adsabs/AstroCLIMB huggingface dataset:
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: TESS light curves of TOI 2589. Dashed vertical lines indicate the transits that were identified.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: Evolution curves of the planetary radius as a function of time color-coded by the water mass fraction of the envelope. The points correspond to the current properties of each planet.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: Planet radius vs. orbital period diagram for the population of transiting giant planets, color-coded by planet mass. The size of the circles scales with the transit spectroscopy metric (TSM; Kempton et al. 2018). The three systems presented in this study stand out owing to their relatively long periods.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: Contrast curve of TOI 2589 obtained with the Speckle imaging facility HRCam at SOAR. The image inset shows the faint companion star (marked with a white arrow). The additional feature above the star is the same companion mirrored in the autocorrelation function, a product of the speckle image reduction.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: Radial velocities of TOI 4406 as a function of the orbital phase of TOI 4406b (FEROS: blue; Coralie: yellow; CHIRON: black; HARPS: orange). The solid line corresponds to the Keplerian model using the posterior parameters of the joint fit.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: Radial velocities of TOI 2589 as a function of the orbital phase of TOI 2589b (FEROS: blue; CHIRON: black; HARPS: orange; CORALIE: yellow). The solid line corresponds to the Keplerian model using the posterior parameters of the joint fit.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: Radial velocities of TOI 2338 as a function of the orbital phase of TOI 2338b (FEROS: blue; HARPS: orange). The solid line corresponds to the Keplerian model using the posterior parameters of the joint fit.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: All photometric transits of TOI 2338b as a function of orbital phase obtained with TESS and ground-based facilities. No detrending was performed on the ground-based light curves, which generates a negative slope in the residuals of LCO-SAAO.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: All photometric transits of TOI 4406b as a function of orbital phase obtained with TESS and ground-based facilities. Residuals are presented in the right panel.
Paper: Three Long-period Transiting Giant Planets from TESS 
Authors: Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François Bouchy, Adrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas
Figure caption: All photometric transits of TOI 2589b as a function of orbital phase obtained with TESS and ground-based facilities.
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Age–radius diagram for all planets smaller than Jupiter, younger than 5 Gyr, and with radius and age uncertainties both smaller than 25%. The data point color corresponds to the planet density for planets with mass uncertainties smaller than 25%. Data collected from the NASA Exoplanet Archive (accessed 2023 Mar 22; NASA Exoplanet Science Institute 2020). K2-136b, c, and d are labeled in red to the left of the planet symbol. There are only four planets in this figure with a stellar age younger than K2-136 and a mass measurement better than 25%: AU Mic b and c (stellar age = 22 ± 3 Myr; Mamajek & Bell 2014) and Kepler-411 b and c (stellar age = 212 ± 31 Myr; Sun et al. 2019). The only other plotted planet <1 Gyr with a mass measurement is the open cluster planet K2-25b (Stefansson et al. 2020), which is slightly larger than K2-136c.
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Scatter plots of S  HK , BIS, and FWHM against the RV for the K2-136 system. All HARPS-N and ESPRESSO data have been separately offset shifted according to the median model offsets listed in Table 4. Blue data points correspond to HARPS-N observations, orange data points to ESPRESSO. In the top-left corner of each subplot is the Spearman correlation coefficient, which can capture nonlinear, monotonic correlations. (The coefficients were calculated with data values but not uncertainties.)
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: X-ray spectra of K2-136 from the XMM pn (left panel), MOS1 (center), and MOS2 (right) EPIC cameras. X-ray counts are binned by 20 in the pn camera, and 15 in the MOS cameras. The orange lines are the best fits using a one-temperature APEC model and assuming a fixed neutral hydrogen column density of 5.5 × 1018 cm−2, typical for Hyads (see Section 4.9.2). The residuals of each fit are shown in the bottom panels. The best-fit parameters are presented in Table 6.
