adsabs/AstroCLIMB huggingface dataset:
Paper: Investigating the Geotechnical Properties of the Lunar South Pole with NASA VIPER’s Mobility System
Authors: Erin Rezich, Valentin T. Bickel, Parker L. Francis, Arno Rogg, Antoine Tardy, Colin Creager, Heather A. Oravec, Alexander Schepelmann, Kimberly Ennico-Smith, Ariel Deutsch, Masatoshi Hirabayashi
Figure caption: VIPER engineering unit demonstrating “crabbing” driving maneuver.
Paper: Investigating the Geotechnical Properties of the Lunar South Pole with NASA VIPER’s Mobility System
Authors: Erin Rezich, Valentin T. Bickel, Parker L. Francis, Arno Rogg, Antoine Tardy, Colin Creager, Heather A. Oravec, Alexander Schepelmann, Kimberly Ennico-Smith, Ariel Deutsch, Masatoshi Hirabayashi
Figure caption: VIPER wheel with quadrature encoding metal finish pattern.
Paper: Investigating the Geotechnical Properties of the Lunar South Pole with NASA VIPER’s Mobility System
Authors: Erin Rezich, Valentin T. Bickel, Parker L. Francis, Arno Rogg, Antoine Tardy, Colin Creager, Heather A. Oravec, Alexander Schepelmann, Kimberly Ennico-Smith, Ariel Deutsch, Masatoshi Hirabayashi
Figure caption: Suspension Assembly torque transducer.
Paper: Investigating the Geotechnical Properties of the Lunar South Pole with NASA VIPER’s Mobility System
Authors: Erin Rezich, Valentin T. Bickel, Parker L. Francis, Arno Rogg, Antoine Tardy, Colin Creager, Heather A. Oravec, Alexander Schepelmann, Kimberly Ennico-Smith, Ariel Deutsch, Masatoshi Hirabayashi
Figure caption: Diagram showing the integrated control scheme.
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: Snapshots of simulated zonal wind profiles from TAM at an altitude z = 307 km. Ls values of 0°, 90°, 180°, and 270° correspond to northern vernal equinox, summer solstice, fall equinox, and winter solstice, respectively. Wind trends are most dynamic around the two equinoxes. The orange line represents the latitude of ingress (−9°), and the green line represents the latitude of egress (31°).
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: Best-match distributions of the angles of the refracted lightspots visible during occultation on the ingress and egress sides of Titan’s disk. Data are depicted in blue, and the model simulations with a starting atmosphere from the TAM simulation at Ls = 120° are depicted in red.
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: Distributions of the angles of the refracted lightspots visible during occultation on the ingress and egress side of Titan’s disk. Data are depicted in blue, and the model simulations (with an atmosphere corresponding to double the GCM wind speeds) at Ls = 30° are depicted in red.
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: Quantitative comparison of data and model can be achieved by treating Titan’s disk as a circle and expressing the sum of the distribution of light around its limb as a function of angle θ. This figure demonstrates this for a model frame near the center of the occultation. Both near- and far-limb spots are visible (inset), and when the sum of the light distribution around the limb is plotted, the peaks of the lightspots are found to be at θ = 156° and θ = −11°.
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: the color map shows line-of-sight CH3CN Doppler shifts, averaged across all observed transitions, overlaid on a Titan wireframe grid at the epoch of our ALMA observations. Velocity contours (labeled in units of m s−1) are also overlaid. Right: error map showing 1σ statistical uncertainties on the Doppler shift for each pixel. The spatial resolution (elliptical beam FWHM) is indicated in the lower left corner.
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 radial distortions (contours of level pressure) corresponding to the 36 zonal wind snapshots in Figure 10. The orange line represents the latitude of ingress (−9°), and the green line represents the latitude of egress (31°).
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: Distributions of the angles of the refracted lightspots visible during occultation on the ingress and egress side of Titan’s disk. Data are depicted in blue, and the model simulations (with an atmosphere corresponding to half the GCM wind speeds) at Ls = 120° are depicted in red.
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: Distributions of the angles of the refracted lightspots visible during occultation on the ingress and egress sides of Titan’s disk. Data are depicted in blue, and the model simulations are depicted in red. Model simulations correspond to a starting zonal wind profile derived from the ALMA data.
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: Zonal wind velocity profile (v(l)) and 1σ error envelope retrieved from our ALMA CH3CN observations on 2022-09-06, using a continuously variable parameterization with latitudinal sampling of 30°.
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 50 km.
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 Theia’s mantle fragments with 25% 25 km and 75% 50 km radii.
