adsabs/AstroCLIMB huggingface dataset:
Paper: The Scorpion Planet Survey: Wide-orbit Giant Planets Around Young A-type Stars
Authors: Kevin Wagner, Dániel Apai, Markus Kasper, Melissa McClure, Massimo Robberto
Figure caption: Left: sensitivity of the Scorpion Planet Survey from Monte Carlo simulations. The contours identify the number of stars around which a planet of a given mass and semimajor axis would have resulted in a detection if they were uniformly present. Right: frequency vs. semimajor axis. The blue points show the measured frequency, whereas the vertical (black) uncertainty shows the 68% confidence interval. The blue ranges denote upper and lower 95% confidence values (i.e., their range denotes the 90% confidence interval). The horizontal bars represent the range of the semimajor axis bins. A power law of f ∝ a −1.7 is shown for comparison (i.e., not as a best fit). The vertical dotted line denotes the inner-most region (∼23 au) at which we would expect to have found ≥1 companion if they were uniformly present.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: Example of a broad Hα candidate (ID 1) whose estimated M BH is less than 106 M ⊙. The top panel shows the redshift-corrected spectrum with the best stellar continuum fit plotted in green. In the bottom panels, the first and third column show the best-fit model with an Hα broad component for each emission line region. The second and forth column show the best-fit model without an Hα broad component. The stellar continuum subtracted spectrum is plotted in black, and the blue line shows the best-fit model composed of narrow Gaussian components (magenta) and an Hα broad component (red). At the bottom of each panel, the residuals between the spectrum and the best-fit model are plotted in black. Spectra of the other 24 broad Hα candidates with estimated M BH < 106 M ⊙ are shown in the Appendix.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: Response function of the selected filters. As an example, the SDSS spectrum of ID1 is plotted (black) along with the kp1494 filter for obtaining the continuum flux (blue) and the kp1517 filter for Hα. The response function of three additional filters (kp1496, kp1497, and kp1498) are also presented. Note that depending on the redshift of each target, we used a different set of filters.
Paper: The Scorpion Planet Survey: Wide-orbit Giant Planets Around Young A-type Stars
Authors: Kevin Wagner, Dániel Apai, Markus Kasper, Melissa McClure, Massimo Robberto
Figure caption: Evolution of relative position angle vs. time of the background object near HD 131399A. The response to the foreground system’s (HD 131399's) greater parallax is most notably apparent in the 2017 and 2018 yr, which confirms this previous exoplanet candidate as a background contaminant.
Paper: The Scorpion Planet Survey: Wide-orbit Giant Planets Around Young A-type Stars
Authors: Kevin Wagner, Dániel Apai, Markus Kasper, Melissa McClure, Massimo Robberto
Figure caption: Left: sensitivity of the Scorpion Planet Survey in the K1 band for IRDIFS_Ext observations. Right: sensitivity in H2-band for IRDIFS observations. In both panels the thick black curve shows the median sensitivity, while the blue and red curves show the best and worst cases for background-limited sensitivity.
Paper: Search for Intermediate-mass Black Holes at Low Redshift with Intra-night Variability
Authors: Lael Shin, Jong-Hak Woo, Donghoon Son, Hojin Cho, Taewoo Kim, Elena Gallo, Wonseok Kang
Figure caption: Luminosity and velocity dispersion of the Hα broad component for the 131 broad Hα candidates. Slanted black lines are equi‐M BH lines. The red line is the selection criterion, 106 M ⊙, for the IMBH candidates.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption:  R NIR measurement as collected in Marcos-Arenal et al. (2021), as a function of the stellar luminosity. The dashed red line shows the expected dust sublimation radius for a temperature of 1500 K following previous work (Monnier & Millan-Gabet 2002; Dullemond & Monnier 2010; Lazareff et al. 2017). The solid orange line shows a moving mean of the measured R NIR values, and is used in the paper as an empirical estimate of R subl (Table 2).
Paper: ExoVista: A Suite of Planetary System Models for Exoplanet Studies
Authors: Christopher C. Stark
Figure caption: Illustration of the piece-wise analytic dust distribution model used for each disk component in generate_disks.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Same as Figure 5 but for spectra from the CRIRES survey (Section 2.1). Line stacks are shown in different colors for 12CO v = 1 − 0 J = 5–18 (black), v = 1 − 0 J = 25-31 (orange), v = 2 − 1 (purple), 13CO v = 1 − 0 (green). The high-J line stack is often missing due to the incomplete spectral coverage of CRIRES. Deviations from a flat continuum at the edges of some lines is due to contamination from nearby lines. The vertical dashed and dotted lines shows the stellar RV and its uncertainty. The measured line shape parameter S is reported at the top right in each plot.
