adsabs/AstroCLIMB huggingface dataset:
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Blackbody curve for K2-18b and a theoretical moon orbiting in a 2:1 resonance with an outer moon. T irr = 293 K and the tidal heating temperature of the moon is also 293 K, giving T tot = 348 K for the moon, which is not nearly enough to match the luminosity of the planet.
Paper: Tidal Heating of Exomoons in Resonance and Implications for Detection
Authors: Armen Tokadjian, Anthony L. Piro
Figure caption: Similar to Figure 13, but including the luminosity of the star. The best wavelength range to observe the system in terms of detecting this moon is shown as green vertical lines and corresponds to 6–8 μm.
Paper: Revising Properties of Planet–Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems  
Authors: Kendall Sullivan, Adam L. Kraus, Daniel Huber, Erik A. Petigura, Elise Evans, Trent Dupuy, Jingwen Zhang, Travis A. Berger, Eric Gaidos, Andrew W. Mann
Figure caption: The separation and Kepler contrast for our observed sample. Although we had a maximum contrast cutoff of 3.5 mag in at least one photometric band, this led to the inclusion of some systems with high optical contrasts but with an NIR contrast that met our selection criterion. The sample only included systems out to angular separations of 2″. Although there is substantial scatter in both dimensions, the most frequent systems are those at close separation and near-equal brightness. The histograms at the top and on the right of the figure show the marginalized distribution in contrast or separation.
Paper: Revising Properties of Planet–Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems  
Authors: Kendall Sullivan, Adam L. Kraus, Daniel Huber, Erik A. Petigura, Elise Evans, Trent Dupuy, Jingwen Zhang, Travis A. Berger, Eric Gaidos, Andrew W. Mann
Figure caption: Left: a series of histograms of the input composite Mathur et al. (2017) T eff (top panel) and the output primary and secondary T eff (middle and bottom panels, respectively). The input temperature distribution and output primary star temperature distribution are both dominated by FGK stars, although there are more hot stars in the retrieved primary star sample because of the upward temperature revision for primaries. Similarly, there are more cool stars and a wide spread for the retrieved secondary star sample because of the downward temperature revision for secondaries. Right: an H-R diagram showing the input Mathur et al. (2017) T eff and radius for each system (magenta points) and the revised T eff and radius for the primary stars (blue points), with lines connecting each system. MIST isochrones at 1, 3, 5, and 7 Gyr are plotted under the points as a reference. We used the 1 Gyr isochrone to calculate the radii, which is a good fit for both the input and output values for most of the stars, although there is scatter in the hottest systems because of significant distance revisions between the KIC and Gaia for many of the stars.
Paper: Revising Properties of Planet–Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems  
Authors: Kendall Sullivan, Adam L. Kraus, Daniel Huber, Erik A. Petigura, Elise Evans, Trent Dupuy, Jingwen Zhang, Travis A. Berger, Eric Gaidos, Andrew W. Mann
Figure caption: Histograms of the input Kepler planet radius (top; Mathur et al. 2017) and the inferred best-fit planetary radii assuming that the primary or secondary stars were the planet hosts (middle and bottom, respectively). The primary and secondary host assumption panels include approximate completeness curves, detailed in the text.
Paper: Revising Properties of Planet–Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems  
Authors: Kendall Sullivan, Adam L. Kraus, Daniel Huber, Erik A. Petigura, Elise Evans, Trent Dupuy, Jingwen Zhang, Travis A. Berger, Eric Gaidos, Andrew W. Mann
Figure caption: A KDE of the revised planetary radii assuming that the primary star is the host in all cases (thick blue line), with KDEs of 100 random draws from the error distributions for each sample underplotted (thin blue lines), as well as the median of the CKS subsample (dark-gray line), with KDEs of 100 random subsamples from CKS underplotted (light-gray lines). The calculation for the gray region showing the completeness limit is described in the text. Neither the 100 observations of the CKS sample nor the median are consistent with our observed radius distribution.
Paper: Revising Properties of Planet–Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems  
Authors: Kendall Sullivan, Adam L. Kraus, Daniel Huber, Erik A. Petigura, Elise Evans, Trent Dupuy, Jingwen Zhang, Travis A. Berger, Eric Gaidos, Andrew W. Mann
Figure caption: Left: planetary radii from this work, calculated assuming that the primary star is the planet host, plotted against the Kepler planetary radius. The light-gray dashed line denotes 1 R ⊕, and the dark-gray dashed line denotes 1.8 R ⊕ (approximately the location of the single-star radius gap). The dotted black line denotes one-to-one correspondence between the axes. The majority of systems have larger radii measured in our work than by Kepler with planetary radii being revised upward by 17% (84th percentile +23%, 16th percentile −16%), with the large spread in the distribution being caused by the wide range in binary properties within the sample. Right: the same as the left panel, but for the case where the secondary star is assumed to be the planet host. The majority of systems fall above the single-star radius gap, with an average planet radius revision of +66% (84th percentile +31%, 16th percentile −127%).
