adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Mass vs. radius diagram showing confirmed planets with masses and radii measured to >3σ precision (black points) and TOI-1751 b (orange). Each panel includes different theoretical composition curves from Zeng et al. (2019). Earth (E), Venus (V), Uranus (U), and Neptune (N) are also shown for context, with the precise masses and radii for these planets lying in the center of the letter symbol. TOI-1751 b is consistent with both rocky and water-rich models. Left: the Earth-like composition is assumed to be 32.5% Fe/Ni-metal plus 67.5% MgSiO3-rock. Curves for 100% H2O and 100% MgSiO3 are also shown. Middle: composition curves assuming an Earth-like planet with the addition of an H2/He atmosphere (made up of a mixture of 75% H2 and 25% He). These curves are evaluated along interior adiabats at different internal specific entropies, labeled by the temperature of the corresponding specific entropy at 100 bar level in the gas envelope (2000 K is sparsely dashed, 1000 K is solid, 700 K is dashed, 500 K is dotted, 300 K is thin solid). Right: composition curves correspond to an Earth-like planet with an H/Heisothermal envelope at various surface temperatures atop an ice-VII (a cubic crystalline form of ice) layer.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Top: RV measurements from APF (blue diamonds) and HIRES (green squares) and the best-fit (median) RV model (orange line) from the joint RV and transit analysis. For clarity, the RV offset for each instrument has been subtracted from the data, and the respective jitter terms have been combined with the instrumental uncertainties to produce the error bars. The orange-shaded region shows the 68% confidence range for the model. Middle: phase-folded radial velocities of TOI-1751 b, with the instrumental offsets and linear trend removed. The APF data (blue triangles) and HIRES data (green squares) are shown with error bars and the best-fit (median) RV model for the planet (orange line). The jitter term for each instrument has been added to the RV uncertainty in quadrature to calculate the error bars. The orange-shaded region indicates the model's 68% confidence range. For clarity, repeated orbital phase coverage is shown in the gray-shaded regions, and we have also binned the data to ∼4 day intervals (white circles with error bars). Bottom: residual radial velocities between the best-fit (median) model and the data.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Mass vs. radius posterior samples from the joint transit and RV fit for TOI-1751 b modeled with MAGRATHEA. Left: models of TOI-1751 b assuming an Earth-like rock/iron ratio, no atmosphere (i.e., AMF = 0%), a supercritical and condensed water layer, and a water envelope. By allowing the planet’s envelope to be made of water, the WMF required to reproduce the planet’s radius is substantially reduced. Gray Xs mark mass and radius samples which are too low density to be modeled with AMF = 0%. Right: models of TOI-1751 b assuming an Earth-like mantle/core ratio, a WMF of 20%, and a non-ideal H/He atmosphere. The non-ideal atmosphere is less compressible than an ideal H/He envelope, and thus a smaller AMF is needed to reproduce the measured planet radius. Isocomposition curves for WMF and AMF are shown with dashed lines.
Paper: Binary Black Hole Mergers and Intermediate-mass Black Holes in Dense Star Clusters with Collisional Runaways
Authors: Rujuta A. Purohit, Giacomo Fragione, Frederic A. Rasio, Grayson C. Petter, Ryan C. Hickox
Figure caption: Solid lines: most massive BH formed in a cluster as a function of the initial cluster mass M CL  for different values of the fraction of cluster mass that undergoes initial collisional runaway, f run. The half-mass–radius is fixed at r h = 1 pc representative of the typical size of young massive clusters. Dashed lines: initial IMBH mass, m run = f run M CL, as a function of M CL. The simulations contain three metallicities as Z ∈ {0.02, 0.002, 0.0002}.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Top: phase-folded TESS light curve of TOI-1751 b. The black points with error bars show the flattened PDCSAP flux from 13 transits, where the error bars are calculated by adding the jitter and instrument uncertainty in quadrature. The orange line shows the best-fit (median) transit model from the joint RV and transit analysis. For clarity, the data are also shown in 1 hr bins (white circles). Bottom: residual flux between the best-fit (median) transit model and the data.
