adsabs/AstroCLIMB huggingface dataset:
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: Examples of hypothetical spot distributions with ∼40% spot coverage and ∼1.4% rotational variability in the TESS bandpass. The left panel provides an example of densely filled latitudinal spot bands in which overdensities of spots lead to rotational variability and apparent spot-crossing events, while the right shows large, nonvariable polar spots with a few additional spots that produce the variability and occasional spot-crossing event. The region occulted by HD 189733 b is outlined by dotted white lines in both panels. Made with spotter (Garcia & Rackham 2023).
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: All posterior parameters from the 2comp model sampling derived from the forward and reverse scan data sets of the 2013 June 5 (orange), 2013 June 24 (gray), and 2022 June 21 (blue) HST observations of HD 189733 A. Both the forward and reverse scan data sets retrieve similar parameter distributions, discussed in Section 4. Here, we see that the retrievals on the distance (D star) and stellar radius (R star) are precise across all data sets. Conversely, there is a discrepancy on the parameter posteriors on the error terms, most obvious with distribution of  a scale from the forward 2013 June 5 data set.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: 2comp posterior parameters inferred from the model sampling derived from the forward and reverse scan data sets of the 2013 June 5 (orange), 2013 June 24 (gray), and 2022 June 21 (blue) HST observations of HD 189733 A. Both the forward and reverse scan data sets retrieve similar parameter distributions, discussed in Section 4. These corner plots compromise the model parameters used to describe the best-fit model data, summarized in Table 4.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: The TESS 120 s light curve of HD 189733 A. TESS data from Sectors 41 and 54 (black) are shown alongside five examples of rotational light curves produced with fleck (gray) for spot radii of 0.05 R  s . The blue bar gives the maximum peak-to-peak amplitude of the observed rotational modulation. We stress that the aim of this analysis is not to fit the evolving light curve entirely but to constrain probabilistically the spot properties consistent with the maximum TESS rotational amplitude. Transits of HD 189733 b have been masked.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: All posterior parameters from the 2comp model sampling derived from the forward and reverse scan data sets of the 2013 June 5 (orange), 2013 June 24 (gray), and 2022 June 21 (blue) HST observations of HD 189733 A, using the (left) PHOENIX and (right) MPS-ATLAS/SPHINX (Witzke et al. 2021; Kostogryz et al. 2023; Iyer et al. 2023) spectral models. Utilizing different spectral grids gives confidence that the parameter retrieval is independent of stellar model.
Paper: Axisymmetric High Spot Coverage on Exoplanet Host HD 189733 A
Authors: Isaac S. Narrett, Benjamin V. Rackham, Julien de Wit
Figure caption: Maximum spot coverage consistent with HD 189733 A's peak-to-peak variability of 1.4% in TESS data as a function of spot radius. Median (points) and 68% confidence intervals (error bars) are shown for the spot coverage of the whole disk and transit chord. Points are offset along the x-axis for clarity.
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Dynamical maps of the second-derivative-based index shown in the ﹩(\dot{\theta },\alpha )﹩ space for the configurations with orbital eccentricities at e = 0.01 (left-hand panel) and e = 0.02 (right-hand panel). The index shown in the color bar corresponds to the base 10 logarithm of the normalized second-derivative-based index ∣∣ΔD∣∣ (to make the structures distinguishable, the index ∣∣ΔD∣∣ is limited in the interval [10,10000]). In both panels, the main V-shape structures are visible. Compared to the maps of FLI shown in Figure 1, minute structures can be visibly observed, especially in the region on the left-hand side of the V-shape structure. Poincaré sections corresponding to the cases of α = 0.35 and α = 0.65 are presented in Figure 3.
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Dynamical maps of the FLI shown in the ﹩(\dot{\theta },\alpha )﹩ space for the configurations with orbital eccentricities at e = 0.01 (left-hand panel) and e = 0.02 (right-hand panel). The index shown in the color bar corresponds to the base 10 logarithm of FLI. In both panels, the main V-shape structures are visible. The red-dashed lines stand for the locations of α = 0.35 and α = 0.65 and their associated Poincaré sections are shown in Figure 3.
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Nominal location of the centers of high-order and secondary resonances determined under the Kernel Hamiltonian model together with the Poincaré surfaces of section for spin–orbit problems with asphericity parameters at α = 0.35 (left-hand panel) and α = 0.65 (right-hand panel). Nominal locations of high-order and secondary resonances are determined by Equation (14). The eccentricity is taken as e = 0.01. The red-dashed lines stand for the dynamical separatrix of the synchronous primary resonance, specified by Equation (10). The primary resonance happens inside the region bounded by the dynamical separatrices.
