adsabs/AstroCLIMB huggingface dataset:
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: Comparison of CV distances obtained from Gaia DR3 and Bailer-Jones et al. (2021) (d BJ). Different apparent G-band magnitude intervals are shown in panels (a), (b), (c), and (d). The red line represents the one-to-one line and the blue dashed lines 500 and 1000 pc distances from the red line.
Paper: Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Authors: Remziye Canbay, Selçuk Bilir, Aykut Özdönmez, Tansel Ak
Figure caption: Distance histogram of CVs in the sample, which is limited using bright and faint limiting magnitudes in the G band. The relative distance errors ﹩{\sigma }_{{d}_{\mathrm{BJ}}}/{d}_{\mathrm{BJ}}﹩ are also shown in the lowest panel.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: Top: EWHα  time series for three of the stars observed with the UCLES spectrograph, offset vertically from one another for ease of viewing. Similar long-term behavior is present in each of these three data sets, suggesting that the cause is not stellar but rather instrumental or environmental. Bottom: stacked periodograms from six stars with at least 100 UCLES Hα measurements spread over the majority of the instrument’s ∼6000 days observational baseline, where no significant signals were detected by RVSearch. The long-term structure seen in the top panel emerges as two humps in this composite periodogram, one at UCLES’ observing baseline (6000 days), and another at half that (3000 days). The impact of the monthly lunar cycle is also evident via a narrow peak at 29.5 days. We therefore treat Hα periods detected around any of these three periods with some degree of caution.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: HR diagram containing the target stars in this study. The dashed blue lines are MIST V1.2 evolutionary tracks from Choi et al. (2016) covering masses 0.7–1.4 M ⊙ over an age range 100 Myr–14 Gyr. The tracks adopt a protosolar mix (initial Y = 0.2703, Z = 0.0142857, [α/Fe] = 0, v/v crit = 0). The Sun is depicted using the ⊙ symbol.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: Stars identified by the EPRV Working Group as potential targets for future DI missions such as HabEx and LUVOIR that would aim to detect and characterize Earth-analog exoplanets. This work focuses primarily on the stars located in the Southern hemisphere.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: Comparison of the uncertainties in previously published works and our updated RV analyses for the planets listed in Table 5 for orbital period (top plot), RV semiamplitude (middle plot), and orbital eccentricity (bottom plot). The gray dashed lines depict a 1:1 ratio, so planets above the line have more-precise results in our analysis while planets below the line have less-precise results here than previously published. The green lines denote a factor of 2 improvement, so planets above the green lines have uncertainties that decreased by 50%. This happens most commonly in the orbital period comparisons, as the additional months/years of data added here include many more orbits of each planet.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: Fifty percent detection sensitivity threshold for each target star at its Earth equivalent irradiation distance (EEID)—the distance from the host star at which the planet will receive the same amount of energy as the Earth receives from the Sun. For the majority of targets, the existing Doppler sets are not yet sensitive to Neptune-mass planets at their respective EEIDs, which would preclude the formation of stable Earth analogs, let alone Earth-mass planets themselves.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: Moving periodogram (MP) for the combined HD 85512 RV data sets. The colors encode the scaled MP power, which is truncated to optimize the visualization of signals. The previously reported 58.43 day planet is visible as a dark-red horizontal band on the left side of the MP, denoting its significance in the first half of the RV time series, but bifurcates and then disappears in later years. A second signal at P ≃ 51 days takes over in the latter half of the time series, but does not exhibit a tight enough period range to be seriously considered as a planet candidate.
