adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: Left and middle: continuum emission images of the LkCa 15 disk at 1.3 and 0.88 mm, respectively, with identical beam size of 50 mas, shown in the bottom left corner of each panel. An asinh color stretch is applied to highlight the faint emission. Right: azimuthally averaged radial intensity profiles in brightness temperature. The three prominent dust rings are marked by the dashed vertical lines. The spectral index profile between the two bands is indicated by the dotted line (y-axis labels on the right side). The Gaussian profile in the bottom right corner shows the FWHM of the synthesized beam.
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: The comparison of near-IR dust scattered light (SPHERE IRDIS J-band imaging polarimeter; Thalmann et al. 2016) and ALMA millimeter dust rings (the three gray ellipses) in the LkCa 15 disk. The inner working angle of 80 mas in the SPHERE image is masked out. The ALMA B6 residual contours are shown at 8σ, 10σ, and 12σ levels in pink. The putative planet location is indicated.
Paper: Migratory Outbursting Quasi-Hilda Object 282P/(323137) 2003 BM80 
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo
Figure caption: Additional results from dynamical integration of 282P orbital clones. For each plot, time t = 0 is UT 2022 January 21. Close encounters with Jupiter and Saturn are so significant that orbital elements cannot be accurately determined before/after −180 ≲ t ≲ 300 yr, given orbital uncertainties. (a) Distance between Jupiter and 282P as a function of time. Indicated Hill radii provide references for the degree of orbit alteration imparted by a close encounter. For reference, the semimajor axes of two Jovian moons are shown: Callisto, the outermost Galilean satellite, and Sinope (Nicholson 1914), a likely captured (Grav et al. 2003) distant irregular and retrograde Jovian moon. (b) Distance between Saturn and 282P as a function of time. The semimajor axis of the irregular Saturnian moon Phoebe, believed to be captured through close encounter (Johnson & Lunine 2005; Jewitt & Haghighipour 2007), is given for reference. (c) Heliocentric distance r evolution. (d) Tisserand parameter with respect to Jupiter T J (Equation (2)), where the horizontal orange line representing T J = 3 indicates the widely adopted boundary between comet-like and asteroid-like orbits.
Paper: Migratory Outbursting Quasi-Hilda Object 282P/(323137) 2003 BM80 
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo
Figure caption: 282P heliocentric distance, observability, apparent brightness, observability, and temperature, from 2012 through 2025. Heliocentric Distance: Activity detections (triangles) are marked as positive (filled red) and negative (unfilled blue) detections and as either inbound (▾) or outbound (▴). Observations are cataloged in Appendix A. Also indicated are perihelion (orange q) and aphelion (blue Q) passages. Apparent Magnitude: The apparent V-band magnitude through time of 282P. Observability: Our observability metric for Cerro Tololo Inter-American Observatory (CTIO), site code 807 (blue solid line) and the Lowell Discovery Telescope (LDT), site code G37 (orange dashed line), depicting the number of hours 282P was observable (>15° above the horizon between sunset and sunrise) during a given universal time (UT) observing date. Opposition events and conjunctions result in maxima and minima concurrent with apparent magnitude, respectively. Temperature: Modeled temperature by date for the thermophysical extremes: a “flat slab” (χ = 1, top line) and an isothermal body (χ = 4, bottom line).
Paper: Migratory Outbursting Quasi-Hilda Object 282P/(323137) 2003 BM80 
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo
Figure caption: Results from dynamical integration of 282P orbital clones. For all plots, time t = 0 corresponds to UT 2022 January 21. Jovian and Saturnian close encounters prevent accurate orbital parameter determination outside −180 ≲ t ≲ 300 yrs, given known orbital uncertainties. (a) Orbital diagram for 282P and nearby planets; note that Uranus and Neptune were included in our simulations, but they are not shown here. (b) Semimajor axis a evolution. (c) Eccentricity e evolution. (d) Inclination i evolution.
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: The disk continuum images and frank residual maps with different synthesized beams for both B6 (top panels) and B7 (bottom panels). Columns correspond to different beam sizes, as indicated in the top panels. The disk images and first row of residual maps were created with the full combined data, while the second row used only the long-baseline data sets.
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: Comparisons of the data and frank model in the visibility profile and image plane for B6 (top panels) and B7 (bottom panels). The data visibilities are binned in 5 k λ shown in gray points. The insert panel shows a zoom-in view of the long-baseline part outward of 1 Mλ with data binned in 50 k λ.
