adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Mass vs. orbital period of confirmed exoplanets with dynamical masses from radial velocity or astrometric detections orbiting Sun-like stars. We define a Sun-like star as any star with a mass and radius in the ranges [0.75–1.25 M ☉] and [0.75–1.25 R ☉], respectively. Earth, Jupiter, and Saturn are also plotted to show their relative location with confirmed exoplanets. The paucity of exoplanets at low masses and long periods reflects the limitations of our observational techniques rather than true exoplanet demographics. Exoplanet data extracted from the composite planetary systems data set, using all systems not flagged as controversial, from the NASA Exoplanet Science Institute (2022), accessed on 2023 September 18.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Corner plot for Roman observing program with 10 yr of observations every 40 days and an assumed 1σ measurement error of 5 μas. Simulated data are of a Jupiter-like exoplanet (subscript 1 above) and an Earth-like exoplanet (subscript 2 above) orbiting a Sun-like star at 10 pc. Plot generated with corner.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Simulated “true” RVs for a Jupiter-like exoplanet around Sun-like star. Predicted Terra Hunting Experiment (THE) observations assuming white noise errors of 0.3 m s−1, and nightly observations for 180 days per year, for 10 yr. And MCMC posterior results for the RVs.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Simulated “true” Earth-like RVs around Sun-like star. Predicted Terra Hunting Experiment (THE) observations assuming white noise errors of 0.3 m s−1, and nightly observations for 180 days per year, for 10 yr. And MCMC posterior results for the RVs.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Stellar radius as a function of effective temperature for the 85 host stars in the TKS sample, with metallicity shown as color gradient. The CKS sample (Petigura et al. 2022) and the Gaia-Kepler sample (Berger et al. 2020a, 2020b) are shown for reference in dark and light gray, respectively.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Four examples of significant TTVs detected among TKS systems, including three from multiplanet systems (panels (a), (b), and (d)) and one from a single-planet system (panel (c)). (a) TOI-1136.01: TTV semiamplitude ≈24 minutes, TTV signal period ≈790 days; (b) TOI-1246.03: TTV semiamplitude ≈61 minutes, TTV signal period ≈990 days; (c) TOI-1279.01: TTV semiamplitude ≈34 minutes, TTV signal period ≈775 days; (d) TOI-1339.03: TTV semiamplitude ≈22 minutes, TTV signal period ≈960 days, with significant scatter likely attributed to TTV chopping. These TTVs are measured from the observed transit midpoints (fit via exoplanet) minus the transit midpoints calculated assuming a linear ephemeris. An estimated sinusoidal signal is shown fit to each set of TTVs, using a Lomb−Scargle periodogram and regression fit from astropy. These significant TTV signals likely arise from dynamical interactions between planetary companions.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Before (top) and after (bottom) applying our detrending and initial TTV fitting procedure to the photometry of TOI-1136, a multiplanet system with high stellar variability. We only show the first sector (Sector 14) of this target’s photometry here, but all sectors display similar variability. We model our detrended transit photometry and measure R  p /R ⋆ values for all four planets that agree with the values reported by Dai et al. (2023) within ∼1.5σ, as opposed to the TOI Catalog values, which are all more than 1.5σ discrepant. Black points highlight transits (±0.75 times T 14), colored vertical dashed lines show modeled transit midpoints, and dark-gray vertical dashed lines show calculated transit midpoints assuming a linear ephemeris. In the sector shown, we find the most significant TTVs for TOI-1136.03 (green) as can be seen by the separation between the modeled and calculated midpoints.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Stellar radius (left) and effective temperature (right) as measured by our stellar characterization procedure (TKS) on the y-axis compared to the values reported by the Gaia DR2 pipeline (top) and the TOI Catalog (bottom) on the x-axis. The TKS results produce reduced uncertainties and are generally consistent with one or both external sources. The residuals of our comparison between R ⋆,TKS and R ⋆,TOI can be seen in Figure 6(a). We also note that the Gaia DR2 pipeline does not report stellar properties when R ⋆,Gaia ≲ 0.5 R ⊙, leaving out two TKS targets.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: (a) Radius and orbital period for all TKS planets, with stellar mass shown as a color scale. Gray background points show the distribution of planets from the CKS sample (Petigura et al. 2022). The radius gap, as defined by Petigura et al. (2022), is shown as the orange shaded region. The Hot Neptune Desert, as defined by Mazeh et al. (2016), is shown as the region marked off by black dashed lines. (b) Same as panel (a), except x-axis is S inc. (c) Same as panel (a), except x-axis is M ⋆ and color scale is P. (d) Same as panel (c), except x-axis is [Fe/H].