Paper: Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions  
Authors: Katherine Laliotis, Jennifer A. Burt, Eric E. Mamajek, Zhexing Li, Volker Perdelwitz, Jinglin Zhao, R. Paul Butler, Bradford Holden, Lee Rosenthal, B. J. Fulton, Fabo Feng, Stephen R. Kane, Jeremy Bailey, Brad Carter, Jeffrey D. Crane, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Gregory Laughlin, Stephen A. Shectman, Johanna K. Teske, C. G. Tinney, Steven S. Vogt, Sharon Xuesong Wang, Robert A. Wittenmyer
Figure caption: Planet, Candidate, or SRC planetary irradiation relative to Earth (S/S ⊕) vs. M sin i (M ⊕). The habitable zone for an Earth analog in a solar-analog system (Kopparapu et al. 2014) is marked in the blue shaded region.
Paper: Magnetic Fields in the Horsehead Nebula
Authors: Jihye Hwang, Kate Pattle, Harriet Parsons, Mallory Go, Jongsoo Kim
Figure caption: Magnetic field vectors overlaid on a two-color composite of HST imaging in two broadband filters, F110W (YJ) and F160W (H), centered at 1153.4 and 1536.9 nm, respectively, taken from the Mikulski Archive for Space Telescopes (MAST) (https://archive.stsci.edu/prepds/heritage/horsehead/). Black and orange segments show magnetic field orientations inferred from JCMT POL-2 850 μm measurements (this work) and Palomar Observatory r-band measurements centered at ∼7200 Å (Zaritsky et al. 1987), respectively. It should be noted that the image is rotated with respect to standard equatorial coordinates.
Paper: Magnetic Fields in the Horsehead Nebula
Authors: Jihye Hwang, Kate Pattle, Harriet Parsons, Mallory Go, Jongsoo Kim
Figure caption: Map of SCUBA-2/POL-2 850 μm intensity in the Horsehead Nebula. Magnetic field orientations are shown as red, blue, and green segments, which were obtained using the JCMT (this work), the Palomar Observatory (Zaritsky et al. 1987), and Planck (Planck Collaboration et al. 2015), respectively. The orange contour level marks a total intensity of 9 mJy beam−1. The circle in the lower right corner shows the JCMT beam size of 14.″1 at 850 μm.
Paper: Magnetic Fields in the Horsehead Nebula
Authors: Jihye Hwang, Kate Pattle, Harriet Parsons, Mallory Go, Jongsoo Kim
Figure caption: Magnetic field orientations obtained using the JCMT (this work), Planck (Planck Collaboration et al. 2015), and Palomar (Zaritsky et al. 1987). Gray and red bars show magnetic field orientations obtained using the JCMT in SMM1 and SMM2, respectively. The magnetic field orientations obtained in SMM2 are approximately parallel to those obtained using Planck. Overall, the magnetic field orientations obtained using Palomar are shifted about 20° compared to those obtained using Planck. The JCMT POL-2 histograms are shown over the angle range 0°–180° E of N, while the Planck and Palomar histograms are shown over the range 180°–360°. Due to the ±180° ambiguity in polarization vector measurements, this range is identical to the range 0°–180°, and so opposite angles on the plot agree. In Cartesian space, the area of each histogram is normalized to 1; it should be noted that the projection onto a circle means that their areas are distorted.
Paper: Magnetic Fields in the Horsehead Nebula
Authors: Jihye Hwang, Kate Pattle, Harriet Parsons, Mallory Go, Jongsoo Kim
Figure caption: Map of C18O velocity dispersion in the Horsehead Nebula. The contours show SCUBA-2 850 μm flux densities of 9, 100, and 150 mJy beam−1. The circle in the lower right-hand corner shows the JCMT beam size of 14.″1 at 850 μm.