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: The model brightness profiles derived with frank, using the parameters described in Section 3. The three prominent dust rings are marked with the gray vertical lines. The data radial profiles from images convolved with a 50 mas beam are shown in dashed lines for comparison.
Paper: Migratory Outbursting Quasi-Hilda Object 282P/(323137) 2003 BM80 
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo
Figure caption: Orbital motion of minor planets (blue lines) as seen in the reference frame corotating with Jupiter (orange lines at right edge of plots). (a) MBC (7968) Elst-Pizarro (133P). (b) JFC 67P/Churyumov–Gerasimenko (previously visited by the European Space Agency (ESA) Rosetta Spacecraft). (c) Centaur (2060) Chiron (95P). (d) (153) Hilda, the namesake of the Hilda dynamical class, in the 3:2 interior mean-motion resonance with Jupiter. (e) Quasi-Hilda 246P/NEAT, also designated 2010 V2 and 2004 F3. (f) Our object of study, 282P, in its quasi-Hilda orbit.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Left panel: the probabilities p NS for each binary black hole in GWTC-2 to be nonspinning, as computed in two different ways: through a Savage–Dickey density ratio and using fully marginalized likelihoods computed via nested sampling and reported in Abbott et al. (2021c). The circles denote GW190408_181802 and GW190828_063405, whose nested sampling results appear to be outliers. Center panel: the spin magnitude posterior for GW190408_181802. Nested sampling yields a Bayes factor of ﹩{{ \mathcal B }}_{{\rm{S}}}^{\mathrm{NS}}\sim 130﹩ in favor of the hypothesis that this event is nonspinning. This would require the spin magnitude posterior to be ∼130 times larger than the (flat) prior at χ 1 = χ 2 = 0. This is inconsistent, though, with the true posterior on the spin magnitudes of GW190408_181802, suggesting that the nested sampling Bayes factor in favor of the nonspinning hypothesis is significantly overestimated. Right panel: as a consistency check, we repeat the counting experiment from Section 3 using the nested sampling Bayes factors serving as input to Galaudage et al. (2021), rather than our Savage–Dickey estimates. We show posteriors obtained using the entire GWTC-2 catalog (solid blue curve) and results after excluding GW190408_181802 from our sample (dashed blue). As mentioned in Section 3, we obtain much closer agreement with the Savage–Dickey result (gray curve) after excluding GW190408_181802.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Posterior on the parameters of the Extended component spin model (Equations (H1) and (H2)) using GWTC-3 data (orange) and just GWTC-2 data (purple). The one-dimensional marginalized posteriors for the BetaSpike+TruncatedMicture model for GWTC-3 are shown in black dashed lines for comparison; this result is identical to that shown in Figures 6 and 16. The Extended model infers a population with smaller f spike and larger f iso than BetaSpike+TruncatedMicture; it also has more support for ﹩{z}_{\min }\gt 0﹩ than BetaSpike+TruncatedMicture, although the z min posterior peaks at a negative value for both cases. The posteriors for the remaining population parameters are qualitatively similar between the two models.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Scatter plot of the minimum (across events) number of effective samples ﹩\min \left[{N}_{\mathrm{eff},i}\right]﹩ and the width of the zero-spin spike ϵ spike for the BetaSpike+TruncatedMixture model. Each point represents a single draw from the posterior shown in Figure 6. Left panel: the minimum number of effective samples as computed across the entire population model. Middle panel: the minimum number of effective samples in the “bulk” (Beta distribution) spin magnitude subpopulation.. Right panel: the minimum number of effective samples in the “spike” (zero-spin half-Gaussian) spin magnitude subpopulation. Dashed vertical lines denote ϵ spike = 0.03, the lower limit we impose on this parameter in our prior. Although the minimum sample count in the spike appears unacceptably low, the minimum is driven by events that are confidently spinning and which therefore do not impact our inference regarding the zero-spin spike (see the left panel of Figure 11). Red points illustrate the minimum effective samples when excluding events these events that are confidently spinning. Green points show the minimum effective sample count if we further exclude events that are “likely” spinning (e.g., middle panel of Figure 11), focusing only on those events that are well described by zero spin. To ensure a reasonable number of effective samples among these remaining events, we bound ϵ spike > 0.03 and note that the region ϵ spike ≲ 0.04 may be subject to elevated Monte Carlo variance.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption:  Spin magnitude posterior samples demonstrating the three classes of events discussed in Figure 10 above. The left-hand panel illustrates a confidently spinning binary, which is clearly identified as a member of the spinning “bulk” population and whose low effective sample count in the spike is therefore unimportant. The middle panel illustrates a “likely” spinning event, defined by having less than a fraction 1/200 of its posterior samples in the region χ 1, χ 2 < 0.1. The right panel, finally, shows an event belonging to neither category; these remaining events are used to generate the green points in Figure 10 above.