adsabs/AstroCLIMB huggingface dataset:
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The panels in the left column show the relationships between the logarithmic mean flare energy and the rotation period for M-, K-, G-, and F-type dwarf stars. The panels on the right represent the logarithmic X-ray luminosity–rotation period relationships. The X-ray luminosities of our stellar samples are estimated from the data provided by S. Freund et al. (2022). The red and black dots represent stars with and without flare detections in this study, respectively. The vertical blue dashed lines pinpoint the transition turnoff values in terms of rotation period that separated the stars into saturated and unsaturated regimes. The red solid lines on the left panels represent the best-fit power-law slope of the flare energy–rotation period relationships in the unsaturated regimes. These values of transition turnoff periods and power-law slopes can be found in Section 6.3 and Table 12.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The period–V amp diagram of the short-cadence stars in TESS Sector 1. The red circles are the EBs identified by A. Prsa et al. (2022). For the stars with no valid rotation period in this study, we assigned to them a default period of 100 days for simplicity and ease of data handling. Note that this does not reflect the actual periods of the objects in question. The vertical and horizontal blue dashed lines represent the benchmarks of rotation period (P rot = 0.2 days) and variation amplitude index (V amp = 0.25), respectively. Based on these, the stars are divided into four quadrants (the numbers are highlighted in green color). Excluding EBs, approximately 95% of the stars are located in Quadrant IV. These stars are generally fitted well by our detrending method and are therefore the primary focus of this study.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: Distribution of star counts and flare star proportions by color index. All stars in this figure are Quadrant IV stars. The top panels show the total number of stars (gray) and flaring stars (orange) for each color index. The bottom panels illustrate the proportion of flaring stars with error bars. We identified 16,923 flare stars out of 371,511 main-sequence stars, indicating that about 4.6% exhibit flare activity. The proportion of flare stars increases with redder color indices, peaking at BP − RP values between 3 and 3.5, corresponding to spectral types M4 and M5. Beyond M5–M6, the proportion of flare stars decreases but then shows an increase at M7. Among giant stars, which include subgiants and red giants, approximately 0.7% (357 out of 50,347 stars) exhibit flaring activity.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The cumulative flare frequency distributions of M-, K-, G-, F-, and A-type dwarf stars. The shaded areas represent the deduced frequency uncertainties due to the detection incompleteness of small-amplitude events. The best-fit power-law indices (α) are not only highlighted with blue dashed lines but also listed in Table 11.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The color–magnitude diagram of flare star fractions. The horizontal axis represents the color index estimated from the Gaia BP and RP magnitudes. The vertical axis shows the absolute Gaia G magnitude. The gradation of colors, transitioning from a sparser distribution of yellow to a more concentrated region of dark blue, signifies the increasing fraction of stars with detected flaring phenomena in the TESS 2 minute survey from Sector 1 to Sector 72.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The relationships between these three flare parameters and the BP − RP color indices. The left panel illustrates that the maximum log flare energy tends to decrease with increasing BP − RP color index. The middle panel demonstrates that the maximum log flare amplitude increases as the BP − RP color index increases. The right panel shows that the maximum log flare duration does not display a strong trend with the BP − RP color index. The red points with error bars represent the binned averages and their corresponding standard deviations, highlighting the overall trends and variances within the data.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The log–log relationships between X-ray luminosity and mean flare luminosity for M-, K-, G-, and F-type dwarf stars. The red unfilled circles represent the stars in the saturated regimes, and the purple circles are the stars in the unsaturated regimes. The black dashed lines represent the best-fit slopes for stars in both saturated and unsaturated regimes. The yellow and blue dashed lines are the best-fit slopes for saturated and unsaturated stars, respectively.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: (a) The relationship between the calibrated flare duration and observed duration (Equation (16)). Panels (b) and (c) illustrate the factors for calibrating flare amplitude and energy as a function of observed duration, as given by Equation (17). The coefficients for the different light-curve noise levels are consolidated in Table 8.
Paper: Scalable, Advanced Machine Learning Based Approaches for Stellar Flare Identification: Application to TESS Short-cadence Data and Analysis of a New Flare Catalog
Authors: Chia-Lung Lin, Dániel Apai, Mark S. Giampapa, Wing-Huen Ip
Figure caption: The flares we detected in two hot subdwarfs, TIC 8901716 in Sector 48 (top panel) and TIC 11895653 in Sector 22 (bottom panel).
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: Gaussian kernel density estimations of TOI-3894's (left) and TOI-5301's (right) stellar mass and age posterior distributions from our EXOFASTv 2 global fits, illustrating a bimodal distribution in both parameters. The cyan dashed line indicates the median value of each parameter, while the shaded region represents the 68% confidence region. The normalized probability densities were estimated using the Gaussian kernel density estimator in the Python package scipy.stats. TOI-3894's fit slightly favored the lower-mass solution, with a probability of 53.0%, while TOI-5301's fit favored the higher-mass solution, with a probability of 78.3%.
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: Speckle high-resolution image and 5σ sensitivity curve from Gemini’s Zorro speckle imager. The observation reveals a source 79.°1 east of north and 0.″663 away from TOI-3321 that is 4.89 mag fainter in Zorro’s 832 nm narrowband filter.