Paper: Magnetic Fields in the Horsehead Nebula
Authors: Jihye Hwang, Kate Pattle, Harriet Parsons, Mallory Go, Jongsoo Kim
Figure caption: Angular dispersion functions measured in SMM1 (left) and SMM2 (right). Blue lines show the quadratic function fitted to the angular dispersion function. The fitted b and m values are shown in the left upper corners of each panel. Note that b is here given in degrees for ease of interpretation.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: The top panel shows the TLS power spectra of the detrended TESS FFI light-curve data of TOI-2525. The planetary transit signal of the more massive planet c is detected at P  c  = 49.24 days. The bottom panel shows the TLS power spectra of the residuals, which reveal the transit signal of the inner, less massive planet at P  b = 23.3 days. The remaining TLS peaks are harmonics and subharmonics of the transit signals. Horizontal dashed lines indicate signal detection efficiency (Hippke et al. 2019) power levels of 5.7, 7.0, and 8.3, which correspond to TLS false-positive rates of 10%, 1%, and 0.1%.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: The RV component of the two-planet dynamical model of TOI-2525, constructed jointly with the TTV data and the RVs from PFS (blue circles). The two RVs from FEROS (red triangles) are overplotted with an optimized RV offset to the model. The left panel shows the time series and the N-body model, and the middle and right panels show a phase-folded representation of the RV data modeled with the dynamical model (with an osculating period). The PFS data uncertainties include the estimated RV jitter added in quadrature to the error budget, while the FEROS data are plotted with their nominal RV uncertainties. The small subpanels show the RV residuals.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Target pixel file image of TOI-2525 in the FFIs of TESS sectors 1, 3–11, and 13. The central (red) borders in the pixel space are the ones used to construct the TESSERACT photometry. Gaia targets are marked with red circles, whose size has been coded by their G magnitude.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: TESS light-curve data and model of the TOI-2525 transit signals, plotted with arbitrary vertical offsets. The left panel shows the transit signal of the inner planet TOI-2525 b and its strong TTV variation, whereas the right panel shows the same for the outer, more massive Jovian planet TOI-2525c. The x-axis of the curves for TOI-2525 b is t n-1333.5070mod23.2915 days, and for TOI-2525c is t n-1335.4101mod49.2424 days.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: The TTVs of TOI-2525 b (blue) and TOI-2525 c (red), fitted with a two-planet dynamical model jointly with the RVs from PFS. The top panels show the TTV time series and best-fit model for each planet, whereas the bottom panels show the TTV residuals.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Posteriors of the dynamical properties at the 2:1 period ratio commensurability of the two-planet system TOI-2525. The posteriors are generated by randomly drawing 10,000 samples from the TTV+RV dynamical model. Each sample is tested for stability, and the overall dynamical properties are evaluated at the 2:1 period ratio commensurability. The derived dynamical parameters are the mean period ratio ﹩{\hat{P}}_{\mathrm{rat}.}﹩; mean eccentricities ﹩{\hat{e}}_{{\rm{b}}}﹩ and ﹩{\hat{e}}_{{\rm{c}}}﹩; mean orbital alignment ﹩{\rm{\Delta }}\hat{\omega }﹩; peak-to-peak amplitudes ampl. e b, ampl. e c, and ampl. Δω; and the planetary dynamical masses and semimajor axes. Note that the posterior distributions of θ 1 and θ 2 are not shown, since these exhibit circulation between 0° and 360°. The black contours on the 2D panels represent the 1σ, 2σ, and 3σ confidence level of the overall posterior samples.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: The top panels are the same as in Figure 7 but for the evolution of the apsidal angle Δω = ω b − ω c and the trajectory evolution as a function of e  b  e  c  times the sine/cosine of Δω, respectively. The trajectory just misses the origin (red dot, centered at [0,0]), which leads to libration of Δω with a semiamplitude of ∼80°. The bottom panels are the same as the top panels but for a random posterior fit that exhibits circulation of Δω (see Figure 6). The trajectory evolution in this case passes through the origin, which leads to brief episodes of circulation of Δω.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Orbital evolution of the TOI-2525 system for a 1000 yr long N-body integration using the Wisdom–Holman scheme. The left panel shows the evolution of the planetary periods, the middle panel shows the eccentricities e b (blue) and e c (red) of the best-fit N-body model, and the right panel shows the evolution of the line-of-sight inclinations i b (blue) and i c (red).