adsabs/AstroCLIMB huggingface dataset:
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: Radius, eccentricity, and semimajor axis evolution for several possible cases of TOI-1420b’s tidal evolution. The colored points indicate parts of each evolution track that match the planet’s present-day radius (1.061 ± 0.029R J), eccentricity (<0.17), and semimajor axis (0.0710 ± 0.0012 au). The blue curves indicate a planet that began on a circular orbit, where the large radius is due entirely to a low bulk metallicity (in this example, Z  p  = 0.13). In red is the “young circularizing” case, in which the planet is relatively young (∼1 Gyr) and at the final stages of fairly rapid circularization (﹩\mathrm{log}({Q}_{p})\,=\,5.5﹩), allowing for a hotter planet with larger bulk metallicity Z  p  = 0.37. Finally, the yellow curves indicate a slower circularization track (﹩\mathrm{log}({Q}_{p})\,=\,6﹩, Z  p  = 0.33), which is a potential compromise between the young age of the red line and the very low metallicity blue line. These are only three illustrative examples of a larger solution space (see Section 5.2).
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: The change of amplitudes, light-curve shapes and the relative phases of maximum light for two typical Milky Way Cepheids, X Cyg, and S Nor, moving top to bottom, from the infrared to the ultraviolet. Notice that the light-curve asymmetry, prominent in the visual, blue, and ultraviolet (UBV), damps down into a more symmetric, cycloidal variation in the near- and mid-infrared (JHK and 3.6). As the amplitude drops, the peak magnitude moves progressively to later phases. Template matching must take all of these wavelength-dependent variations into account when using light curves at one wavelength to predict light curves at another. Inspired by Wisńiewski & Johnson (1968), the above plots were constructed from individual Cepheid photometry files compiled by one of us (B.F.M.) over the last 50 yr. Individual photometry files, including references to the original publications, can be obtained, upon request, from the first author.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Tight correlation of interband period–luminosity residuals (derived from Figure 2). This example shows the detailed scaling of B-band residuals as a function of V-band residuals. The slope is well defined and the scatter is very low. Here the slope is DB/DV = 1.37 mag/mag, and the residual scatter around the fit is only ±0.043 mag. The slope defines the expansion/compression factor in using either one of these PL relations to predict the width of the other and the relative placement of points therein.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Residual scatter in the predicted B-band PL relation after random-phase corrections to mean light have been applied. For our sample the residual scatter is σ = ±0.043 mag. Dashed lines, on either side of zero, indicate 1σ deviations.
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: Predicted planet radii at a pressure level of 1 nbar in the atmosphere for a range of atmospheric mass fractions and intrinsic temperatures T int of 25 K (dark red), 50 K (red), 75 K (orange), and 100 K (yellow). The span in the shaded regions represents the impact of the uncertainty in the planet's mass on the model. The 1σ range of the observed radius is shown in the gray region. For atmospheric mass fractions <0.3, no model is able to match the observed radius for a haze that is optically thick in the slant geometry at 1 nbar.