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Predictive checks of the three effective spin models explored in Section 4. Under each model, we repeatedly generate sets of “Observed” χ eff values drawn from our binary black hole observations, and sets of “Predicted” values according to the fitted models; see Appendix C for further details. Each trace among the three subplots represents one such realization, with the spread among traces reflecting both our uncertainty in the properties of each observed binary as well as the uncertainty in model hyperparameters. A model that provides a good fit to observation will yield an ensemble of traces centered symmetrically around the diagonal, whereas any systematic departure from the diagonal would indicate model failure. No such departures are seen, and so all three effective spin models are able to successfully reproduce observation.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Follow-up exploration of the injected mock catalog that most strongly (and incorrectly) excludes ζ spike = 0 in Figure 3. Left: the joint posterior on ζ spike and μ eff from the selected catalog. In general, we find significant correlations between ζ spike and the mean μ eff of the spinning “bulk” population. Mock catalogs that most strongly disfavor ζ spike = 0 are generally those that have the largest inferred μ eff. Middle: the individual events comprising the selected catalog. The event with the largest measured χ eff (and hence the event that most strongly influences μ eff) is highlighted. Right: the solid blue curve shows the updated ζ spike posterior after removing the highlighted high-spin event. Compared to the original ζ spike measurement (dashed black curve), the updated posterior is now more (correctly) consistent with ζ spike = 0.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Posterior on the parameters of the BetaSpike+TruncatedMicture component spin model, now using only GWTC-2 events (purple). The shaded region in the μ  χ –σ  χ  two-dimensional posterior is the region excluded by the prior cut on the shape parameters of the beta distribution α, β > 1. For reference, results using the full GWTC-3 event list are shown in orange; the GWTC-3 result is identical to the one presented in Figure 6. We find broadly consistent results between the two catalogs, including no requirement for a zero-spin subpopulation as well as a preference for spins misaligned by more than 90° relative to binaries’ Newtonian orbital angular momentum.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: As in Figure 8 above, but for the component spin models studied in Section 5. We explore each model’s ability to predict the observed spin magnitudes (first and second columns), spin tilts (third and fourth columns), and effective spins (fifth column). Again, we see no clear departures from the diagonal, such that none of the four models can be rejected as a poor descriptor of our data. The Beta+Mixture and BetaSpike+Mixture models may exhibit slight tension with observation, possibly overpredicting the occurrence of very negative ﹩\cos {\theta }_{1}﹩ and χ eff, but additional data are required to confirm the significance of this tendency.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Validation of the KDE likelihood approach discussed in Appendix E. Each subplot shows the marginalized posterior for the fraction of events contained within a narrow spike at χ eff = 0. Solid lines show posteriors computed using the KDE method, while dashed lines show posteriors obtained using ordinary Monte Carlo averaging (Appendix B). Results are shown for a variety of spike widths, from broad spikes with standard deviation ϵ = 0.03 to narrow spikes with ϵ = 10−4. We see that the KDE method yields consistent and convergent results as ϵ approaches zero, while the Monte Carlo averaging gives increasingly divergent results for small spike widths due to growing Monte Carlo errors.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: The fraction of binary black holes among GWTC-2 (solid blue line; Abbott et al. 2021c) with χ eff = 0, inferred using the GaussianSpike effective spin model. For comparison, the dashed black curve shows the result obtained using GWTC-3 (Abbott et al. 2021d); this is the same result shown in Figure 3 in the main text. Both results are consistent with one another, showing no evidence for a distinct subpopulation of events with χ eff = 0, although the GWTC-3 result more strongly favors ζ spike = 0.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: The χ eff distribution as inferred by a BimodalGaussian effective spin model, defined as the sum of two Gaussians (see Appendix A). Solid blue lines denote the 90% credible intervals, while blue light curves are select individual draws from the posterior. For reference, the dashed black curve shows the mean χ eff distribution as inferred using a single Gaussian. Both results are consistent with one another, indicating no evidence for bimodal features, narrow or otherwise, in the binary black hole χ eff distribution.