Paper: Dynamical Structures Associated with High-Order and Secondary Resonances in the Spin–Orbit Problem
Authors: Hanlun Lei
Figure caption: Nominal locations of high-order and secondary spin–orbit resonances determined under the Kernel Hamiltonian model shown in the ﹩(\dot{\theta },\alpha )﹩ space (left-hand panel) and comparisons to dynamical maps of the second-derivative-based index in the case of e = 0.01 (right-hand panel). The map shown in the right-hand panel is the same as that presented in the left-hand panel of Figure 2. In the left-hand panel, the shaded region stands for the parameter space where the synchronous primary resonance happens. Those resonances inside the primary resonance are called secondary resonances and those outside the primary resonance are referred to as high-order spin–orbit resonances.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The observed population of Jupiter Trojans in the MPC catalog as of 2023 February represented using the distribution of the A, B, and C orbital parameters: L4 cloud on top, L5 cloud at the bottom. As to their definition, see Equations (1), (2), and (3). The red lines are approximate fits of the background population using the simple few-parametric functions in Equations (6), (7), and (8), avoiding the contribution of the major families. In particular, we used: α 1 = 1, α 2 = 1.3 and s A = 0.095 for the inclination distribution, β 1 = 0.87, β 2 = 1.75 and s B = 0.04 for the eccentricity distribution, and γ = 1 and s C = 0.045 in the L4 population, and α 1 = 1.2, α 2 = 1.6 and s A = 0.15 for the inclination distribution, β 1 = 0.85, β 2 = 1.6 and s B = 0.038 for the eccentricity distribution, and γ = 1 and s C = 0.045 in the L5 population. The most prominent Trojan families contribute to the total population with specific values of the proper elements. As usual, they are most noticeable in the inclination distribution (left panel; the Thronium family was formerly called 1996 RJ). The population in Eurybates family accounts for more than 10% of the observed population in L4. The Ennomos/Deiphobus clan (see the Appendix) may represent a slightly smaller share among the L5 Trojans.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The same as in Figure 15, but now the cumulative rather than differential distribution is shown. The principal Trojan families are also shown: (i) Eurybates (green), Hektor (cyan), Arkesilaos (magenta), Thronium (yellow) in the L4 population, and (ii) Ennomos/Deiphobus clan in the L5 population. Eurybates has the largest population with 875 known members, followed by Arkesilaos with 235 known members (see Table 4). Even at magnitude 14.5 these two families represent compositely ≃12% of the total L4 population. Furthermore, the magnitude distribution is much steeper (see the dashed gray extrapolation), and their population may reach up to 25–30% of the total population at magnitudes 16.5–17 if continued with a straight power law. The Ennomos/Deiphobus is equally abundant among the L5 population: at magnitude ≃14.25, their population represents ≃10% of the total, and this fraction increases toward a larger magnitude.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Results of a numerical experiment probing stability of Trojan orbits in the L4 cloud. Orbits of 28 clone variants were started in different bins in the C vs. B plane (i.e., librations amplitude vs. eccentricity), with four different fixed values of A (i.e., inclination) given by the label. Residence in the libration zone about the L4 stationary point was monitored throughout the simulation, reaching 100 Myr period of time. All orbits in the white cells are stable, and all orbits in the black cells are unstable (i.e., escaped from the Trojan region within the integration). The gray bins were found partially stable, and the scale of grayness is linearly proportional to the number of clone orbits that escaped. The stability limit is shown by the red dashed line connecting the first bins with 50% partial instability for the given B value. The blue symbols show the known Trojan population within the ±0.05 value of A referred to as the nominal value.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The observed population of Jupiter Trojans in the MPC catalog as of 2023 February represented by 2D projections in the A, B, and C orbital parameters: (i) A vs. C (left), (ii) B vs. C (middle), and (iii) A vs. B (right). The top panels are for the L4 cloud, and the bottom panels are for the L5 cloud. Two distinct features are worth noting: (i) correlation between C and B in the middle panels (such that larger B requires smaller C), which is the expression of orbital stability constraint, and (ii) orbital clusters, most distinctly seen in the A vs. B plane in the right panels (see also Figure 9 in Vinogradova 2015, 2019). The gray line in the middle panels approximates the stability limit (we improve this guess by a direct numerical experiment in Figures 12 and 13). The latter are the Trojan families, collections of fragments from the collisional disruption of parent bodies. Curiously, the L4 cloud shows clear evidence of nine families, starting with the best-known Eurybates case (e.g., Brož & Rozehnal 2011; Rozehnal et al. 2016; Marschall et al. 2022). The families in L5, while also existing, seem to be blurred by either higher ejection velocities, dynamical diffusion at their particular location, or some other effect.