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: Corner plot for key fitting parameters in the final joint fit.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Left: spatial distribution of sources considered in this study. Blue points show stars previously associated with the Mon R2 region from infrared and X-ray surveys, which are mainly concentrated in the central cluster and the two groupings to the east: GGD 12-15 and GGD 16-17. Red points result from our initial Gaia query and show the broad distribution of the optical sources that we tested for potential cluster membership. Right: histograms in proper motion R.A., proper motion decl., and parallax with red indicating the Gaia stars and blue bars showing the ±3σ range of the previously associated stars. The lower right panel is a color–magnitude diagram in Gaia G-RP vs. RP filters for the same two populations.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical structures at initial values of g 1 = 0 and g 2 = 0 under different mass ratios. The green dots represent flipping orbits. The red dots are the octupole-order resonant orbits that librate around σ = 0 and cannot flip. The blue dots represent orbits that are outside resonance and cannot flip. Stable periodic orbits are represented by black dots, and unstable ones are denoted by yellow dots. The white area stands for the forbidden region.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical structures associated with the octupole-order resonance centered at σ = 0 under different mass ratios. The regions denoted by different colors stand for orbits inside resonance, and the color bars represent different levels of the Hamiltonian. The pure blue regions stand for orbits outside resonance. The black dots represent stable periodic orbits, and the red dots represent unstable periodic orbits. The white area stands for the forbidden region. The initial angles are fixed at g 1 = 0 and g 2 = 0.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Same as Figure 9, but the initial angles are set at g 1 = 0 and g 2 = π, representing orbital flips about octupole-order resonance centered at σ = π.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical maps of the normalized second-derivative-based index ﹩\parallel {\rm{\Delta }}D\parallel ﹩ associated with the octupole-order resonance centered at σ = π. The initial angles are fixed at g 1 = 0 and g 2 = π. Black dots stand for the stable periodic orbits associated with the octupole-order resonance centered at σ = π.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical maps of the normalized second-derivative-based index ﹩\parallel {\rm{\Delta }}D\parallel ﹩ associated with the octupole-order resonance centered at σ = 0. The initial angles are fixed at g 1 = 0 and g 2 = 0. Black dots stand for the stable periodic orbits associated with the octupole-order resonance centered at σ = 0.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Same as Figure 6, but the initial angles are fixed at g 1 = 0 and g 2 = π, representing dynamical structures associated with the octupole-order resonance centered at σ = π.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical maps of the normalized second-derivative-based index ﹩\parallel {\rm{\Delta }}D\parallel ﹩ corresponding to the quadrupole-order resonance. The initial angles are fixed at g 1 = π/2 and g 2 = π/2. Black dots correspond to the stable periodic orbits associated with Kozai resonance.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: Dynamical structures at initial values of g 1 = π/2 and g 2 = π/2 under different mass ratios. The green dots represent flipping orbits. The red dots are Kozai resonant orbits that cannot flip. The blue dots represent orbits that are outside Kozai resonance and cannot flip. Stable periodic orbits are represented by black dots. The white area stands for the forbidden region.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: The FLI maps under different mass ratios with the initial angles of g 1 = π/2 and g 2 = π/2. The chaotic orbits are marked by yellow dots. The white area stands for the forbidden region.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. II. Speckle Observations of 16 Low-separation Systems
Authors: Ilija Medan, Sébastien Lépine, Zachary Hartman, Keivan G. Stassun
Figure caption: Left panel: the likelihood of a system being a binary for a value of ﹩\mu ^{\prime} ﹩, ﹩P(\mu ^{\prime} | B)﹩, for Binary 1. This likelihood is simulated from 10,000 random orbits drawn from uniform distributions, where the longitude of periastron is over the range of [0°, 360°], the eccentricity over [0, 0.95], the mean anomaly over [0°, 360°], the longitude of the ascending node over [0°, 360°], and the inclination over [0°, 90°] where is is made to be uniform in cos(i). The likelihood distributions shown are smoothed using a Kernel Density Estimator with a Gaussian kernel. The different colored solid lines show the likelihood for various assumed percent errors applied to the simulated speckle separations and position angles, i.e., σ  ρ /ρ and σ  θ /﹩(2\pi )﹩. The dashed black line is the value of ﹩\mu ^{\prime} ﹩ for Binary 1 from Table 4. Right panel: the likelihood of a system being a chance alignment for a value of ﹩\mu ^{\prime} ﹩, ﹩P(\mu ^{\prime} | C)﹩, for Binary 1. To generate these likelihood distributions, 10,000 field stars from a 5° region around the primary source are selected. By fixing the proper motion of the primary and using the proper motions of these field stars as that of the secondary, the relative motion between the Gaia and speckle epochs can be found. The likelihood distributions shown are smoothed using a Kernel Density Estimator with a Gaussian kernel. The different colored solid lines show the likelihood for various assumed percent errors applied to the simulated speckle separations and position angles, i.e., σ  ρ /ρ and σ  θ /﹩(2\pi )﹩. The dashed black line is the value of ﹩\mu ^{\prime} ﹩ for Binary 1 from Table 4.