Paper: Revising Properties of Planet–Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems  
Authors: Kendall Sullivan, Adam L. Kraus, Daniel Huber, Erik A. Petigura, Elise Evans, Trent Dupuy, Jingwen Zhang, Travis A. Berger, Eric Gaidos, Andrew W. Mann
Figure caption: The planet radius assuming that the planets all orbit the primary stars, plotted against the planets’ orbital periods (blue points), with a KDE underlaid (blue contours). The KDE has a kernel size of 0.25 in both log(period) and linear radius and shows no clear gap in the period–radius distribution. All quantities are in terms of detected planets, not occurrence rate.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Local linear model-predicted vs. ASPCAP abundances of the doppelgänger (left), doppelgänger AK  (middle), and KOI (right) samples for the twelve elements considered. The points are colored by log g. The rms difference between the ASPCAP and predicted abundances, intrinsic dispersions, and bias measurements are provided in the upper left corners of each panel. A dashed 1-to-1 line is plotted in all panels for comparison.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: The radius vs. orbital period distribution for our sample of 130 KOI systems, with the ASPCAP-reported [Fe/H] of their host stars marked in color. Hot/warm Jupiters are defined as planets with R > 8 R ⊕ and P < 100 days (red region), hot/warm sub-Saturns with 4 R ⊕ < R < 8 R ⊕ and P <100 days (orange region), cold Jupiters with R > 8 R ⊕ and P > 100 days (purple region), cold sub-Saturns with 4 R ⊕ < R < 8 R ⊕ and P > 100 days (dark blue region), and super-Earths/sub-Neptunes with R < 4 R ⊕ (light blue region).
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: The ﹩\mathrm{log}g﹩ vs. T eff probability density functions for the ∼129,000 high-fidelity APOGEE DR17 stars (gray). The contours represent areas encompassing 10% of the cumulative probability mass. The 130 non “False Positive” KOIs included in the high-fidelity sample with doppelgängers are shown as circles, with colors representing their [Fe/H] values.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: The ΔT eff (upper left), Δ﹩\mathrm{log}g﹩ (upper right), Δ[Fe/H] (lower left), and Δ[Mg/H] (lower right) distributions for each KOI-doppelgänger pair. The average associated errors added in quadrature (for KOIs and doppelgängers) for each parameter are shown in the dashed red lines, and encompass the majority of the distributions (∼77%, ∼85%, ∼78%, and ∼81% for the ΔT eff, Δ﹩\mathrm{log}g﹩, Δ[Fe/H], and Δ[Mg/H] distributions, respectively).
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: The left panel displays the [Fe/H] distributions for our KOI (red) and doppelgänger (blue) samples, as well as that of a sample of non-planet host field stars drawn from the Kepler field (gray). The right panel displays the [Mg/H] distributions for our KOI (red) and doppelgänger (blue) samples, as well as that of a sample of non-planet host field stars drawn from the Kepler field selected to have the same [Fe/H] as our KOI sample (gray).
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Examples of separate linear trends fitted to volatile (blue) and refractory (red) abundances ordered by T c for our KOIs and corresponding doppelgängers. The boundary between volatile and refractory elements is set to T c = 1000 K. Linear fits to the ASPCAP and predicted abundances are provided in the upper and lower panels, respectively. There are no individual errors associated with the predicted abundances, but the median intrinsic dispersion values for the KOI and doppelgänger samples across all abundances are shown in the upper left corners of the predicted abundance panels.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Intercept difference (refractory − volatile) distributions from linear trend fits to the T c-ordered refractory and volatile abundances of individual stars in the KOI (red) and doppelgänger (blue) samples. The distributions for the predicted and ASPCAP abundances are provided in the right and left panels, respectively. The contributions corresponding to the KOIs with the top five largest intercept differences are outlined in black in the KOI ASPCAP distribution. Four out of these five KOIs overlap with the five KOIs that are outliers in predicted and ASPCAP [Na/H] space.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Linear trend slope distributions for the T c-ordered abundances of individual stars in the KOI (red) and doppelgänger (blue) samples, for only refractory elements (T c > 1000 K). The distributions for the predicted and ASPCAP abundances are provided in the right and left panels, respectively. The slope contributions from our five Na outlier stars are represented by the transparent regions of the distribution.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Local linear model-predicted vs. ASPCAP abundances of the higher quality ([X/H]err < 0.07 dex) doppelgänger (left), doppelgänger A  K  (middle), and KOI (right) samples for [Na/H]. The points are colored by ﹩\mathrm{log}g﹩. The rms difference between the ASPCAP and predicted abundances, intrinsic dispersion, and bias measurements are provided in the upper left corners of each panel. A dashed 1-to-1 line is plotted in all panels for comparison.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Intrinsic dispersion measurements σ intrinsic for all T c ordered abundances, for the KOI sample (red), doppelgänger sample (navy), and A  K  doppelgänger sample (light blue). There are no apparent trends with T c, but the KOI [Na/H] prediction intrinsic dispersion is noticeably larger than those of the doppelgänger samples.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Spectra of the five KOIs that appear to be outliers in predicted and ASPCAP [Na/H] space (red), zoomed into the region with Na spectral features used to derive [Na/H] abundances with the ASPCAP pipeline (window center at 16378.276 Å; Feeney et al. (2021), marked by the dashed line). The spectra of the corresponding outlier doppelgängers are shown in black.
