adsabs/AstroCLIMB huggingface dataset:
Paper: Lake Stars as an Earth Analog for Europa’s Manannán Crater Spider Feature
Authors: Lauren E. Mc Keown, Elodie Lesage, Jennifer E. Scully, Erin J. Leonard, Robert T. Pappalardo, Marjorie Potter, Victor Tsai, Mathieu Choukroun, Elodie Gloesener, Serina Diniega, Nicholas Hatcher, Duncan McBryde
Figure caption: Lake stars in Breckenridge, CO. (a) A dendritic lake star at Maggie pond with third-order branches. (b) A baby lake star (left) next to a more developed feature but with only second-order branches (right). (c) Lake stars at Ollie's Pond with Darcy flow lines, indicative of water flow through porous snow, preserved. (d) A “tendril” with a rock aimed at it to show that the feature is solid clearer ice surrounded by more frosted ice. (e) Clear rows of “protostars” (left) and larger, more dendritic lake stars closer to a building in its shadow and possibly more cold trapped (right). (f) A group of well-developed dendritic lake stars at Maggie Pond’s edge. (g) Several layers of ice, burying lake stars at Ollie Pond. (h) A 2 inch sample of ice demonstrating that the lake star pattern is transparent ice surrounded by more frosted ice.
Paper: Lake Stars as an Earth Analog for Europa’s Manannán Crater Spider Feature
Authors: Lauren E. Mc Keown, Elodie Lesage, Jennifer E. Scully, Erin J. Leonard, Robert T. Pappalardo, Marjorie Potter, Victor Tsai, Mathieu Choukroun, Elodie Gloesener, Serina Diniega, Nicholas Hatcher, Duncan McBryde
Figure caption: Cartoon of the hypothesized formation process showing a “cutout” of Europa’s ice shell. (a), (b) An impactor hits the surface of Europa, forming Manannán crater. (c) A transient atmosphere develops from the vaporized ejecta. (d) A brine reservoir develops beneath the surface. (e) Freezing of the reservoir triggers fracture of the ice above, and liquid erupts at the surface. (f) The erupted liquid spreads through the porous ice layer, forming the spider-like pattern observed in Manannán. Image Credit: Wax Visuals, https://waxvisuals.com/.
Paper: Lake Stars as an Earth Analog for Europa’s Manannán Crater Spider Feature
Authors: Lauren E. Mc Keown, Elodie Lesage, Jennifer E. Scully, Erin J. Leonard, Robert T. Pappalardo, Marjorie Potter, Victor Tsai, Mathieu Choukroun, Elodie Gloesener, Serina Diniega, Nicholas Hatcher, Duncan McBryde
Figure caption: Image of a Martian spider at −87.95°N, 91.726°E showing how a dendritic spider pattern might appear “asterisk like” at lower resolutions. (a) An example of a spider (300 m in diameter) in the Murray Lab CTX global mosaic (6 km pixel–1). (b) The spider in a HiRISE image (25 cm pixel–1).
Paper: Lake Stars as an Earth Analog for Europa’s Manannán Crater Spider Feature
Authors: Lauren E. Mc Keown, Elodie Lesage, Jennifer E. Scully, Erin J. Leonard, Robert T. Pappalardo, Marjorie Potter, Victor Tsai, Mathieu Choukroun, Elodie Gloesener, Serina Diniega, Nicholas Hatcher, Duncan McBryde
Figure caption: (a) Erupted volume and (b) critical freezing time of a brine reservoir as a function of its radius and depth bellow the surface (E. Lesage et al. 2022). The dark-blue area shows reservoirs that cannot trigger eruptions because of the viscous rheology of the surrounding ice, where viscosity decreases with depth. The area in the white dashed line shows the possible range of characteristics of the source brine reservoir inferred from the erupted volume range calculated in Section 3.