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. II. Speckle Observations of 16 Low-separation Systems
Authors: Ilija Medan, Sébastien Lépine, Zachary Hartman, Keivan G. Stassun
Figure caption: Violin plot of the pixel scales (top row) and offset in the position angle from the true value for the calibration binaries (bottom row). In each plot, the blue violin plots are for the 562 nm camera and the red for the 832 nm camera. The data points and error bars show the 50th and 16th/84th percentiles, respectively. These percentiles correspond to the values shown in Table 2. The shaded regions in the plots show the distribution of the data, as estimated by a Gaussian Kernel Density Estimator. In both rows, the solid black bar separates the astrometric calibrations for ‘Alopeke (GN in the x-axis labels) and Zorro (GS in the x-axis labels). In each label, the year and month of the observing run is shown.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. II. Speckle Observations of 16 Low-separation Systems
Authors: Ilija Medan, Sébastien Lépine, Zachary Hartman, Keivan G. Stassun
Figure caption: Example of the data products produced by the Gemini speckle pipeline for Binary 2 in Table 3. The red and blue lines in the far left panel show the contrast limit for the 832 nm and 562 nm bands, respectively, which is a result of using the background flux levels to determine the faintest companions one can reliably detect as a function of separation. In the four panels on the right, we show the autocorrelation functions (top row) and reconstructed images (bottom row) for the binary in each bandpass, where the bandpass is indicated in the top left corner of each panel.
Paper: Detecting New Visual Binaries in Gaia DR3 with Gaia and Two Micron All Sky Survey (2MASS) Photometry. II. Speckle Observations of 16 Low-separation Systems
Authors: Ilija Medan, Sébastien Lépine, Zachary Hartman, Keivan G. Stassun
Figure caption: Distribution of projected physical separations (left panel) and Gaia G magnitude (right panel) for candidate binary stars resolved by Gaia eDR3. The blue histograms are for candidate binaries identified with our method with s < 30 au, and that have not been identified as binaries in previous studies. The orange histograms are for binaries identified in El-Badry et al. (2021) with d < 200 pc and s < 30 au. The green histograms are for candidate binaries identified with our method but already listed in the Washington Double Star Catalog (Mason et al. 2001) or observed with high-resolution imaging in previous studies.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Semimajor axis prediction test: truncating the observational arc until 2017 June 1 (subscript short) with respect to the full arc (subscript long). The difference in semimajor axis is normalized by the predictor uncertainty (i.e., (a long − a short)/σ  a,short). A Gaussian distribution is included for reference. The pdf is estimated by the bin count divided by the number of objects times the bin width (i.e., count/(N · w  i )).
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Normalized orbital fit residuals of asteroid 3557 Sokolsky (H = 11.06), using the photocenter offset uncertainty factor (blue, λ = 0.3) and without photocenter offset uncertainty factor (orange, λ = 0). Both solutions include the photocenter offset correction. Residuals removed from the fit are shown with a cross symbol, whereas circles are included in the fit. The dashed lines show the ±3σ bounds for reference. The automatic rejection algorithm is from Carpino et al. (2003).
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Semimajor axis prediction tests of the 20,915 asteroids with H < 14 and σ  a,FPR < 10−8 au truncating the observational arc until 2017 June 1, shown as in Figure 11. The predictions are made with or without photocenter offset correction and setting λ to the following values: with correction, λ = 0.3 (blue); with correction, λ = 0.0 (orange); and without correction, λ = 0.0 (yellow). The mean and standard deviations of the prediction errors using the three approaches are in Table 1.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Semimajor axis difference between long-arc solutions of the 20,915 asteroids with H < 14 and σ  a,FPR < 10−8 au. The nominal long-arc solution is compared to the long-arc solution without photocenter correction or photocenter offset uncertainty factor. The differences are normalized to the uncertainties in the latter (λ = 0). Cyan line indicates the moving median of the distribution, with 3σ standard deviation of the median bounds.