Paper: Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Authors: Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell
Figure caption: Linear trend slope distributions for the T c-ordered abundances of individual stars in the KOI (red) and doppelgänger (blue) samples. The distributions for the predicted and ASPCAP abundances are provided in the right and left panels, respectively. The slope contributions from our five Na outlier stars are represented by the transparent regions of the distribution.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: (a) Proper motion diagrams of stars in the baseline samples of W Ser, RX Cas, SX Cas, and V367 Cyg. μ  δ  and μ  α  are proper motions in decl. and R.A. in mas yr−1. The dotted lines mark the proper motions of the W Ser systems. Typical 1σ random errors in the proper motions of all stars in these diagrams are ±0.02–0.03 mas yr−1 along each axis. The vast majority of objects in the baseline samples are scattered throughout the diagrams and are likely not related to the W Ser systems. Still, there are objects that have proper motions that are similar to those of the W Ser systems. The locations of W Ser and RX Cas indicate that their kinematic properties differ in a systematic way from those of most other stars in their baseline samples. (b) Same as Figure 1(a), but showing the proper motion diagrams of baseline sample stars near W Cru, V644 Mon, V1507 Cyg, and V356 Sgr. There are obvious concentrations on the proper motion plane around V644 Mon and W Cru. The large baseline sample for W Cru is due to the substantial line-of-sight distance that is sampled for this system. A concentration of objects is evident in the proper motion plane of V1507 Cyg that is offset from the proper motions of that system.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: (Top panel) Composite proper motion diagram of the W Ser, RX Cas, SX Cas, V367 Cyg, and V356 Sgr baseline samples. The proper motions of each system have been subtracted from those of individual stars to align the samples. The origin is at the intersection of the dotted lines. There is an apparent concentration of objects at the origin, indicating a general tendency for the W Ser systems to have companions. The green square is 3 mas yr−1 on a side, and shows the approximate extraction area adopted to identify companions for these stars. (Bottom panel) Number density of sources in the top panel (i.e., the number of objects per mas2 yr−2) vs. the radial offset from the origin. The dashed line shows the average density in the four bins with the greatest offsets from the origin, where the density in proper motion space appears to be stable. While the error bars are large, there is a tendency for the density of objects in proper motion space to decrease with increasing offset out to ∼4.5 mas yr−1.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: Envelopes around the W Ser systems. Each panel shows an image in W2 that subtends 70″ × 70″. A PSF that has been scaled to minimize the residuals near the center of each system has been subtracted from each image, to highlight signal from envelopes and surrounding stars. The PSF-subtracted images are displayed with a common scaling factor to facilitate system-to-system comparisons of envelope brightness. Extended envelopes are clearly seen around W Ser, RX Cas, V367 Cyg, W Cru, and V644 Mon. While not evident in this figure, a very faint envelope is also present around V1507 Cyg. The prominent substructures within the envelopes are likely artifacts of the PSF-subtraction process (see text).