Paper: ExoVista: A Suite of Planetary System Models for Exoplanet Studies
Authors: Christopher C. Stark
Figure caption: A sample of the variety of scattering phase functions produced by generate_disks (colored lines) compared to the best fit to Saturn’s D68 ringlet of Hedman & Stark (2015; black dashed line).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Overview of H I Pfund β line shapes observed in this survey. The stacked line profile of CO v = 1 − 0 lines is overplotted in red for reference.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Examples of full iSHELL spectra obtained in this survey. (The full sample of spectra is available for interactive visualization at www.spexodisks.com).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Plots of the three excitation tracers presented in Section 4.7, here shown against the stellar and accretion luminosity.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The analytically predicted, time-averaged cumulative distribution functions in period ratio for various systems. The parameter being varied is indicated by the color bar to the right of each plot, where the fiducial value is plotted in white for reference. The resonance location at ﹩\tfrac{5}{3}﹩ is indicated with a vertical dotted line. All the parameters affect the height and width of the peak, the most notable being the eccentricity of either planet, shown in panels (d) and (e).
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The analytically predicted cumulative distribution function in period ratio for the fiducial system. The time-averaged period ratio is shown in solid magenta, and a random period ratio from within the time period is shown in dashed magenta. The same distributions are shown for a comparable N-body simulation in cyan (solid is averaged and dashed is random). The black dashed line shows the initial flat period ratio distribution. The resonance location at ﹩\tfrac{5}{3}﹩ is indicated with a vertical dotted line. There is reasonable agreement between the numerical and analytical distributions, and in both cases, the peak at resonance only appears when the period ratios are averaged.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: For our generated planet pairs near the 3:1 resonance, we split the population into two halves. First, by the log of the mass ratio (log ﹩\tfrac{{m}_{1}+{m}_{2}}{{M}_{\star }}﹩), shown in the top panels as the combined eccentricity (a) and period ratio (b) distributions for these two halves of the population. In the bottom panels, we split the population into two halves by the combined eccentricity and show the log mass ratio (c) and period ratio (d) distributions for these two halves. While both mass and eccentricity affect the period ratio distribution, the time-averaged peak at resonance is still present even in the low-mass sample, but it disappears in the low-eccentricity sample, indicating the eccentricity is more strongly contributing to the effect.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The analytically predicted (a) probability density and (b) cumulative distribution of time-averaged period ratios near the 5:3 mean-motion resonance for three populations of Kepler-like planet pairs. Each population has a different Rayleigh scale for the planets’ individual eccentricities. The nominal resonance value is marked with a dotted line. As seen in the simulated data, there is a strong, very narrow peak associated with increased eccentricity.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: Comparison of the estimated fractional peak area of the (a) 3:1 and (b) 5:3 mean-motion resonances for a variety of eccentricity scales. The Kepler sample is in blue and the simulated combined Rayleigh distribution samples in black. The median values are plotted with the 1σ values as error bars. The Kepler sample is not consistent with the higher-eccentricity distributions, but is consistent with all those below a certain level, allowing for an upper limit constraint on the Kepler samples’ eccentricity distributions.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The subsamples (magenta) and corresponding median model (black) for two Rayleigh example eccentricity scales: the low-eccentricity σ = 0.05 for the (a) 3:1 and (b) 5:3 resonances, and the moderate-eccentricity σ = 0.25 for the (c) 3:1 and (c) 5:3 resonances. At low eccentricities, the distribution shows very little peak, while the peak appears more clearly as the eccentricity increases. Our model captures the behavior of the peak at various eccentricity scales.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The circularization timescale of the inner planet of our generated populations, scaled by Q. Based on a typical Q value of ∼100 for terrestrial planets, we expect that perhaps half of our sample may have undergone one tidal circularization timescale in 100 Myr, indicating that maintaining these planets at such high eccentricities may be difficult.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The probability of the Kepler planet pairs being part of an excess peak associated with 5:3 mean-motion resonance and not part of the background continuum of period ratios. All pairs with a nonzero median probability are plotted; see Table 3 for planet names and values.
