adsabs/AstroCLIMB huggingface dataset:
Paper: Exoplanet Atmospheric Refraction Effects in the Kepler Sample
Authors: Déreck-Alexandre Lizotte, Jason Rowe, James Sikora, Michael R. B. Matesic
Figure caption: Binned Kepler photometry (blue dots) corresponding to three 500-KOI realizations (without replacement) from the above period–radius valley (APRV) population. From this, we see significant sensitivity to systematic noise across realizations. As refraction effects are expected to be symmetric, we have binned the pre/post transit data, as to reduce the point-to-point error. Regardless of systematic variability, the refraction effect is distinguishable near ingress/egress in each realization.
Paper: Exoplanet Atmospheric Refraction Effects in the Kepler Sample
Authors: Déreck-Alexandre Lizotte, Jason Rowe, James Sikora, Michael R. B. Matesic
Figure caption: Binned Kepler photometry (blue dots) of the KOI population which both exists above the period–radius valley and below the H2 atmospheric evaporation limit shown in Figure 4. Overlaid is a clear H2 atmosphere (μ = 2 g mol–1) refraction model (solid red line). Despite these exoplanets being the only ones in the APRV population capable of holding H/He atmospheres, any possible refraction effects are severely dampened when compared to the simulated effect for an optically thin H/He atmosphere.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: The normalized relative flux of WASP-19b as a function of the time (the offset from mid-transit time and in TDB-based BJD) of individual transits observed by TESS between epochs 4778 and 4803: the points are the data of raw flux, solid red lines are best-fit models for model flux, and E is the calculated epoch number.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: The normalized relative flux of WASP-19b as a function of the time (the offset from mid-transit time and in TDB-based BJD) of individual transits taken from ETD between epochs 614 and 5322: here the points, solid red lines, and E represent the same elements as described in Figure A1.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: GLS periodogram computed for the 252 timing residuals of WASP-19b. The purple dashed line indicates the FAP level of the highest peak. The other dashed lines from top to bottom indicate the threshold levels of FAP = 1% and 5%, respectively..
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Same as Figure A1 but for epochs 6655–6675.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: The O − C diagram as a function of epoch along with the best-fit sinusoidal variability.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Residual plot for the apsidal precession model.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Same as Figure A1 but for epochs 4804–5735.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Same as Figure A1 but for epochs 5736–6629.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Same as Figure A1 but for epochs 6630–6654.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: O − C diagram for analyzing 252 mid-transit times of WASP-19b. The blue filled square show the data from L. Abe et al. (2013), the red filled squares are from E. R. Adams et al. (2024), the green filled square is from D. R. Anderson et al. (2010), the black filled circle is from D. R. Anderson et al. (2013), the brown filled asterisks are from L. M. Bernabò et al. (2024), the magenta filled circles are from P. Cortés-Zuleta et al. (2020), the yellow filled upward triangles are from D. Dragomir et al. (2011), the green filled circles are from N. Espinoza et al. (2019), the orange filled right triangles are from the quality 1 and quality 2 data of ETD, the blue filled circles are from ExoClock, the red filled circle is from L. Hebb et al. (2010), the green asterisk is from C. Hellier et al. (2011), the black filled squares are from M. Lendl et al. (2013), the brown filled squares are from L. Mancini et al. (2013), the magenta filled squares are from K. C. Patra et al. (2020), the yellow filled squares are from R. Petrucci et al. (2020), the green filled upward triangle is from E. Sedaghati et al. (2015), the orange filled upward triangle is from J. Southworth et al. (2017), the blue filled asterisks is from TESS data, the red filled asterisks is from J. Tregloan-Reed et al. (2013), the green x-shaped markers are from I. Wong et al. (2016). The dashed black line, red and blue curves represent the linear, orbital decay, and apsidal precession models. The lines are drawn for 100 randomly chosen sets of parameters from the Markov chains of posteriors of the orbital decay (brown) and apsidal precession (cyan) models. The models are extrapolated for the next ∼10 yr to illustrate the broad spectrum of possible solutions.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Stellar spot-affected transit LCs of WASP-19b from different sectors of TESS. The solid lines represent the best-fit models, and the residuals are shown below each LC.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Stellar spot-affected transit LCs of WASP-19b from ETD. The solid lines represent the best-fit models, and the residuals are shown below each LC.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: The normalized relative flux of WASP-19b as a function of the time (the offset from mid-transit time and in TDB-based BJD) of individual transits taken from ExoClock between epochs 4784 and 6012: here, the points, solid red lines, and E represent the same elements as described in Figure A1.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: The Carina star-forming complex region. The labeled six observed tiles, e1040, e1041, e1085, e1086, e1130, and e1131, are from the VVVX survey. The symbols indicate targets observed on each of the three APOGEE-2 observed plates. In the background the DSS2 image of the complete field is shown, in the galactic coordinates, with galactic north up and galactic east to the left.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Same as Figure A6 but for epochs 7078–7145.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Typical APOGEE-2 H-band spectra around the Br 11 region. The spectra are normalized to the continuum by ASPCAP. The red line shows the wavelength of the Br 11 line in the air. The green lines show the 16795 to 16830 Å wavelength interval.