Paper: JWST/NIRSpec Observations of Salacia-Actaea and Máni: Exploring Population-level Trends among Water-ice-rich Kuiper Belt Objects
Authors: Ian Wong, Bryan J. Holler, Silvia Protopapa, Aurélie Guilbert-Lepoutre, William M. Grundy, John A. Stansberry, Heidi B. Hammel, Stefanie N. Milam, Rosario Brunetto, Joshua P. Emery, Estela Fernández-Valenzuela, Noemí Pinilla-Alonso
Figure caption: Plot of the measured band depths of the 2 μm H2O (top), 3 μm H2O (middle), and ∼4.25 μm fundamental CO2 absorption features as a function of V-band absolute magnitude HV for H2O-type objects. The points are color coded by dynamical class. The band depths for Salacia and Máni are highlighted by the larger markers and labeled “S” and “M,” respectively. The three brightest/largest H2O-type members of the resonant KBO population (orange squares) are, in order, Charon, Orcus, and Achlys. The band-depth values, absolute magnitudes, and dynamical classifications shown in this figure are available as a machine-readable data behind the figure file.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: JWST/NIRSpec Observations of Salacia-Actaea and Máni: Exploring Population-level Trends among Water-ice-rich Kuiper Belt Objects
Authors: Ian Wong, Bryan J. Holler, Silvia Protopapa, Aurélie Guilbert-Lepoutre, William M. Grundy, John A. Stansberry, Heidi B. Hammel, Stefanie N. Milam, Rosario Brunetto, Joshua P. Emery, Estela Fernández-Valenzuela, Noemí Pinilla-Alonso
Figure caption: A selection of 4.0–4.5 μm reflectance spectra of H2O-type KBOs, normalized to unity at 4.3 μm. The spectra are arranged from top to bottom in order of increasing object size. The vertical dotted line at 4.27 μm denotes the expected band center for crystalline CO2 ice. The larger objects display distinctly broader and blueshifted absorption features than the smaller KBOs. The spectrum of Charon, obtained with the high-spectral-resolution G395H grating of NIRSpec, reveals complex fine structure within the CO2 band. The black curve shows the same spectrum convolved to the lower spectral resolution of the PRISM grating.
Paper: JWST/NIRSpec Observations of Salacia-Actaea and Máni: Exploring Population-level Trends among Water-ice-rich Kuiper Belt Objects
Authors: Ian Wong, Bryan J. Holler, Silvia Protopapa, Aurélie Guilbert-Lepoutre, William M. Grundy, John A. Stansberry, Heidi B. Hammel, Stefanie N. Milam, Rosario Brunetto, Joshua P. Emery, Estela Fernández-Valenzuela, Noemí Pinilla-Alonso
Figure caption: The reflectance spectra of Salacia (top) and Máni (bottom), normalized to unity at 2.5 μm. The detected absorption bands of H2O and CO2 ice are labeled. The red triangles correspond to the location of the 1.65 μm H2O-ice spectral feature that likely indicates the crystalline phase, which is clearly discernible in the spectrum of Máni. The inverted orange triangles mark the 3.1 μm Fresnel reflection peak of H2O ice.
Paper: JWST/NIRSpec Observations of Salacia-Actaea and Máni: Exploring Population-level Trends among Water-ice-rich Kuiper Belt Objects
Authors: Ian Wong, Bryan J. Holler, Silvia Protopapa, Aurélie Guilbert-Lepoutre, William M. Grundy, John A. Stansberry, Heidi B. Hammel, Stefanie N. Milam, Rosario Brunetto, Joshua P. Emery, Estela Fernández-Valenzuela, Noemí Pinilla-Alonso
Figure caption: The reflectance spectra of Salacia (blue) and Máni (green) alongside the sample of H2O-type KBOs (black) from N. Pinilla-Alonso et al. (2025), illustrating the broad similarities in overall continuum shape and absorption bands. The average CO2-type KBO (orange) and organics-type KBO (red) spectra are also included for comparison. All spectra have been normalized to unity at 2.5 μm.
Paper: JWST/NIRSpec Observations of Salacia-Actaea and Máni: Exploring Population-level Trends among Water-ice-rich Kuiper Belt Objects
Authors: Ian Wong, Bryan J. Holler, Silvia Protopapa, Aurélie Guilbert-Lepoutre, William M. Grundy, John A. Stansberry, Heidi B. Hammel, Stefanie N. Milam, Rosario Brunetto, Joshua P. Emery, Estela Fernández-Valenzuela, Noemí Pinilla-Alonso
Figure caption: Wavelength-averaged IFU images from the first dithered exposures of Salacia and Máni. A logarithmic stretch was applied to the flux scaling to highlight the PSF shapes and background variations. The black dots and circles denote the best-fit centroid positions and the spectral extraction apertures, respectively. In the case of Máni, the masked pixels across the field of view correspond to relatively bright background sources that were flagged prior to spectral extraction (see text for details).
Paper: Prebiotic Chemistry Insights for Dragonfly: Thermodynamics of Amino Acid Synthesis in Selk Crater on Titan
Authors: Ishaan Madan, Ben K. D. Pearce
Figure caption: Thermodynamic validation of our Cantera framework against B. K. D. Pearce & R. E. Pudritz (2016). Equilibrium yields (expressed as product in kg units/water in kg units) are plotted for four nucleobase-forming reactions: (a) 5 HCN → adenine, (b) HCN + NH3 + H2O → adenine, (c) 3 HCN + CH2O → cytosine, and (d) 5 HCN + H2O → guanine + H2. Olive solid lines with circle markers show the results of our Cantera equilibrium calculations using NASA-9 polynomial coefficients derived from CHNOSZ data, while black dashed lines with square markers reproduce the mass-yield trends reported by B. K. D. Pearce & R. E. Pudritz (2016). The maximum deviation across all reactions within 0 °C–250 °C is <5%. The vertical dashed gray line at 311 °C denotes the boiling point of water at a pressure of 100 bar.