Paper: Binary Black Hole Mergers and Intermediate-mass Black Holes in Dense Star Clusters with Collisional Runaways
Authors: Rujuta A. Purohit, Giacomo Fragione, Frederic A. Rasio, Grayson C. Petter, Ryan C. Hickox
Figure caption: The growth of IMBHs (ratio of its mass to the initial mass) in clusters with initial cluster mass M CL = 106 M ⊙ as a function of time for different values of f run. For clusters with higher values of f run, the ratio does not increase significantly, while IMBHs in clusters with smaller values of f run  grow significantly over time.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Posterior probability distributions for the joint RV and transit fit parameters for TOI-1751 b. The orange lines indicate the median value of the sample distribution, and the dashed black lines indicate a 68% interquantile range.
Paper: The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System
Authors: Anmol Desai, Emma V. Turtelboom, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M. Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn
Figure caption: Auxiliary posterior distributions for the joint RV and transit fit parameters for TOI-1751 b. The orange lines indicate the median value of the sample distribution, and the dashed black lines indicate a 68% interquantile range.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Heat map of recall rates of the Random Forest classifier for the synthetic planetary injections as a function of injected period and radius bins.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Effective S/N of the injected planetary signals. (Left) Comparison of the effective S/N (based on IQR rather than standard deviation) of the injected planetary transit to the effective S/N of the best transit from TCF. The injected planetary signals that were used in the training set are plotted as purple triangles, while injected signals whose period was not recovered by the TCF are gray triangles. Light curves whose TCF peak periods were unaffected by the injected planetary signal are plotted in turquoise. The dashed orange lines show approximate lower bounds of injected planets used in the training set. (Right) Fraction of injected planetary signals that were recovered given the spread of effective S/N of the best transit from TCF.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Comparison of the synthetic orbital parameters that were injected into random light curves for the positive (purple triangles) and negative (orange points) training sets with the orbital parameters from the best TCF transit model. Injected FPs were used supplement the negative training set and only represent about half of the negative training set (see Section 4.2). The top panel shows the distribution of injected orbital parameters, and the bottom panel shows the distribution of the best orbital parameters from TCF analysis. Smooth contours are plotted on both panels to aid the eye in seeing the underlying distribution.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Recall rates by the Random Forest classifier for 1,042 previously identified planet candidates from various surveys. (Top) Heat map as a function of planet radius and orbital period found with TCF. (Bottom) Candidate planets from various surveys superposed on the DTARPS-S heat map for injected planets from Figure 17. Gold squares are recovered objects and black points are not recovered.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Two sources of contamination that affect the DTARPS-S Analysis List of potential planetary transits. (Left) TCF Periodogram and folded ARIMAX residual light curve of TIC 254214344 that shows an unconvincing peak in the TCF periodogram with no clear transit in the folded light curve. (Right) Random Forest prediction score for the full set of DIAmante-extracted light curves showing clusters of stars subject to ephemeris matching and periodic satellite operations as red points.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Recall rates by the DTARPS-S RF classifier for 364 M20 DIAmante candidates. (Top) Heat map as a function of planet radius and orbital period found with TCF. The colors give the recall rate, and the numbers are the number of M20 candidates in each period–radius bin. (Bottom) Candidate planets from M20 superposed on the DTARPS-S heat map for injected planets from Figure 17. Blue diamonds are recovered objects, and black points are not recovered.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Recall rates by the Random Forest classifier for 202 Confirmed Planets in the NASA Exoplanet Archive (NASA Exoplanet Science Institute 2022). (Top) Heat map as a function of planet radius and orbital period found with TCF. (Bottom) Confirmed planets from the NASA Exoplanet Archive superposed on the DTARPS-S heat map for injected planets from Figure 17. Red circles are recovered objects and black points are not recovered.