Paper: Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Takashi Tsukagoshi, Kenji Furuya, Takahiro Ueda
Figure caption: Integrated spectrum of the 12CO J = 3 − 2 line in the 0.″2 aperture (black solid line) with the uncertainty (gray shaded area) and a 3σ noise level (black dotted line). The gray dashed line indicates the synthetic spectra of the Huang et al. (2018) model with a Gaussian line profile, while the green solid line shows the best-fit model results using the Voigt line profile (see Section 2.3). Blue- and red-masked ranges are used to create the averaged visibilities for each wing. v denotes the velocity shift from the systemic velocity.
Paper: Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Takashi Tsukagoshi, Kenji Furuya, Takahiro Ueda
Figure caption: (a) UV distance vs. azimuthally averaged complex visibilities (black circles). The green points and gray dotted lines indicate the best-fit model and the cavity-sized uniform disk model, respectively. (b) Averaged intensity maps with Briggs weighting (robust = 0) for the redshifted and blueshifted line wings in the color scale and the black solid contour with 3σ and 5σ (σ = 0.38 mJy beam−1). The maps with natural weighting are shown in Figure 4. (c) 233 GHz continuum maps of Tsukagoshi et al. (2019). (d) Centroid velocity map. The white dashed circles in panel (b), (c), and (d) indicate the inner cavity radius (Andrews et al. 2016). The gray solid contour shows the dust continuum emission (Tsukagoshi et al. 2019). The contour starts from the brightness temperature of 10 K with an interval of 5 K.
Paper: Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Takashi Tsukagoshi, Kenji Furuya, Takahiro Ueda
Figure caption: Comparison of the observed averaged intensity maps with natural weighting and best-fit models. The residual maps are also plotted. The black contours start from 5σ with an interval of 5σ with σ = 0.23 mJy beam−1. We also show maps with finer resolution in Figure 2(b).
Paper: Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Takashi Tsukagoshi, Kenji Furuya, Takahiro Ueda
Figure caption: (a) Posterior distributions of the model parameters. (b) Best-fit midplane H2 density. (c) Best-fit gas surface density. The green solid lines show the best-fit model. The models with parameters randomly selected from the posterior distributions are plotted in light green.
Paper: Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Takashi Tsukagoshi, Kenji Furuya, Takahiro Ueda
Figure caption: (a) Radial profiles of the gas surface density. The green solid lines show the best-fit model. The models with parameters randomly selected from the posterior distributions are plotted in light green. The MMSN model and the Calahan et al. (2021) model are also shown in gray lines. The gray dotted lines indicate the gas surface density converted from the dust surface density of Macías et al. (2021), assuming a gas-to-dust surface density ratio of 10 and 100. In the right panel, we also show the gas surface density when the Toomre Q equals unity, and the gas surface density profiles starting from r = 10 au of the best-fit profile with fixing the total gas masses to 0.023 M ⊙ or 0.06 M ⊙. (b) The α viscosity parameter for each gas surface density profile, assuming a steady accretion disk.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Joint constraints on Bond albedo and the heat redistribution parameter, assuming that GJ 1252b radiates as a blackbody at its 4.5 μm brightness temperature. More heavily shaded regions indicate higher probabilities in the main panel, with the contour lines demarcating the enclosed 1σ, 2σ, and 3σ confidence intervals. The dashed lines in the 1D posterior distribution plots show the 95.4% (2σ) confidence limit for the indicated parameter. Our measurements of GJ 1252b constrain f > 0.40, A  B  < 0.41, and f(1 − A  B ) > 0.37.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Normalized dayside brightness temperatures, T  B,4.5 μm, of all super-Earths with infrared flux measurements plotted vs. planet radius (left) and ﹩{T}_{\mathrm{eq},\max }﹩ (right). The two smaller, cooler planets have 4.5 μm brightness temperatures consistent with no atmosphere and zero albedo, while the larger, hotter planets are significantly cooler and consistent with uniform redistribution of incident radiation and/or nonzero albedo.(The data used to create this figure are available.)