Paper: Prebiotic Chemistry Insights for Dragonfly: Thermodynamics of Amino Acid Synthesis in Selk Crater on Titan
Authors: Ishaan Madan, Ben K. D. Pearce
Figure caption: Validation of the Gibbs free energy estimator using glycine. Black line shows the raw QC results across temperature, which exhibit a monotonic increase. The red line applies the analog-slope correction described in the main manuscript, which matches the CHNOSZ trend to within 17%. Olive square markers show the reference CHNOSZ database values.
Paper: Prebiotic Chemistry Insights for Dragonfly: Thermodynamics of Amino Acid Synthesis in Selk Crater on Titan
Authors: Ishaan Madan, Ben K. D. Pearce
Figure caption: Heat map of amino-acid percent yields at 0°C relative to the starting HCN inventory in our fiducial models with a 10% survival factor. Columns correspond to varying NH3 concentrations (0%–10% of the total water content). Rows list the 21 amino acids evaluated. Cell shading follows a viridis scale from 0% (purple) to 100% (yellow).
Paper: Prebiotic Chemistry Insights for Dragonfly: Thermodynamics of Amino Acid Synthesis in Selk Crater on Titan
Authors: Ishaan Madan, Ben K. D. Pearce
Figure caption: Heat maps of amino-acid percent yields at 0°C relative to the starting HCN inventory with 1% and 30% survival factors for the initial organic inventory. Columns correspond to varying NH3 concentrations (0%–10% of the total water content). Rows list the 21 amino acids evaluated. Cell shading follows a viridis scale from 0% (purple) to 100% (yellow).
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: Orbit fit quality (χ2 per degree of freedom) as a function of Quaoar’s J2 and Weywot’s inclination (with respect to Quaoar’s equatorial plane). Red dashed lines show the values expected from the undifferentiated oblate and triaxial shape models. The red cross shows the J2 and inclination value measured in the constrained orbit fit. We note that the best fit quality is at J2 ∼ 0.4, but we limit the range of J2 displayed to better show the fit quality at more realistic values of Quaoar’s J2. For reference, the p-value of ﹩{\chi }_{\mathrm{pdf}}^{2}=1﹩ (1.8) is 0.46 (0.01).
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: Resonance splitting of Weywot’s 6:1 MMR based on the constrained fit, the differentiated occultation model, the differentiated light-curve model, and the unconstrained fit. The various 6:1 subresonances are shown as dashed black lines, with the nominal location of the resonance shown in blue. Quaoar’s 3:1 SOR is shown with green lines. Ring detections of Q1R (B. Morgado et al. 2023; C. Pereira et al. 2023; B. Proudfoot et al. 2025) are displayed as shaded red regions (with ring radius and ring width), where darker shading is associated with more numerous ring detections. For realistic values of Quaoar’s J2 (i.e., all except the unconstrained model), Weywot’s 6:1 is on the inner edge of the ring, possibly providing a confinement mechanism against inward viscous spreading.
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: J2 values for Quaoar as a function of core size and core density assuming a two-layer interior structure model with spherical cores (left) and triaxial cores (right). The two-layer interior model consists of a rocky core (with chosen core density) surrounded by a partially differentiated shell of mixed ice and rock. Points at core radii of 0 km correspond to an undifferentiated model, and the maximum core radii correspond to a fully differentiated body with a shell density of water ice (920 kg m−3). Core densities are chosen to bound likely core densities of TNOs with 2600 kg m−3 corresponding to hydrated rock and 3800 kg m−3 corresponding to dehydrated rock.
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: A corner plot showing the posterior distribution from our constrained orbit fit. Along the diagonal are the marginal (1D) posterior distributions for each parameter alongside the 2D joint posterior distributions for each pair of parameters. Contours on the joint distributions show the 1σ, 2σ, and 3σ confidence regions, and black points correspond to individual samples from the MCMC chain.
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: The COL-COB offsets implied by our constrained (left) and unconstrained (right) orbit fits. The COL is shown as a red ellipse (based on the orbit fit posterior) and the COB is marked with a black cross. Quaoar is shown as a sphere with an angular diameter of 36 mas. The equator and subobserver longitude are shown with blue lines. Over our observational baseline, a constant offset in ecliptic latitude and longitude is a good approximation of a COB-COL offset caused by longitudinal albedo features.