Paper: Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass
Authors: Andrew W. Mayo, Courtney D. Dressing, Andrew Vanderburg, Charles D. Fortenbach, Florian Lienhard, Luca Malavolta, Annelies Mortier, Alejandro Núñez, Tyler Richey-Yowell, Emma V. Turtelboom, Aldo S. Bonomo, David W. Latham, Mercedes López-Morales, Evgenya Shkolnik, Alessandro Sozzetti, Marcel A. Agüeros, Luca Borsato, David Charbonneau, Rosario Cosentino, Stephanie T. Douglas, Xavier Dumusque, Adriano Ghedina, Rose Gibson, Valentina Granata, Avet Harutyunyan, R. D. Haywood, Gaia Lacedelli, Vania Lorenzi, Antonio Magazzù, A. F. Martinez Fiorenzano, Giuseppina Micela, Emilio Molinari, Marco Montalto, Domenico Nardiello, Valerio Nascimbeni, Isabella Pagano, Giampaolo Piotto, Lorenzo Pino, Ennio Poretti, Gaetano Scandariato, Stephane Udry, Lars A. Buchhave
Figure caption: Simulation of JWST transmission spectra for K2-136c using JET (Fortenbach & Dressing 2020). The top and bottom panels correspond to the NIRISS SOSS-Or1 (0.81–2.81 μm) instrument, and the NIRSpec G395M (2.87–5.18 μm) instrument, respectively. The gray line in both panels is the modeled atmospheric spectrum assuming low metallicity (5x solar) and no clouds, while the blue data points are the simulated instrument spectra for one observed transit with NIRISS SOSS, and two observed transits with NIRSpec G395M, including the effects of photon noise, and instrument systematics.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Impact parameters for TOI-216 b in blue and TOI-216 c in pink, with shaded regions marking 68% and 95% of fitted models. A negative impact parameter is used as TOI-216 b crosses over the face of the star to the opposite side relative to TOI-216 c. The light gray shaded region marks a grazing transit for TOI-216 b, the dark gray region indicates the planet has stopped transiting entirely. TOI-216 b will fully transit for over 200 yr, TOI-216 c is always fully transiting.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Measured impact parameters from the light curve fitting alone for each transit of TOI-216 c are shown as black points, following the approach of Dawson (2020). The spread of dynamical models fit to the data is shown in pink, the shaded regions mark 68% and 95% of n-body simulations. The individual transit impact parameters have highly correlated measurement uncertainties. The impact parameter for TOI-216 c has no significant change over the TESS observation baseline.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: The mutual angle between the orbital planes of TOI-216 b and c with shaded regions marking 68% and 95% of fitted models. The changes in mutual inclination are primarily due to changes in the sky-plane inclination of the two planets, reaching minima where the impact parameters coincide.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Eccentricity variation for TOI-216 b (blue) and c (pink) over a 150 yr period based on the maximum-likelihood dynamical model of the system. The left panel highlights a shorter period of time to show a 1500 day long periodicity in the eccentricity of b. The right panel shows a more slowly varying 8900 day period in eccentricity.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Transit-timing variations for TOI-216 b (blue) and c (pink) over a 150 yr period based on the maximum-likelihood dynamical model of the system. The left panels highlight a shorter period of time to show a 1500 day long periodicity in TTVs. The right panel shows a more slowly varying 8900 day period in transit times.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: The trajectory of the maximum-likelihood dynamical model showing the libration of angles around a fixed point for TOI-216 b (blue), and the circulating nature of TOI-216 c (pink).
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: The amplitude of TTV oscillations for planets in known TTV systems against the average orbital period of the planet. TOI-216 b is marked in blue, TOI-216 c is marked in pink.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Measured impact parameters from the light curve fitting alone for each transit of TOI-216 b are shown as black points. The spread of dynamical models fit to the data is shown in blue, while the shaded regions mark 68% and 95% of n-body simulations. The light gray region indicates a grazing transit. The impact parameter for TOI-216 b has changed from grazing to fully transiting over the TESS observing baseline.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Observed TTVs for TOI-216 b (blue) and c (pink) shown as points. Error bars for b (∼3 minutes) and c (∼1 minute) are too small to be seen at this scale. Narrow shaded regions indicate 68% and 95% credible intervals of fitted models. The TTVs are anticorrelated with TOI-216 b having a larger amplitude due to its lower mass and higher eccentricity. The TTVs change quasisinusoidally over a period of ∼1500 days.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Light curves of TOI-216 b divided between year 1 (left) and year 3 onward (right) of TESS observations, phase aligned to the center of the transit. The best fitting model is shown in black for each individual transit. Binned data for each time interval is shown as white points.
Paper: Transit Depth Variations Reveal TOI-216 b to be a Super-puff
Authors: Brendan J. McKee, Benjamin T. Montet
Figure caption: Light curves of TOI-216 c divided between year 1 (left) and year 3 onward (right) of TESS observations, phase aligned to the center of the transit. The best fitting model is shown in black for each individual transit. Binned data for each time interval is shown as white points.