Paper: Period Ratio Sculpting near Second-order Mean-motion Resonances
Authors: Nora Bailey, Gregory Gilbert, Daniel Fabrycky
Figure caption: The same as Figure 13, but for the 5:3 resonance.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: (a) Same as Figure 6(a), except that the time resolution is six data points per period. (b) Same as Figure 6(a), except that the time resolution is four data points per period. (c) Same as Figure 6(a), except that the time resolution is three data points per period.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: (a) Same as Figure 6(a), except that the S/N is 40. (b) Same as Figure 6(a), except that the S/N is 10.
Paper: Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Kyu-Ha Hwang, Weicheng Zang, Andrew Gould, Andrzej Udalski, Ian A. Bond, Hongjing Yang, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Radek Poleski, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Brandon Munford, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Hikaru Shoji, Stela Ishitani Silva, Takahiro Sumi, Daisuke Suzuki, Paul J. Tristram, Atsunori Yonehara, Xiangyu Zhang, Wei Zhu, Matthew T. Penny, Pascal Fouqué
Figure caption: Cumulative distribution of recovered and discovered KMT prime-field planets from 2018–2019 (black) compared to the mass-ratio function breaks proposed by Suzuki et al. (2016) and Jung et al. (2019b; magenta). The cyan dashed line simply connects the first and last KMT detections. If the underlying distribution of mass ratios (after multiplying by the detection efficiency) were uniform in ﹩\mathrm{log}q﹩, the cumulative distribution would approximately follow this line. The red event names at left indicate the mass ratios of the only known q < 2 × 10−4 planets from 2018–2019 nonprime fields. If no other such planets are found when the AnomalyFinder is applied to these fields, the cumulative distribution will be as shown in red.
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Summary of the transit ephemeris refinement analysis. Positive values of ΔBIC indicate mid-transit times that are disfavored relative to a nondetection. We consider mid-transit times with ΔBIC ≥ 10 (gray regions) to be ruled out by the ground-based photometry. Negative values of ΔBIC indicate times where the transit model provided a good fit. However, this could be coincidental, and we do not interpret a large negative ΔBIC as evidence of the transit. The 1σ and 3σ ranges for mid-transit time (T  C ) from the final ephemeris (Table 3) are shown as vertical lines. Each mid-transit time corresponds to a specific orbital period of TOI-2180 b, as indicated at the top of the figure.
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: The RV measurements of TOI-2180. Panel (a): RV time series after subtraction of an offset velocity from each data set. Transit windows are shown in green. Panel (b): residuals between the RV time series and best-fit planet model not including acceleration terms. A quadratic trend is visible on top of the Keplerian signal from TOI-2180 b. Panel (c): phase-folded RVs after removal of the acceleration terms. A phase of zero corresponds to conjunction (transit).
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Single transit of TOI-2180 b observed by TESS with short cadence. Top: unflattened PDCSAP flux and the trend from the Savitzky–Golay filter. Bottom: flattened light curve. The red points are individual exposures (gray points) binned by a factor of 40. The blue line shows the best-fit transit model.
Paper: The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 Day Orbit with the Automated Planet Finder Telescope 
Authors: Paul A. Dalba, Stephen R. Kane, Diana Dragomir, Steven Villanueva, Karen A. Collins, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Benjamin Fulton, Howard Isaacson, Judah Van Zandt, Andrew W. Howard, Daniel P. Thorngren, Steve B. Howell, Natalie M. Batalha, Ashley Chontos, Ian J. M. Crossfield, Courtney D. Dressing, Daniel Huber, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Casey L. Brinkman, Steven Giacalone, Michelle L. Hill, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Paul Benni, Pat Boyce, Thomas M. Esposito, E. Girardin, Didier Laloum, Pablo Lewin, Christopher R. Mann, Franck Marchis, Richard P. Schwarz, Gregor Srdoc, Jana Steuer, Thirupathi Sivarani, Athira Unni, Nora L. Eisner, Tara Fetherolf, Zhexing Li, Xinyu Yao, Joshua Pepper, George R. Ricker, Roland Vanderspek, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins, Christopher J. Burke, Jason D. Eastman, Michael B. Lund, David R. Rodriguez, Pamela Rowden, Eric B. Ting, Jesus Noel Villaseñor
Figure caption: Orbital period posterior for TOI-2180 b. The light blue shows the full posterior, while the dark blue shows the region that is still allowed after the transit ephemeris refinement using ground-based photometry, which rules out the most likely orbital periods (around the mean and median) inferred from the comprehensive EXOFASTv2 analysis.