adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: The SED fit to TOI-3984 A. Red points are the measurements from broadband photometry, while blue points represent the MIST model flux. The horizontal bars represent the width for each filter. A NextGen BT-SETTL model (Allard et al. 2012) is overlaid for reference as a gray line and smoothed for clarity as a black line. The BT-SETTL model is not used as part of the SED fit.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 3 but displaying the ground-based photometry for TOI-3984 A. Panels (a)−(f) are the light curves from RBO, Soka, and ARCTIC plotted with model posteriors (shaded regions) from the joint fit to the photometry and RVs.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: The 5σ contrast curves for TOI-3984 A obtained from speckle imaging with NESSI in the Sloan ﹩{z}^{{\prime} }﹩ filter. The data reveal no bright companions at separations of 0.″2–1.″75. The inset is the 4.″7 × 4.″7 NESSI speckle image centered on TOI-3984 A in the Sloan ﹩{z}^{{\prime} }﹩ filter.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 8 but for TOI-5293 A. Panel (a) shows the HPF RVs. Panel (b) displays the phase-folded RVs plotted with model posteriors.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 6 but for TOI-5293 A. Shown is the 5σ contrast curve for TOI-5293 A obtained from speckle imaging using NESSI along with an inset displaying the 4.″7 × 4.″7 reconstructed speckle image in the Sloan ﹩{z}^{{\prime} }﹩ filter.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 12 but for TOI-5293 A.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Panel (a) displays the ZTF photometry for TOI-3984 A in each filter along with the best-fitting Gaussian process model for reference. Panels (b) and (c) are the GLS periodograms for the zr and zg photometry from ZTF. An FAP of 0.01% (following Zechmeister & Kürster 2009) is shown for reference. Panel (d) presents the ground-based ZTF photometry from panel (a) phased to the derived rotation period. The large black points represent 4 day bins of the phased photometry. Panel (e) presents the posterior distribution of the rotation period from the Gaussian process model. The derived rotation period is ﹩{50.0}_{-2.7}^{+2.8}﹩ days.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 14 but for TOI-5293 A. Panel (a) displays the ZTF photometry along with the best-fitting Gaussian process model for reference. Panel (b) presents the GLS periodogram for the ZTF data. Panel (c) presents the phased ground-based ZTF photometry, with large black points representing 2 day bins. Panel (d) presents the posterior distribution of the rotation period. The derived rotation period is ﹩{20.6}_{-0.4}^{+0.3}﹩ days.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Nominal position of TIC 1101522311, the white dwarf companion to TOI-3984 A, on the color–magnitude diagram for white dwarfs identified in Gaia EDR3 by Gentile Fusillo et al. (2021). Contours for fixed masses from Bédard et al. (2020) are plotted for reference. The best-matching cooling track from the models is shown with a dashed line.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: A tour of the relevant photometry of the star V1298 Tau. Panel (a): detailed view of the K2 photometry (purple points), with a beating envelope overplotted in solid pink. The beating envelope is drawn to illustrate the effect of spot beating on the overall variability amplitude, not to fit the data precisely. The envelope drawn is constructed from the beating of three sinusoids at 2.70, 2.85, and 3.00 days. Signatures of beating can be seen by eye: two peaks of different amplitudes phase up toward the end of the K2 baseline, producing a single-peaked variability pattern and a larger overall variability amplitude. Panel (b): detailed view of the TESS photometry (purple points). Beating characteristics are also visible, although the baseline is shorter than that of K2. Panels (c), (d), and (e): relative views of K2, LCO, and TESS photometry, emphasizing the relative temporal baselines and variability amplitudes. A typical error bar for each data set is also shown in the bottom left corner of each panel. The differences in wavelength coverage and flux dilution between the K2, LCO, and TESS photometry largely account for the overall differences in amplitude of the signals. Both the K2 and TESS data cover less than one complete beat period of the two largest-amplitude periodic signals, but the LCO photometry (which is contemporaneous with the RVs of SM21) covers a longer temporal baseline. Panel (e): all photometry, plotted on the same panel to emphasize the relative time elapsed between each data set. Takeaway: differential rotation effects are visible by eye in both the K2 and TESS data sets.