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Residuals of (a) stellar radius R ⋆, (b) planet-to-star radius ratio R  p /R ⋆, and (c) planet radius R  p  between our results and the TOI Catalog measurements (i.e., residual = (R ⋆,TKS − R ⋆,TOI)/σ(R ⋆,TOI)). Dashed vertical lines show the 15th, 50th, and 85th percentiles of each distribution of residuals.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Distribution of median planet radius measurements for the TKS sample from this work, compared against the median radii taken from the TOI Catalog (green). Shaded regions show specific planet categories, classified by planetary radius. We observe a sparser radius gap region using TKS results than is implied by radii from the TOI Catalog, likely owing to our higher-precision measurements.
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Planet-to-star radius ratio R  p /R ⋆ as measured by our planet characterization pipeline (TKS; y-axis) compared to the radius ratio values reported by the TOI Catalog (x-axis). The TKS results have significantly reduced uncertainties and are generally consistent with the TOI Catalog results (see Section 4.2).
Paper: The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars
Authors: Mason G. MacDougall, Erik A. Petigura, Gregory J. Gilbert, Isabel Angelo, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Tara Fetherolf, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Jack Lubin, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Samuel W. Yee
Figure caption: Diagram demonstrating the flow of data throughout the TKS light-curve modeling pipeline. Yellow arrows are data inputs, gray boxes are processes, and blue ovals are data products.
Paper: Dynamical Stability of Polar Circumbinary Orbits and Planet Formation in the Planetary Disk of 99 Herculis
Authors: Ying Wang, Wei Sun, Ji-lin Zhou, Ming Yang, Fu-yao Liu
Figure caption: The outcomes of collisions mainly include seven regimes, which are determined by the impact velocity V i as well as the impact factor b. The corresponding mass of the largest remnant can be calculated by the four equations ﹩{M}_{\mathrm{lr}1}={M}_{{\rm{p}}}+{M}_{\mathrm{targ}\ },﹩                   ﹩{M}_{\mathrm{lr}2}=\left(-0.5\left({Q}_{{\rm{R}}}/{Q}_{\mathrm{RD}}^{{\prime} * }-1\right)+0.5\right){M}_{\mathrm{tot}},﹩                   ﹩{M}_{\mathrm{lr}3}=\tfrac{0.1}{{1.8}^{\eta }}{({Q}_{{\rm{R}}}/Q{{\prime} }_{\mathrm{RD}}^{* })}^{\eta }{M}_{\mathrm{tot}},﹩ and ﹩{M}_{\mathrm{lr}4}={M}_{\mathrm{targ}\ }.﹩ Other variants appearing in these equations and in this figure can be found in Leinhardt & Stewart (2011) and Stewart & Leinhardt (2012).
Paper: Dynamical Stability of Polar Circumbinary Orbits and Planet Formation in the Planetary Disk of 99 Herculis
Authors: Ying Wang, Wei Sun, Ji-lin Zhou, Ming Yang, Fu-yao Liu
Figure caption: The collision outcomes among planetesimals in the polar protoplanetary disk of 99 Herculis system, the coplanar disk of the same binary stars (coplanar case), and the general disk around single stars with the mass of 99 Herculis system (standard case) for comparison. The coplanar case has the same initial conditions as the polar case except for the inclination, which is randomly chosen from 0°–5°. The standard case has the same initial conditions as the coplanar case except the host is a single star with mass 1.4 M ⊙, the total mass of 99 Herculis.
Paper: Dynamical Stability of Polar Circumbinary Orbits and Planet Formation in the Planetary Disk of 99 Herculis
Authors: Ying Wang, Wei Sun, Ji-lin Zhou, Ming Yang, Fu-yao Liu
Figure caption: The phase space (Ω2, i 2) of the simplified Hamiltonian in Equation (1) for 99 Herculis. The red region is the libration zone where the inclination and longitude of the outer orbit ascending node librate in a certain range. The green region is the circulation zone where the longitude of the outer orbit ascending node can circulate in ﹩\left[0^\circ ,360^\circ \right]﹩. The black line is the separatrix between circulation and libration in Equation (2).
Paper: Dynamical Stability of Polar Circumbinary Orbits and Planet Formation in the Planetary Disk of 99 Herculis
Authors: Ying Wang, Wei Sun, Ji-lin Zhou, Ming Yang, Fu-yao Liu
Figure caption: Several fitted curves of Equations (4) and (5), as well as the respective raw data of the minimum stable radii of test particles in polar orbits around binaries with different eccentricities and mass ratios within 107 T 1.