Paper: Investigating Transit Timing Variations in the Ultrashort Period Exoplanet WASP-19b
Authors: Shraddha Biswas, Ing-Guey Jiang, Li-Chin Yeh, Hsin-Min Liu, Kaviya Parthasarathy, Devesh P. Sariya, D. Bisht, Mohit Singh Bisht, A. Raj
Figure caption: Same as Figure A6 but for epochs (5619–6964).
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Results of the statistical analysis of the light curves for the most probable Carina members. Upper left: histogram of the number of observations (epochs) per object. Red bars represent all sources, light green corresponds to reliable sources, and blue indicates periodic variables among the reliable ones. Upper right: amplitude vs. mean KS magnitude diagram. Lower left: skewness vs. kurtosis diagram. Lower right: kurtosis vs. ﹩{\mathrm{log}}﹩(best period) diagram. The color coding is the same for all three diagrams: red for all, light green for reliable, and red crosses marking periodic variables. These plots help identify the nature of the variability and highlight objects with non-Gaussian or burst-like behavior.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Upper panels: the KS vs. (J − KS); G vs. (BP − RP) color–magnitude diagrams with the YSOs of the Carina region overplotted. The magnitudes and colors are not corrected for the reddening and distance modulus. The color points are as follows. Red triangles: emission-line YSOs; blue squares: absorption-line YSOs; yellow circles: literature/Variable YSOs. Lower panels: Absolute magnitudes vs. corresponding dereddened colors in both systems. The colors and symbols are labeled.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Parallaxes (in Log scale), distances, and proper motions of the YSOs from Gaia DR3. The index numbers on the x-axis refer to the number of the star sorted by R.A. (C. Göppl & T. Preibisch 2022). The solid lines are the lineal and Gaussian fits plotted for illustration.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Upper panel: the StarHorse (left) and Gaia DR3 derived temperatures (right) of the YSOs. Middle panel: the StarHorse and Gaia DR3 derived [Fe/H] in dex. Lower panel: the StarHorse and Gaia DR3 derived masses. The colors and symbols are shown in the bar labels.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Left: the 2D t-SNE projection of the stellar spectra, colored according to their K-means cluster assignment. Right: the 2D t-SNE projection of the stellar spectra, colored according to the maximum flux value in the Br 11 spectral line. The colors and symbols are labeled.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Comparison of derived temperatures (in K) and metallicity from the value-added catalogs APOGEE Net, StarHorse, and AstroNN.
Paper: Young Stellar Objects in the Carina Nebula: Near-infrared Variability and Spectroscopy
Authors: Jura Borissova, Radostin Kurtev, Josemanuel Escobar, Javier Alonso-García, Nicolas Medina, Javier Osses, Zhen Guo, Philip W. Lucas, Michael Kuhn, Dante Minniti, Kevin R. Covey, Roberto K. Saito, Francisco Förster
Figure caption: Examples of the light curves of variable stars with KS amplitudes greater than 1.0 mag and emission in the Br 11 line.
Paper: An Efficient Method for Measuring the Color of a Natural Satellite with Astrometric Applications
Authors: X. Q. Fang, Q. Y. Peng, X. Lu, B. F. Guo
Figure caption: The responses of the Johnson–Cousins BVRI filters and the Gaia DR3 G, BP, and RP filters (source: https://svo2.cab.inta-csic.es/svo/theory/fps3/).
Paper: An Efficient Method for Measuring the Color of a Natural Satellite with Astrometric Applications
Authors: X. Q. Fang, Q. Y. Peng, X. Lu, B. F. Guo
Figure caption: Transformations from different instrumental color combinations to the Gaia standard color, using observations of NGC 2324 as an example. Each plot presents the results of a randomly selected pair of frames. For the BP − RP color, the b − i combination demonstrates smaller uncertainties compared to the others, while for the G − RP color, the c − i combination is preferred; refer to Table 2 for further details.