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: Smoothed activity-only component of the preferred model of SM21, together with the Keplerian model components. Top: 100 random draws from the posterior describing the planet b Keplerian are also shown, to illustrate that this effect holds true across the posterior, and not simply for one point estimate. The light gray solid line shows the full activity-only model component, and the darker gray shows this model averaged over a (randomly chosen) 11.2 day timescale. (Note that the same pattern holds when choosing a slightly different smoothing timescale; i.e., this is not a result of aliasing.) Shaded gray regions indicate where there are observations. Bottom: same as the top, but with a zoomed-in y-axis. Takeaways: the activity-only component changes suddenly in windows of time where there are observations. When the activity-only component is averaged over shorter-timescale variations, the GP contributes to the fit on timescales similar to the Keplerians, even interfering destructively at some times. This casts doubt on the reality of the Keplerian signals reported in SM21, indicating that they may be favored because of overfitting.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: Demonstration of the impact of constructing separate covariance matrices and adding the log(likelihoods). Compare with Figure 12. The data and best-fit parameters are for K2-131, published in Dai et al. (2017), for demonstration purposes only. Top: GP mean prediction (black solid line) and 1σ uncertainties (purple filled), together with the HARPS-N data points on which the GP is conditioned (purple points). Middle: same as the top, but for PFS data. Bottom: residuals with respect to the GP mean prediction. Takeaway: when separate covariance matrices for each RV instrument are used, contemporaneous data are uncorrelated in the model, allowing additional degrees of freedom.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: Lomb–Scargle periodograms of the photometric data shown in Figure 9. Top: zoom in on the presumed rotation period, showing several nearby peaks in all three data sets. Bottom: same as the top over a wider period range. Takeaway: multiple closely related periodicities are visible in Fourier space for all three photometric data sets, providing more evidence for differentially rotating active regions.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: Same as Figure 11 (in particular, using the exact same data and GP hyperparameters), but here a single covariance matrix is constructed, following the suggestion in Section 4.1. Takeaway: constructing a single covariance matrix requires that GP predictions for separate instruments are scalar multiples of one another, which is more consistent with physical expectations and results in a more constrained model than one with a separate covariance matrix for each instrument.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: HARPS-N RVs and contemporaneous LCO photometry from SM21, phase folded to the rotation period and colored by observation time. Top: LCO photometry. Bottom: HARPS-N RVs, with fitted jitter values from the preferred SM21 fit added to the error bars. One- and two-component sinusoidal fits are also shown. Takeaway: the presence of a strong periodogram peak at P rot/2 results from the higher-order shape of the RV rotation pattern. This pattern is not present in the LCO photometry, which is approximately sinusoidal over the rotation period.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: Lomb–Scargle periodogram of all RV data presented in SM21, and two-component sinusoidal fit passed through the same window function. Top: periodogram of all RVs (solid purple line) and a two-component sinusoidal fit to the data (filled gray). Middle/bottom: same, but zoomed in. The rotation period, its harmonic, and its 1 day aliases are labeled. Takeaway: the dominant Lomb–Scargle periodogram structure can be explained as harmonics and aliases of a single period at 2.91 days.
Paper: Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Sarah Blunt, Adolfo Carvalho, Trevor J. David, Charles Beichman, Jon K. Zink, Eric Gaidos, Aida Behmard, Luke G. Bouma, Devin Cody, Fei Dai, Daniel Foreman-Mackey, Sam Grunblatt, Andrew W. Howard, Molly Kosiarek, Heather A. Knutson, Ryan A. Rubenzahl, Corey Beard, Ashley Chontos, Steven Giacalone, Teruyuki Hirano, Marshall C. Johnson, Jack Lubin, Joseph M. Akana Murphy, Erik A Petigura, Judah Van Zandt, Lauren Weiss
Figure caption: Another visualization of Figure 4. Same as Figure 3, except computed using the same method as for Figure 4. Takeaway: the larger and more uniform spread of residuals for the HARPS-N data on which the model was conditioned provides more evidence that the preferred SM21 model is overfitting.