Paper: Dynamical Stability of Polar Circumbinary Orbits and Planet Formation in the Planetary Disk of 99 Herculis
Authors: Ying Wang, Wei Sun, Ji-lin Zhou, Ming Yang, Fu-yao Liu
Figure caption: The collisional timescale of planetesimals in a polar circumbinary disk, ﹩{T}_{\mathrm{col}}^{{\rm{P}}}﹩, and in a coplanar circumbinary disk, ﹩{T}_{\mathrm{col}}^{{\rm{C}}}﹩, obtained by Equation (11) combined with Equation (10). The scaling factor of a solid surface density is set at a moderate value of f  d  = 10.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: Comparison of the gr-band absolute magnitudes at maximum light between globular clusters Miras (open magenta circles) and extragalactic Miras (in various symbols). For extragalactic Miras, literature μ (see text for details) were adopted to convert m  X  to M  X   m  (after corrected for extinction). The left and right panels are for the comparisons of O-rich Miras and C-rich Miras, respectively. The lines are same as in Figure 6, but extrapolated to a longer period.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: The extinction-corrected PL relations in the gr band for the 14 globular clusters Miras as listed in Table 1. The solid lines are the fitted PL relations, while the dotted lines represent the ±2.5σ boundaries. Note that these PL relations are fitted for magnitudes at maximum light, and not the mean lights.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: Examples of r-band ZTF light curves for two Miras in NGC 6822. The orange triangles marked the expected epochs of maximum light (based on the literature period), and the brightest observed data points tend to be found near these orange triangles.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: The PL relations at maximum lights for all of the Miras listed in Tables 1 and 2. The symbols are same as in Figure 9. However, for a better visualization, open and filled symbols were used represent all of the O-rich and C-rich Miras, respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: The gr-band ZTF light curves for the three short-period O-rich extragalactic Miras. The symbols are same as in the right panels of Figure 2.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, 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, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Comparison of light curves between AnomalyFinder (1L1S) and the best fit (2L1S) for OGLE-2016-BLG-0185. Note that the data sets shown in this figure are produced by the KMTNet pipeline, which is actually used for the AnomalyFinder process.
Paper: Beating Stellar Systematic Error Floors Using Transit-based Densities
Authors: Jason D. Eastman, Hannah Diamond-Lowe, Jamie Tayar
Figure caption: A corner plot of the WASP-4 stellar parameters. The contours show the 68% and 95% confidence intervals for the MIST+SED fit (green), the transit-only fit (blue), and the MIST+transit+SED fit (magenta). From this, we can see just how the addition of the transit constrains the stellar density and significantly improves the precision of R * and T eff—to well beyond the systematic floors imposed on the SED and MIST evolutionary models. The areas under each curve in the histograms are proportional to likelihood and are normalized to have the same area between each of the fits for a given parameter. For  ρ * in particular, we can see the huge impact the transit has on shifting the probability to a narrow, high peak.
Paper: Beating Stellar Systematic Error Floors Using Transit-based Densities
Authors: Jason D. Eastman, Hannah Diamond-Lowe, Jamie Tayar
Figure caption: A contour plot showing the maximum allowed unaccounted blend in the transit light curve as a function of impact parameter b and planet-to-star radius ratio p such that its systematic impact  ρ * is below the 2% systematic impact from M *. That is, the leftmost contour shows the family of planets whose systematics on the light-curve-determined  ρ * would be dominated by blends larger than 3% of the host star flux. Stated differently, as long as the unaccounted flux was less than 3%, the largest source of systematic error in the model would come from M *.
Paper: Beating Stellar Systematic Error Floors Using Transit-based Densities
Authors: Jason D. Eastman, Hannah Diamond-Lowe, Jamie Tayar
Figure caption: A contour plot of the error in ﹩\mathrm{log}{g}_{* }﹩ as a function of the percent errors in M * and R *, derived from Equation (22). A typical spectroscopic constraint of 0.1 dex corresponds to 2% error for a solar-type star. When we get systematic-error-dominated values for M * and R * (without a transit density), we still do about 2× better than spectroscopy.
Paper: Beating Stellar Systematic Error Floors Using Transit-based Densities
Authors: Jason D. Eastman, Hannah Diamond-Lowe, Jamie Tayar
Figure caption: A plot of ﹩{\sigma }_{\mathrm{log}{g}_{* }}﹩ as a function of ﹩{\sigma }_{\,{\rho }_{* }}﹩, assuming ﹩{\sigma }_{{M}_{* }}=5 \% ﹩. The break-even point of ﹩\mathrm{log}{g}_{* }=0.042﹩ dex, where ﹩{\sigma }_{{M}_{* }}=5 \% ﹩ and from Tayar et al. (2022), is shown as a vertical red dashed line and corresponds to ﹩{\sigma }_{\,{\rho }_{* }}\sim 9 \% ﹩.