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: The architecture of the Quaoar system, as seen from Earth, shown to scale on 2006 September 21 12:00 UT. Locations of various SORs and MMRs are shown as colored ellipses. Quaoar's pole orientation, ring width, and ring orientation are based on B. Proudfoot et al. (2025). Quaoar’s shape is based on G. Margoti (2024), although the rotational phase is unknown, but selected to be at light-curve maximum. Weywot’s diameter is from E. Fernandez-Valenzuela et al. (2025, in preparation). Weywot's orbit is from this work.
Paper: Beyond Point Masses. V. Weywot’s Non-Keplerian Orbit
Authors: Benjamin Proudfoot, Will Grundy, Darin Ragozzine, Estela Fernández-Valenzuela
Figure caption: Similar to Figure 2 but for the unconstrained orbit fit.
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: The top panels show the diamond-shaped caustic (concentration of light rays) that results from a planet with a uniformly rotating, oblate atmosphere (depicted as a black oval, top left panel). The black lines represent refracted starlight, and the caustic is highlighted in red. The top right panel depicts a magnified version of the caustic for the atmosphere on the left, showing the abrupt variations in flux that are present. Observation chords intersecting the caustic show rapid changes in flux at the center of an occultation event, allowing observers to determine the shape of the caustic. The bottom panels show the caustic that is formed in an alternative case: when the atmosphere is not uniformly rotating, but rather has a strong zonal wind in the north causing atmospheric distortion (highlighted by the red flattened circle outline). The distorted atmosphere produces a triangle-shaped caustic (the red triangle in the middle of the bottom left panel); the caustic and its flux variations are depicted in the bottom right panel. As in the case of the oblate atmosphere, observation chords that intersect the caustic capture variations in flux that allow mapping of the caustic. As caustics are highly sensitive to nonspherical distortions, observations of the central flash allow observers to determine the shape of Titan’s atmosphere and therefore the zonal wind profile at the time of the occultation. (From Figures 9 and 10 of B. Sicardy 2022.)
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: Peak-normalized wind contribution function for the observed CH3CN J = 35–34 transitions at 643 GHz.
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: (a) The atmospheric temperature profile derived by the HASI instrument on board the Huygens probe. (b) Pressure is calculated from the temperature profile by leveraging the law of hydrostatic equilibrium and approximating Titan’s atmosphere as 100% nitrogen. (c) The integrated line-of-sight refractivity is found by stepping across 8000 km chords with step size = 1 km. At each step, refractivity ν is calculated, and the integrated line-of-sight refractivity is the sum of ν · ds across the chord. (d) Bending angles are calculated from the gradient of the phase delay screen. The orange vertical line in panels (b)–(d) denotes Titan’s surface.
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: Main figure: path of the star (from the vantage point of Maunakea) as it is occulted by Titan. Red plus signs represent 1-minute increments. The center of the occultation shadow path passes within 50 km of Maunakea, making this site ideal for perceiving the “central flash” (rapidly changing stellar refraction patterns) that occurs near the center of the occultation shadow path. Inset: full shadow path of star 2MASS 21312124–1602427, Kmag = 12.9. The hatched line represents the center of the shadow path; solid lines are the outer edges.
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: Continuum-subtracted ALMA observations of Titan on 2022-09-06, showing the spectrally integrated line flux maps for the CH3CN J = 35–34 and J = 36–35 bands (left panels) and corresponding spectra (right panels), integrated within a ﹩1\mathop{.}\limits^{^{\prime\prime} }2﹩-diameter circular aperture centered on Titan. The FWHM of the spatial resolution element (ellipse) is shown in the lower left corner of the maps.
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: Top: linear fits (green and pink lines) to calculate x- and y-offsets between the centers of Titan and the occulted star. Bottom: residuals in the x- (left) and y-directions (right) following the subtraction of the fit.
Paper: Zonal Winds in Titan’s Middle Atmosphere from a Stellar Occultation Observed with Keck Adaptive Optics
Authors: Theresa C. Marlin, Eliot F. Young, Katherine de Kleer, Martin Cordiner, Nicholas A. Lombardo, Imke de Pater, Juan M. Lora, Paul Corlies, Richard Cosentino, Conor Nixon, Sébastien Rodriguez, Alexander Thelen
Figure caption: Left: reduced data from pre-event. Scattered light around both Titan and the star are caused by Earth’s atmosphere. Right: the same frame following Richardson–Lucy deconvolution. Circle center and radius determined by fitting a circle to radial gradient minima around the limb.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Snapshots of compositional (panels (a)–(d)) and temperature (panels (e)–(h)) field for the twice-higher-density Theia case (B = 2) compared to the reference case.
Paper: Survival of Asteroid-sized Debris from the Moon-forming Impactor in Earth’s Deep Mantle with Implications for Its Solar System Provenance
Authors: Qian Yuan
Figure caption: Compositional snapshots of Theia’s mantle fragments with a uniform radius of 25 km.