Paper: Orbital Alignment of the Eccentric Warm Jupiter TOI-677 b
Authors: Elyar Sedaghati, Andrés Jordán, Rafael Brahm, Diego J. Muñoz, Cristobal Petrovich, Melissa J. Hobson
Figure caption: (a) Altitude of the target star TOI-677 during the night of observations, with the duration of ESPRESSO exposures highlighted in red and the full transit in cyan. The numbers in the plot represent the angular separation of the target and the moon at each instance. (b) The variations of image quality delivered at the detector and corrected for the airmass. (c) The median spectral S/N values in the echelle orders recorded by the blue and red detectors. (d) Variations of the ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ activity index, indicative of the chromospheric contributions of the H and K Calcium lines, excluding the photospheric component. The shaded regions present the 1σ uncertainty, estimated by the ESPRESSO pipeline. (e) The variations of the Hα index, calculated for the wider 1.6 Å central bandpass, with the shaded region again representing the 1σ uncertainty (Gomes da Silva et al. 2011). The two red arrows indicate the times at which variation in the index coincides with the systematic noise in the RVs, resulting in deviations from the expected RM effect (see Figure 2).
Paper: Orbital Alignment of the Eccentric Warm Jupiter TOI-677 b
Authors: Elyar Sedaghati, Andrés Jordán, Rafael Brahm, Diego J. Muñoz, Cristobal Petrovich, Melissa J. Hobson
Figure caption: Top: radial velocity measurements of TOI-677 during the primary transit of TOI-677 b, demonstrating the RM effect, presented as circles including error bars. Note that neither the systemic velocity nor the underlying orbital reflex motion have been removed and have been included as parameters in the modeling process. The blue line represents the best-fit analytical model ﹩{ \mathcal M }(t)﹩, including an RM and RV component, and the red line is this same model, which also includes the GP noise model component. The dark and light gray shaded regions represent the 1 and 3σ uncertainties of this model, respectively. The orange line shows the variations of the Hα 1.6 index, where the units have not been included (see bottom panel of Figure 1). This represents the free regressor used to model the covariance matrix. Bottom: the residuals of both models, where colors have been chosen according to the corresponding model.
Paper: Orbital Alignment of the Eccentric Warm Jupiter TOI-677 b
Authors: Elyar Sedaghati, Andrés Jordán, Rafael Brahm, Diego J. Muñoz, Cristobal Petrovich, Melissa J. Hobson
Figure caption: Sample of all currently measured absolute sky-projected obliquity angles λ for exoplanets as a function of semimajor axes. The colors of the data points represent the eccentricity of each system, and the sizes are indicative of planetary radius. The data point representing TOI-677 b is highlighted with a thick red border and text, while all warm planets on misaligned orbits have been annotated in black. Values used for this plot are compiled from the TEPCat (Southworth 2011) database.
Paper: Orbital Alignment of the Eccentric Warm Jupiter TOI-677 b
Authors: Elyar Sedaghati, Andrés Jordán, Rafael Brahm, Diego J. Muñoz, Cristobal Petrovich, Melissa J. Hobson
Figure caption: Top: TOI-677 RV data from all the different instruments used for measurement. The solid black line represents the best-fit model where the eccentricity is taken as a free parameter. The posteriors of this fit are given in blue in bottom part of Figure 5. The smaller panel below shows the residuals of this fit. Bottom: the same as the top, but with a model fit with the eccentricity fixed to 0. In all panels, zooms have been made into the regions of dense data for better demonstration of the model precision. For both cases, the log evidence is annotated at the top left corner.
Paper: Orbital Alignment of the Eccentric Warm Jupiter TOI-677 b
Authors: Elyar Sedaghati, Andrés Jordán, Rafael Brahm, Diego J. Muñoz, Cristobal Petrovich, Melissa J. Hobson
Figure caption: Top: posterior probability distributions from the Nested Sampling algorithm, for the fitted orbital parameters of the possible outer companion to TOI-677 b. The blue plot (bottom left) is for the fit with eccentricity taken as a free parameter, and the red plot (top right) for a circular orbit fit. For each posterior probability distribution, the median and the upper and lower 68th percentile confidence intervals are given as solutions and plotted as dashed lines.
Paper: Orbital Alignment of the Eccentric Warm Jupiter TOI-677 b
Authors: Elyar Sedaghati, Andrés Jordán, Rafael Brahm, Diego J. Muñoz, Cristobal Petrovich, Melissa J. Hobson
Figure caption: Joint and singular posterior probability distributions for some of the fitted parameters of the GP model ﹩{ \mathcal M }(t)﹩ fitted to the ESPRESSO transit RV data of TOI-677 b. The different colors represent the three independent MCMC simulations, where the lines show the 1, 2 and 3σ levels of the joint distributions. At the top of each column, the median and the 16th/84th quartiles of the combined distributions are given as the final best-fit solution for each parameter, with the full results for all the parameters given in Table 2.