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Detection probability ﹩{ \mathcal P }(A,B,C;H)﹩ of the L4 (left panels) and L5 (right panels) population Trojans in a specific set of the orbital bins centered about B = 0.055 and C = 1.605 values: various curves for a full range of values of the A parameter from 0 to 0.7 (the upper curves for the smallest A value, progressing to the lowest curve for the largest A values). The abscissa is the absolute magnitude H. The top panels are for phase I of the CSS operations, and the bottom panels are for phase II of the CSS operations (Section 2). The five major Trojan L4 and L5 families are intersected by the chosen string of bins at different values of A (i.e., orbital inclination). The respective detection probability curves are color-highlighted: (i) Eurybates centered at A ≃ 0.125 and Arkesilaos at A ≃ 0.15 (both represented in red, L4), (ii) Hektor at A ≃ 0.325 (green, L4), (iii) Thronium at A ≃ 0.525 (magenta, L4), and (iv) Ennomos/Deiphobus at A ≃ 0.475 (red, L5). Bins/families at higher inclinations have progressively smaller detection probability. For instance, at magnitude 14.75, the detection probability spread from the smallest to the largest inclination bins in the L4 population is ≃0.4 to ≃0.72 (phase II) and ≃0.12 to ≃0.65 (phase I). Detection probability in phase I and high-inclination bins are systematically much lower, not reaching unity even for large Trojans (small H values). A more subtle effect concerns phase II, in which the detection probability for the same bins in the L5 swarm levels off the unity earlier by about 0.3 mag.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Differential magnitude distribution of Trojan populations (bin width 0.25 mag): (i) left is the complete count (L4 and L5 together), (ii) middle is the L4 cloud, and (iii) right is the L5 cloud. The black line is the population in the MPC database, the blue line is detections by CSS during phase I, and the red line is detections by CSS during phase II. The dashed gray curve on the right panel reproduces the MPC L4 population for the sake of comparison. We find it curious that the L5 population has nearly empty two bins centered at ≃9.5 mag: there are 46 L4 objects with H < 10 vs. 26 L5 objects with H < 10. While this may be an effect of a small number of statistics, the paucity of the L5 continues beyond magnitude 11.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Detection probability ﹩\bar{{ \mathcal P }}(H)﹩ of the L4 (red curve) and L5 (blue curve) population Trojans averaged over all orbital bins. Two variants of weighting defined in Equation (31) are shown: (i) a uniform weight w = 1 (dashed lines), and (ii) a weight based on Equations (6)–(8) (solid lines). The abscissa is the absolute magnitude H. The left panel is for phase I of the CSS operations, and the right panel is for phase II of the CSS operations (Section 2). The vertical dashed line at 13.7 mag in the right panel is an approximate formal completeness limit. This limit is not reached during phase I because of its shorter timespan and fields of view pointing near the ecliptic (thus missing a fraction of high-inclination Trojans).
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The same is in Figure 12, but now for the L5 Trojan population.
Paper: Orbital and Absolute Magnitude Distribution of Jupiter Trojans
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Comparison of the stability limits for Trojan orbits in the C vs. B plane determined by our numerical experiment spanning 100 Myr. Different curves for seven different values of A are labeled and identified by color. The upper panel is for L4 Trojans, and the bottom panel is for L5 Trojans; for the sake of comparison, we transformed B → − B in this panel. There is no difference in the orbital stability for L4 and L5 clouds (see also Robutel & Gabern 2006; Di Sisto et al. 2014).
Paper: Detection of an Atmospheric Outflow from the Young Hot Saturn TOI-1268b
Authors: Jorge Pérez-González, Michael Greklek-McKeon, Shreyas Vissapragada, Morgan Saidel, Heather A. Knutson, Dion Linssen, Antonija Oklopčić
Figure caption: Mass vs. orbital period for the population of transiting exoplanets with fractional mass uncertainties smaller 30%. The Neptune desert boundaries from Mazeh et al. (2016) are overplotted as dashed lines. Planets orbiting stars with 4000 K  <  T eff  <  5400 K are the most favorable targets for 1083 nm metastable helium observations; these systems are outlined in red. The seven planets with previously published Palomar/WIRC helium measurements tabulated in Vissapragada et al. (2022) and TOI-1268b are outlined in blue. Gray shading indicates the magnitude of each star, and the point size is proportional to the logarithm of the predicted signal-to-noise ratio in the WIRC helium bandpass. Figure adapted from Vissapragada et al. (2022).