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: Posterior pdf of TOI-1855 b’s radius. The black, labeled, vertical dashed line represents the posterior mode, 1.38R J. The cyan vertical dashed line and shaded region represent the median and 68% confidence interval, ﹩{1.65}_{-0.37}^{+0.52}﹩                      R J. The allowed planetary radius was constrained by an upper limit of 2.5R J.
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: AO images and sensitivity curves for TOI-3919 and TOI-5301. Top: Palomar PHARO AO image and 5σ sensitivity curve of TOI-3919 showing no detection of a companion star, down to the detection limits of the instrument. The magenta shaded region represents the uncertainty on the contrast curve. Bottom: Keck2 NIRC2 AO image and 5σ sensitivity curve of TOI-5232, showing a clear detection of a stellar companion at a separation of 1.″417 with Δmag = 2.952 in the Kcont filter.
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption:  TESS, follow-up, and archival observations of TOI-1855 as they compare to the EXOFASTv 2 results. Top left: unbinned TESS and follow-up ground-based transits, phase-folded and shown in comparison to the best-fit time of conjunction with an arbitrary normalized flux offset. Multiple TESS sectors in the same cadence are stacked on top of each other. Bottom left: the SED of the target star compared to the best-fit EXOFASTv 2 model. Residuals are shown on a linear scale, using the same units as the primary y-axis. Top right: RV observations vs. time, including any significant long-term trend. The residuals are shown in the subpanel below in the same units. Middle right: RV observations phase-folded using the best-fit ephemeris from the EXOFASTv 2 global fit. The phase is shifted so that the transit occurs at Phase + Offset = 0. The residuals are shown in the subpanel below in the same units. Bottom right: the evolutionary track and current evolutionary stage of the planet according to the best-fit MIST model. The blue line indicates the best-fit MIST track, while the black contours show the 1σ and 2σ constraints on the star’s current T eff and log g from the MIST isochrone alone. The green contours represent the 1σ and 2σ constraints on the star’s T eff and log g from the EXOFASTv 2 global fit, combining constraints from observations of the star and planet. The red plus sign indicates the median and 68% confidence interval reported in Table 6.
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: Eccentricity and semimajor-axis distribution of the planets discovered in this work, compared to giant planets in the literature and several avenues and outcomes of giant planet migration (similar to Figure 4 in Dawson & Johnson 2018). The region labeled “Stellar Collision” corresponds to a giant planet colliding with the star, assuming that the star is 1 R ⊙ in size. The region labeled “Tidal Disruption” corresponds to a Jupiter-like planet falling within the Roche limit of the Sun. Finally, the red region corresponds to the tidal circularization of a highly eccentric giant planet around a Sun-like star. The blue circles represent the EXOFASTv 2 median semimajor axis and eccentricity of the planets in this work, while the gray circles represent substellar bodies discovered by TESS with masses between 0.25M J and 13M J and reported eccentricities, obtained from the NASA Exoplanet Archive. Many of the eccentric planets, including those that fall outside of the three shaded regions, can be explained by planet–planet scattering that has not yet or will not be tidally circularized. The equations that describe each of these shaded regions are shown in Dawson & Johnson (2018).
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: Same as Figure 6, but for TOI-5301. Similarly to Figure 10, TOI-5301 had a bimodal distribution of possible stellar masses, and we therefore represent the median and standard deviation of either solution in the bottom right panel.
Paper: Migration and Evolution of giant ExoPlanets (MEEP). I. Nine Newly Confirmed Hot Jupiters from the TESS Mission
Authors: Jack Schulte, Joseph E. Rodriguez, Allyson Bieryla, Samuel N. Quinn, Karen A. Collins, Samuel W. Yee, Andrew C. Nine, Melinda Soares-Furtado, David W. Latham, Jason D. Eastman, Khalid Barkaoui, David R. Ciardi, Diana Dragomir, Mark E. Everett, Steven Giacalone, Ismael Mireles, Felipe Murgas, Norio Narita, Avi Shporer, Ivan A. Strakhov, Stephanie Striegel, Martin Vaňko, Noah Vowell, Gavin Wang, Carl Ziegler, Michael Bellaver, Paul Benni, Serge Bergeron, Henri M. J. Boffin, César Briceño, Catherine A. Clark, Kevin I. Collins, Jerome P. de Leon, Courtney D. Dressing, Phil Evans, Emma Esparza-Borges, Jeremy Fedewa, Akihiko Fukui, Tianjun Gan, Ivan S. Gerasimov, Joel D. Hartman, Holden Gill, Michaël Gillon, Keith Horne, Ferran Grau Horta, Steve B. Howell, Keisuke Isogai, Emmanuël Jehin, Jon M. Jenkins, Raine Karjalainen, John F. Kielkopf, Kathryn V. Lester, Colin Littlefield, Michael B. Lund, Andrew W. Mann, Mason McCormack, Edward J. Michaels, Shane Painter, Enric Palle, Hannu Parviainen, David-Michael Peterson, Francisco J. Pozuelos, Zachary Raup, Phillip Reed, Howard M. Relles, George R. Ricker, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Gregor Srdoc, Chris Stockdale, Hannah Sullivan, Mathilde Timmermans, Joshua N. Winn
Figure caption: Same as Figure 6, but for TOI-3894. TOI-3894's EXOFASTv 2 global fit was bimodal in stellar mass and age. To represent both modes, we show median values and standard deviations from each stellar mass solution in the bottom right panel.