Paper: An Efficient Method for Measuring the Color of a Natural Satellite with Astrometric Applications
Authors: X. Q. Fang, Q. Y. Peng, X. Lu, B. F. Guo
Figure caption: The upper panels display example plots for estimating the object’s color using a pair frames. The bottom panels show the phased colors of all observations.
Paper: An Efficient Method for Measuring the Color of a Natural Satellite with Astrometric Applications
Authors: X. Q. Fang, Q. Y. Peng, X. Lu, B. F. Guo
Figure caption: Example plots of the DCR function used to correct the DCR effect. The curves derived from different nights exhibit subtle differences, and the zero point varies each night due to changes of the background reference stars.
Paper: An Efficient Method for Measuring the Color of a Natural Satellite with Astrometric Applications
Authors: X. Q. Fang, Q. Y. Peng, X. Lu, B. F. Guo
Figure caption: The (O − C) residuals before and after DCR correction using the estimated colors.
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: Phase-folded light curves from TESS. The data are binned in intervals of 2 minutes (gray) and 10 minutes (black). The solid blue line depicts the median posterior model, with light blue shading indicating the 1σ (68%) confidence interval.
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: Sensitivity curves (5σ contrast) for our targets from high-resolution imaging. The insets show the high-resolution images. Companions are seen near TOI-4051, TOI-4731, and TOI-5706.
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: J-band light curves from Palomar. The gray data points correspond to the unbinned data and the black data points correspond to data binned in 10 minutes intervals. The solid red line is the median model from the posterior distribution. The light red shading corresponds to the 1σ (68%) confidence interval. The solid blue curve shows the median TESS light curve projected into the J band by applying J band limb darkening coefficients.
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: Ground-based light curves from LCOGT, KeplerCam, and MuSCAT2. The colored data points correspond to the binned data at 5 minutes cadence. The solid black line is the median model from the posterior distribution. The solid blue curve is the median TESS light curve projected into the corresponding band.
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: Least-squares deconvolution profiles of the TRES stellar spectra of TOI-4731 showing the normalized line strength difference as a function of velocity. The velocity scale has been offset so that scattered moonlight occurs at 0 km s−1. The black line represents the observed profile, while the red line shows the best-fit model. The observations were taken on UT 2022-01-03, UT 2022-01-26, and UT 2022-03-09, corresponding to phases 31.7, 47.5, and 76.2, respectively, based on the TESS photometric ephemeris. Radial velocity measurements confirm that the primary peak remains stationary across all epochs (RV = 31.2, 30.2, and 30.7 km s−1 at phases 31.7, 47.5, and 76.2, respectively), while a secondary peak exhibits clear orbital motion: red-shifted at +50 km s−1 (phase 31.7), hidden behind the primary peak (phase 47.5), and blue-shifted at -50 km s−1 (phase 76.2). This phase-dependent spectroscopic behavior, combined with V-shaped transits, indicates a potential hierarchical triple system where an inner eclipsing binary (responsible for the moving secondary peak) orbits a much brighter tertiary star (responsible for the stationary primary peak).
Paper: Validation of TESS Planet Candidates with Multicolor Transit Photometry and TRICERATOPS+
Authors: Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Steven Giacalone, W. Garrett Levine, Morgan Saidel, Shreyas Vissapragada, David R. Ciardi, Karen A. Collins, David W. Latham, Cristilyn N. Watkins, Polina A. Budnikova, Dmitry V. Cheryasov, Akihiko Fukui, Allyson Bieryla, Avi Shporer, Benjamin M. Tofflemire, Catherine A. Clark, Chris Stockdale, Colin Littlefield, Emily Gilbert, Enric Palle, Eric Girardin, Felipe Murgas, Galen J. Bergsten, Hugh P. Osborn, Ian J. M. Crossfield, Jerome de Leon, Jesus Higuera, Keisuke Isogai, Mark E. Everett, Michael B. Lund, Norio Narita, Richard P. Schwarz, Roberto Zambelli, Steve B. Howell
Figure caption: The properties of the validated systems (stars) and possible planets with radii smaller than 8 R⊕ (circles) from our sample compared to the confirmed systems (gray circles) from the NASA Exoplanet Archive. The validated systems and possible planets are color-coded based on their insolation flux.