Paper: Detection of an Atmospheric Outflow from the Young Hot Saturn TOI-1268b
Authors: Jorge Pérez-González, Michael Greklek-McKeon, Shreyas Vissapragada, Morgan Saidel, Heather A. Knutson, Dion Linssen, Antonija Oklopčić
Figure caption: Combined constraint on the mass-loss rate and temperature. The orange dark and light areas are 1σ and 2σ contours from the temperature constrained profile. The blue dark and light areas are the best-fit models, 1σ and 2σ contours of the mass-loss-rate profiles. The 1σ contour of joint constraint is shown in black. The 1σ constraints of simulations ran at three times and one third of the EUV flux are shown in gray.
Paper: Detection of an Atmospheric Outflow from the Young Hot Saturn TOI-1268b
Authors: Jorge Pérez-González, Michael Greklek-McKeon, Shreyas Vissapragada, Morgan Saidel, Heather A. Knutson, Dion Linssen, Antonija Oklopčić
Figure caption: Left: combined WIRC light curve for TOI-1268b including data from both Palomar nights, with circle markers for night 1 and triangle markers for night 2. The blue curve is the best-fit transit model with the radius ratio from the TESS bandpass, and the red curve is the best-fit transit model with the radius ratio in the WIRC helium bandpass, with the 1σ uncertainty in the transit depth shown as light red shading. Right:   TESS data with the joint WIRC+TESS model showed in blue. Unbinned photometry is shown in gray, while black points are binned to 5 minutes.
Paper: Detection of an Atmospheric Outflow from the Young Hot Saturn TOI-1268b
Authors: Jorge Pérez-González, Michael Greklek-McKeon, Shreyas Vissapragada, Morgan Saidel, Heather A. Knutson, Dion Linssen, Antonija Oklopčić
Figure caption: Allan deviation plot for the joint WIRC+TESS fit. The black points indicate the root-mean-square error of the binned residuals for each light curve, solid red line indicates the expected noise from photon noise statistics and the dashed red line indicates the photon noise scaled up the root-mean-square error of the binned residuals.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Similar to Figure 9. The local conditions for sliding window are represented by Range. magred, R 2 red and σ red. σ red represents the standard deviation of local residuals. The red bar graph highlights the areas with the poorest local goodness of fit (R 2).
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Targets with a period greater than 1.2 days are excluded. The blue dots indicate the original light curve, the orange lines indicate the interpolated curves, and the green dots indicate the reconstructed light curves.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Similar to Figure 10. The light curves of contact binary candidates can be reconstructed well.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: The examples of 10 candidate objects of contact binary stars that are not present in catalog obtained by Prša et al. (2022).
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: The period, goodness of fit(R 2), and temperature distributions are shown.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Light curves of other types cannot be reconstructed well. The blue dots indicate the original light curve, the orange lines indicate the interpolated curves, and the green dots indicate the reconstructed light curves.
Paper: Detection of Contact Binary Candidates Observed By TESS Using the Autoencoder Neural Network
Authors: Xu Ding, ZhiMing Song, ChuanJun Wang, KaiFan Ji
Figure caption: Left: the blue dots are the light curve with time-flux observed by TESS. Right: Similar to Figures 8 and 9, the blue dots indicate the original light curve, the orange lines indicate the interpolated curves, and the green dots indicate the reconstructed light curves.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Corner plots (left: unscattered input; middle: combination of five independently scattered inputs) from the EXPLOR (black) and the TAUREX (blue) retrievals obtained for the 1D (i.e., spatially homogeneous atmosphere) JWST eclipse examples, and retrieved T–p structure (right) for the unscattered case. In the scattered case the final posteriors are obtained by adding the resampled weighted traces from the five different scattered instances. In the T–p plot, the solid lines and shaded regions are the median and 1σ and 3σ regions, respectively, while the dashed lines are the true values from the forward model. Widening of the posteriors and the retrieved T–p profiles for the TAUREX retrievals, even when the maps are unscattered, shows the effect of information dilution arising from the reduction process. In the scattered case, the TAUREX solutions are less stable to the noise properties, most likely due to incorrect propagation of non-Gaussian components arising during the reduction process.
Paper: Toward Atmospheric Retrievals of Panchromatic Light Curves: EXPLOR-ing Generalized Inversion Techniques for Transiting Exoplanets with JWST and Ariel
Authors: Q. Changeat, Y. Ito, A. F. Al-Refaie, K. H. Yip, T. Lueftinger
Figure caption: Observed spectra obtained when the EXPLOR simulations are reduced using POP (data points), and best-fit spectra (solid lines) from corresponding 1D TAUREX 3 retrievals. The reduction was performed on simulated eclipses of WASP-43 b that are similar to Scenario 1 (the raw data shown in Figure B1). The black case corresponds to an unscattered spectro-temporal flux map, while the colored cases are five different instances of scattered spectro-temporal flux maps. Note that the spectra are offset for better clarity. Overall the 1D TAUREX 3 retrievals are able to explain the data.