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: Angular distributions of stars in the baseline (black line) and final (green line) samples. Cumulative number counts in 30° wide bins are shown along the y-axis. Position angles (PAs) were measured centered on the W Ser systems, with 0° to the east. The distributions have been normalized to the total number of objects in each sample. Objects that are uniformly distributed on the sky define a diagonal that is indicated by the dotted lines. In most cases, the baseline samples are consistent with a uniform distribution. Possible exceptions are V367 Cyg and V644 Mon, where there is a tendency for objects to be concentrated between 260° and 360°. A Kolmogorov–Smirnov (KS) test indicates that the angular distributions defined by the baseline and final samples of RX Cas and V1507 Cyg differ at the 75%–85% confidence level.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: (a) Locations on the sky of stars in the baseline (black crosses) and final (green squares) samples of W Ser, RX Cas, SX Cas, and V367 Cyg. Offsets in R.A. and decl. from each W Ser system are plotted. (b) Same as Figure 3(a), but showing the locations of stars near W Cru, V1507 Cyg, V644 Mon, and V356 Sgr. The large number of objects in the W Cru final sample is a consequence of the large volume sampled around this system.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: (a) Comparisons with nonrotating, solar-metallicity MIST isochrones. The sequences have ages log(t yr) = 7.5 (black), 8.0 (blue), 8.5 (green), 9.0 (yellow), and 9.5 (red). Points are plotted using the same identification scheme as in Figure 6(a). The log(t yr) estimated for each system is shown under the system name. The entries in brackets for RX Cas and SX Cas are age estimates that are based on the second-brightest main-sequence star, as an SGB is not visible in the final-sample CMDs of those systems. The estimated uncertainties in the ages are 0.1–0.2 dex (see text). (b) Same as Figure 7(a), but showing CMDs for W Cru, V644 Mon, V1507 Cyg, and V356 Sgr. Two age estimates are given for W Cru, V644 Mon, and V356 Sgr, and the entry in brackets is that based on the second-brightest main-sequence star.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: (a) (G, Bp − Rp) CMDs of stars in the baseline (black crosses) and final (green squares) samples of W Ser, RX Cas, SX Cas, and V367 Cyg. The W Ser system, which is circled in black in each panel, is the brightest object in each CMD. The main sequence is the dominant feature in each CMD. The stars with red colors that are above and to the right of the main sequence are likely SGB stars that belong to an intermediate-age field population. (b) Same as Figure 6(a), but showing the CMDs for W Cru, V644 Mon, V1507 Cyg, and V356 Sgr. SGB sequences are seen above and to the right of the main sequence in the baseline sample CMDs of W Cru, V644 Mon, and V1507 Cyg.
Paper: The Environments around W Serpentis Systems: Independent Limits on System Masses and Extended Envelopes
Authors: T. J. Davidge
Figure caption: Same as Figure 4, but showing radial distributions centered on the W Ser systems. Cumulative number counts have been measured in 0.°05 angular bins on the sky centered on the W Ser systems, with the distributions normalized to the total number of counts in each sample. System-to-system differences in the slopes and total angular extents of the baseline distributions are due to the wide range in system distances. With the exception of SX Cas, and to a lesser extent W Cru and V1507 Cyg, the radial distributions of the baseline and final samples are not significantly different.
Paper: A Catalog of Nearby Accelerating Star Candidates in Gaia DR3
Authors: Marc L. Whiting, Joshua B. Hill, Benjamin C. Bromley, Scott J. Kenyon
Figure caption: Predicted vs. true χ 2 for linear drift in the HGCA from Gaia DR2 and EDR3 astrometry. The true χ 2 values are reported in the HGCA (Brandt 2021), while the predictions are generated with the RANDOM FOREST regressor. The darker points and blue contours (at containment thresholds of 2%, 20%, 50%, 80%, and 98%) correspond to the training set, with half of the sources in the HGCA chosen at random. The remaining stars constitute the test set. The lighter-shaded points and red contours indicate the test set’s predicted vs. true χ 2. The training set results are characteristic of the RANDOM FOREST regressor; it is derived from a decision tree algorithm, which gives perfect correlations between the true and predicted values. With RANDOM FOREST, this correlation is blurred by randomness in the decision tree branch choices, seen in the blue contours—they show a strong but imperfect correlation between the true and predicted χ 2. This approach preserves broader significant trends in the data, allowing them to be revealed in the test set. Without the randomness, the regressor would be overly tuned to the details of the training set, significantly reducing the effectiveness as a predictor of χ 2 in other data. Here, the predicted χ 2 shows a correlation between true values and predictions, which becomes stronger at larger χ 2.
Paper: A Catalog of Nearby Accelerating Star Candidates in Gaia DR3
Authors: Marc L. Whiting, Joshua B. Hill, Benjamin C. Bromley, Scott J. Kenyon
Figure caption: The CMD of the GNASC, derived from the machine-learning algorithm described in the text. The left panel is the complete catalog containing 29,684 stars from Gaia EDR3. Parallax and brightness cuts ensure that the stars included here are those with high-quality astrometric measurements. The panel on the right shows the CMD for our catalog’s top 500 sources, which are the subset of the most promising candidates sorted by the χ 2 values. The panel on the right is more heavily weighted toward the upper main sequence than toward the bulk of the sample (left), which has a more significant fraction of lower-main-sequence stars. The unique catalog of stars offers promising accelerating candidates expected to lead to the discovery of new stellar and substellar companions.