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Specificity of DTARPS-S RF classifier for 513 previously identified False Positives. A red colored bin represents a high percentage of False Positives with correct classification as a non-planetary signal. The numbers of False Positives in each bin are labeled.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Radius–Period plots of the injected planets (Section 4.1) colored by the recall rate for the injected planet, given only the injected transit TCF signal S/Neff for TESS with three different hypothetical observational durations: one month, one year, and four years. Green indicates a high recall rate for the injected planet, and yellow indicates a low recall rate for the injected planet.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Outcome of simulations organized by mass and initial mutual inclination between TOI 4633c and the binary orbit. We show 600 MERCURY integrations run for 106 yr each across three scenarios indicated by the labels on the figures: (1) without the 34 days planet, (2) where TOI 4633b has initial inclination of ∼88° narrowly avoiding transit and is coplanar with TOI 4633c, and (3) where TOI 4633b is coplanar with the binary orbit. The x-axis is the initial mutual inclination set between TOI 4633c and the binary orbit, and the y-axis is the average eccentricity of TOI 4633c during the final 10% of the integration time. Each simulation is represented by a point–blue for runs that remain stable and red for unstable.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Planet mass vs. planet orbital period for all systems with masses measured to 30% or better uncertainty. We have highlighted planets around bright stars in color. Within the bright star sample, we distinguish between single-planet systems (orange circles) and systems with more than one planet (purple squares). TOI 4633 c is the second longest-period planet in a bright host star system (however, we do note that planet c does not have a mass measured to 30% or better uncertainty). Furthermore, both planets in the system are fairly high mass and likely not rocky, which is unusual compared to the confirmed population of multi-planet systems.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Planet radius vs. planet mass for all confirmed planets listed in the NASA exoplanet archive with a mass measurement with 30% uncertainty or better. Bright systems (m  V  < 10) are highlighted with a black outline. TOI 4633 c is shown by the blue triangle, where uncertainties correspond to our radial velocity fit. Although the existence of a second star in this system means that the radial velocity amplitude is diluted and thus the true planet mass may be larger, the lack of planets with the radius of TOI 4633 c at masses larger than 47 M ⊕ suggests that the planet is unlikely to be significantly more massive than what is reported here.
Paper: Planet Hunters TESS. V. A Planetary System Around a Binary Star, Including a Mini-Neptune in the Habitable Zone
Authors: Nora L. Eisner, Samuel K. Grunblatt, Oscar Barragán, Thea H. Faridani, Chris Lintott, Suzanne Aigrain, Cole Johnston, Ian R. Mason, Keivan G. Stassun, Megan Bedell, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Guillaume Hebrard, David W. Hogg, Steve B. Howell, Baptiste Klein, Joe Llama, Joshua N. Winn, Lily L. Zhao, Joseph M. Akana Murphy, Corey Beard, Casey L. Brinkman, Ashley Chontos, Pia Cortes-Zuleta, Xavier Delfosse, Steven Giacalone, Emily A. Gilbert, Neda Heidari, Rae Holcomb, Jon M. Jenkins, Flavien Kiefer, Jack Lubin, Eder Martioli, Alex S. Polanski, Nicholas Saunders, Sara Seager, Avi Shporer, Dakotah Tyler, Judah Van Zandt, Safaa Alhassan, Daval J. Amratlal, Lais I. Antonel, Simon L. S. Bentzen, Milton K. D Bosch, David Bundy, Itayi Chitsiga, Jérôme F. Delaunay, Xavier Doisy, Richard Ferstenou, Mark Fynø, James M. Geary, Gerry Haynaly, Pete Hermes, Marc Huten, Sam Lee, Paul Metcalfe, Garry J. Pennell, Joanna Puszkarska, Thomas Schäfer, Lisa Stiller, Christopher Tanner, Allan Tarr, Andrew Wilkinson
Figure caption: Stellar effective temperature vs. effective incident flux on a planet. The boundaries of the habitable zone defined by Kopparapu et al. (2014) are illustrated as shaded regions. The black circles show all transiting exoplanets listed in the NASA exoplanet archive, where the filled circles show only planets that have a mass measurement to better than 30% accuracy. The orange triangle shows the properties of TOI 4633 c. There are no other transiting planets within the habitable zone that are brighter than 11th magnitude, and only four that are brighter than 13th magnitude.