel is shown in the top panel. The detrended photometry is shown in the middle panel, with the eclipses overlaid in blue. The bottom panel shows the residuals.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Derived mass and radius of the companion of TOI-5375 plotted with other objects near the hydrogen-burning mass limit. For reference, Kepler-503 is plotted in blue (Cañas et al. 2018); TOI-148, TOI-587, and TOI-681 are plotted in blue, orange, and green, respectively, while other low-mass stars and high-mass substellar companions from von Boetticher et al. (2017) are plotted as gray circles. We show solar metallicity ([M/H] = 0.0) evolutionary isochrone tracks from Baraffe et al. (2015; solid lines) and from (Marley et al. 2021; dashed lines). These models are for substellar companions and low-mass stars and span the ages 0.4, 1, 4, and 10 Gyr.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Phase-folded photometric observations for TOI-5375 in Sector 20. The gray points are the detrended data, the red points are 300 s bins, and the model is shown in blue with a thin blue shaded region indicating a 1σ deviation. The median residual value for the joint fit over all sectors and including the primary and secondary eclipse is 1330 ppm.
Paper: TOI-5375 B: A Very Low Mass Star at the Hydrogen-burning Limit Orbiting an Early M-type Star 
Authors: Mika Lambert, Chad F. Bender, Shubham Kanodia, Caleb I. Cañas, Andrew Monson, Gudmundur Stefánsson, William D. Cochran, Mark E. Everett, Arvind F. Gupta, Fred Hearty, Henry A. Kobulnicky, Jessica E. Libby-Roberts, Andrea S. J. Lin, Suvrath Mahadevan, Joe P. Ninan, Brock A. Parker, Paul Robertson, Christian Schwab, Ryan C. Terrien
Figure caption: Phase-folded photometric observations of the secondary eclipse for TOI-5375 in Sector 20. Plot markers are identical to those used in Figure 6.
Paper: Systematic KMTNet Planetary Anomaly Search. VIII. Complete Sample of 2019 Subprime Field Planets
Authors: Youn Kil Jung, Weicheng Zang, Hanyue Wang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Jonathan Green, Steve Hennerley, Andrew Marmont, Shude Mao, Dan Maoz, Jennie McCormick, Tim Natusch, Matthew T. Penny, Ian Porritt, Wei Zhu
Figure caption: Scatter plot on the  π  E plane derived from the MCMC of the two parallax models of KMT-2019-BLG-0298 presented in Table 2, color-coded (red, yellow, green, cyan, blue) for Δχ 2 < (1, 4, 9, 16, 25). The contours are effectively 1D, with widths σ(π E,∥) ≡ σ ∥ ∼ 0.039 and 0.046. The black contours show the mean and covariances (Δχ 2 = 1) that are used in Section 5.1.
Paper: Systematic KMTNet Planetary Anomaly Search. VIII. Complete Sample of 2019 Subprime Field Planets
Authors: Youn Kil Jung, Weicheng Zang, Hanyue Wang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Jonathan Green, Steve Hennerley, Andrew Marmont, Shude Mao, Dan Maoz, Jennie McCormick, Tim Natusch, Matthew T. Penny, Ian Porritt, Wei Zhu
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the two planetary models of KMT-2019-BLG-0298 specified in Table 2, plus the 1L2S model. The caustic topologies are shown in the insets for both the close and wide geometries, but the wide geometry is decisively favored by Δχ 2 = 19. The 1L2S model is excluded at Δχ 2 = 125.
Paper: Systematic KMTNet Planetary Anomaly Search. VIII. Complete Sample of 2019 Subprime Field Planets
Authors: Youn Kil Jung, Weicheng Zang, Hanyue Wang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Jonathan Green, Steve Hennerley, Andrew Marmont, Shude Mao, Dan Maoz, Jennie McCormick, Tim Natusch, Matthew T. Penny, Ian Porritt, Wei Zhu
Figure caption: Scatter plot on the  π  E plane derived from the MCMC of the four parallax models of OGLE-2019-BLG-0249 presented in Table 7, color-coded (red, yellow, green, cyan, blue) for Δχ 2 < (1, 4, 9, 16, 25). The contours are effectively 1D, with typical widths σ ∥ ∼ 0.0080 and 0.0065, for the close and wide solutions, respectively. The black contours show the mean and covariances that are used in Section 5.4.
Paper: Systematic KMTNet Planetary Anomaly Search. VIII. Complete Sample of 2019 Subprime Field Planets
Authors: Youn Kil Jung, Weicheng Zang, Hanyue Wang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Jonathan Green, Steve Hennerley, Andrew Marmont, Shude Mao, Dan Maoz, Jennie McCormick, Tim Natusch, Matthew T. Penny, Ian Porritt, Wei Zhu
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the three planetary models of KMT-2019-BLG-1216 specified in Table 3, plus the 1L2S model. The caustic topologies are shown in the insets for the inner, outer, and off-axis models. The first two are perfectly degenerate, but the last is decisively disfavored at Δχ 2 = 24. The 1L2S model is excluded at Δχ 2 = 57.
Paper: Systematic KMTNet Planetary Anomaly Search. VIII. Complete Sample of 2019 Subprime Field Planets
Authors: Youn Kil Jung, Weicheng Zang, Hanyue Wang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Jonathan Green, Steve Hennerley, Andrew Marmont, Shude Mao, Dan Maoz, Jennie McCormick, Tim Natusch, Matthew T. Penny, Ian Porritt, Wei Zhu
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the two planetary models of OGLE-2019-BLG-0249 specified in Table 7 with the caustic topologies shown as insets. Also shown are the 1L1S and 1L2S models.