Paper: Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Shantanu P. Naidu, Ryan S. Park
Figure caption: Sensitivity of the semimajor axis to perturber masses via Monte Carlo as a function of the formal uncertainty in the semimajor axis. The results are of 1000 asteroids randomly picked from the H < 14 and σ  a,FPR < 10−8 au group.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HR 8799 (Marois et al. 2008, 2010) for Sequence 10 in Table 1.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HR 8799 (Marois et al. 2008, 2010) for Sequence 12 in Table 1.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Orbital period, radii, and densities of the planets with mass estimates from this work. KOI numbers for which at least one planet does not have a previously reported mass value or upper limit are shown in underlined bold text. The size of the circles represents the absolute planetary size, and the color scale indicates our adopted density. Only planets with densities estimated to the significance of more than 4σ are color filled; others are open. For some of the planets (e.g., in the systems KOI-593 and KOI-1589) the relative masses are well constrained, but the absolute mass (and hence density) is not well constrained owing to a high uncertainty on the stellar mass and radius, and hence these planets are shown here open. For reference, the legend shows the size and density of Earth, Jupiter, and Neptune. The short vertical black lines indicate the locations of the closest first-order MMRs to the observed period ratio of adjacent planets. The black plus signs similarly indicate the locations of second-order MMRs—note that many planets are close to these MMRs. Both first- and second-order MMRs are indicated only if they are close to the observed period ratios. We do not show second-order MMRs that are a multiplication of a first-order MMR (e.g., 4:2 and 2:1).
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: An example for the N-body matching test performed on the best-fitting solution of the planetary system of Kepler-79 (KOI-152), demonstrating the ability of AnalyticLC to generate a model consistent with full N-body integration of a four-planet system. The mismatch is quantified as ﹩{\chi }_{\mathrm{Nbody}}^{2}\sim 10﹩, (σ Nbody = 0.0321)—a systematic error much smaller than the statistical error arising from the data uncertainty. (a) TTV pattern of the N-body model (o) and the AnalyticLC model (x) for the four planets in this system (b in blue, c in red, d in yellow, e in purple). The symbols are on top of each other at this scale. (b) “Residuals”: times of midtransit mismatch between the N-body-generated model and AnalyticLC, which is of order a few seconds for the innermost planet and of order a minute for the three outer planets. (c) Manifestation of the mismatch to terms of relative flux. The mismatch standard deviation within the in-transit points is 0.7, 10, 25.5, and 9 ppm for the four planets correspondingly, innermost to outermost. The typical Kepler short-cadence data (which is almost all of the data) uncertainty for this star (∼1000–1200 ppm).
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: An overview of the N-body match with AnalyticLC for all our runs, including both this work and the former work of the two- and three-transiting-planet systems, including runs that both did and did not pass our acceptance criteria. This map demonstrates the accuracy limits of AnalyticLC. The horizontal axis is the largest magnitude of all free eccentricities and inclinations in the system at the best-fitting solution derived by AnalyticLC. The vertical axis is the minimal closest approach in the system in units of mutual Hill radii. The color of the points represents the value of σ Nbody, with points at which σ Nbody > 1.5 (which do not pass our acceptance criterion) also marked with black edges.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Observed phases. Transit is at ϕ = 0, and secondary eclipse is at ϕ = 0.5. The colors of the sectors indicate whether the planet signal is blue- or redshifted during those phases. Not to scale.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Observing conditions on each of the three nights data were taken.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Distribution of observed stellar binary inclinations integrated over all stellar types, compared with inclinations drawn from an isotropic distribution. The “strict” sample is shown in purple, while the “loose” sample and the control sample are shown as black and green unfilled histograms, respectively. The mean and standard deviation of 150,000 random draws from an isotropic distribution, each containing 40 systems (the same number as our “strict” sample), are shown as dark blue error bars.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Normalized distribution of inclinations for the “strict” sample (purple filled histogram) with no s or T eff cuts, as well as the more restricted hot star (orange outline) and cool star (blue filled histogram) samples for comparison. Overplotted in the same colors is the maximum likelihood von Mises probability density function fitted to the full “strict” sample (μ = 90.°0 and κ = 3.8) and to the cool star subset sample (μ = 90.°8 and κ = 11.1), each of which demonstrates a single peak. The von Mises probability density function for a simulated isotropic distribution, with 30,000 draws as in Figure 7, is shown in black for reference, with μ = 90.°0 and κ = 2.7.