Paper: Europa’s Sodium and Potassium Exosphere during Juno’s Flyby
Authors: Emma Lovett, Carl Schmidt, Patrick Lierle
Figure caption: HIRES spectrum over Europa’s disk with the Na filter and 25 s integration time. Top panels: 2D spectra after different steps of data reduction. Bottom panels: spatial average of the above 2D spectrum. The middle and right 1D spectra share the right y-axis, as denoted by the red dotted line along zero Na. Left panels: 2D spectra after standard CCD corrections, order straightening, and flux calibration. Reflected sunlight overwhelms Europa’s atmospheric emission. Middle panels: spectrum after solar reflectance subtraction, where regions within ∼3 RE are masked out because self-subtracted noise levels preclude accurate recovery of exospheric emission. Very broad faint Iogenic Na background emission is evident, blueshifted by ∼2 Å. Right panels: spectrum after interpolation and subtraction of Iogenic emission, which is assumed uniform across the slit length.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: A suite of Titan phase curves taken at different wavelengths. At each wavelength, extreme forward scattering is apparent at high phase angles, even at wavelengths where the disk of Titan appears dim when observing at low phase angles (e.g., 4.0 μm). The effect is strong enough that Titan’s disk-averaged brightness is greater at high phase than at low phase for almost all wavelengths. The top-left phase curve, taken at 0.88 μm, suffers from saturation-related issues at high phase.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: A near-full-phase AgΦ(α) spectrum of Titan. Data from E. Karkoschka (1998) are included for comparison. The spectrum was obtained by taking the disk-averaged spectra of 10 cubes with phase angle α < 3°. Data were acquired at very low phase angle and, thus, approximate the geometric albedo spectrum of Titan. Certain spectral features and their sources are also identified. Features at 3.31 μm and 4.54 μm are discussed in Section 4.2. Features in the Cassini data are consistent with the model results from M. Es-sayeh et al. (2023) and recent James Webb Space Telescope data from C. A. Nixon et al. (2025).
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: AgΦ(α) of Titan as a function of wavelength and phase angle. Vertical black lines indicate phase angles at which there were no cubes to consider. Bright horizontal bands are associated with continuum between strong methane absorption bands.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Major steps in the disk detection process on two cubes: (far left) an unaltered cube; (center left) edge pixels identified using Canny edge detection—some pixels along terrain boundaries are falsely identified as edge pixels; (center right) the accumulator array after applying a circle Hough transform; (far right) the final array, containing only data from the disk of Titan. Data were taken at 2 μm.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Left: a selection of approximate planetary phase functions from across the near-infrared spectrum accessible to VIMS-IR. The colors of fits are indicative of the VIMS-IR band at which they were generated. Curves are normalized to 10° due to a sparse set of data at phase angles below 10°. Right: the value of Titan’s planetary phase function Φ(α) at the max phase angle in our data set, α = 165°. The magnitude of this value broadly scales with wavelength. Some dips within the structure correspond to spectral continuum regions, similar to features in the infrared spectrum of Titan (gray; spectrum averaged over all cubes).
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Comparison of Titan (orange) and Earth (blue) phase-dependent brightness in color–color space. Earth values are from spectral models in T. D. Robinson et al. (2010). Adopted spectral elements at 1.08, 1.28, and 1.60 μm are continuum for both worlds and within the anticipated spectral coverage for HWO. Point saturation indicates phase angle, indicating that Earth and Titan separate well in this color–color space except at very large phase angles.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Top: a comparison of two phase curves from the present work (3.00 μm in teal; 5.00 μm in red) and two phase curves from A. García Muñoz et al. (2017; 569 nm in light gray; 938 nm in dark gray). Phase curves are normalized to their respective lowest-phase observation and offset from one another for clarity. Bottom: a comparison of the 938 nm phase curve from A. García Muñoz et al. (2017) with our phase curve at 933 nm. The curves share a similar shape, though our phase curve has much more noise because of saturation issues.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Comparison of a Titan phase curve at a continuum wavelength (0.9 μm) to Earth’s broadband visible phase curve (data from E. Pallé et al. 2003; J. Qiu et al. 2003).
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Non–local thermodynamic equilibrium emission signatures in the spectrally resolved phase curves of Titan. As explained in the text, the feature at 4.54 μm is likely affected by issues related to the instrument or cube calibration.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Images of Titan at 3.31 μm (left) and 4.54 μm (right), showing source locations of emission.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: The spatial distribution of cubes by their subspacecraft coordinates. Most cubes used in the present study were acquired in quick succession by Cassini during Titan passes, hence the clustering.
Paper: Extreme Forward Scattering Observed in Disk-averaged Near-infrared Phase Curves of Titan
Authors: Chase Cooper, Tyler D. Robinson, Jason W. Barnes, L. C. Mayorga, Lily Robinthal
Figure caption: Images from identified “Cbright” flyby groups displaying likely cloud structures. Images are taken at 2.8 μm.
Paper: Deuterated Water Ice on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, M. Ryleigh Davis, Swaroop Chandra
Figure caption: The continuum-divided spectra of the Saturnian satellites, in the region of the O–D absorption. The red line shows a Gaussian fit to the data using a fixed width. Most satellites have separate measurements for the leading and trailing hemispheres, but Hyperion and Phoebe, which are not synchronously rotating, only have single measurements. The O–D absorption is robustly detected at nearly every satellite.
Paper: Deuterated Water Ice on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, M. Ryleigh Davis, Swaroop Chandra
Figure caption: The ratio of the depth of the 4.14 μm absorption to 2 μm absorption for each of the satellites. The leading hemispheres are shown as black points, while the trailing hemispheres are red. Hyperion and Phoebe, which are nonsynchronously rotating, are shown in blue. The D/H value derived using the C19 calibration is shown on the right. The value measured for Enceladus is shown as the bold horizontal line, while the 1σ upper and lower limits are shown as thinner dashed lines. The D/H value shown for Phoebe is derived from calibration to a radiative transfer model, rather than from the 4.14-to-2 μm depth ratio.
Paper: Deuterated Water Ice on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, M. Ryleigh Davis, Swaroop Chandra
Figure caption: A comparison of the continuum-divided JWST spectrum of Phoebe and the VIMS spectrum of Phoebe from C19. Also shown is the average spectrum of all of the Saturnian satellites with robust 4.14 μm absorption detections. The JWST data rule out an absorption with the position and depth of that seen by VIMS at the 10σ level.
Paper: Deuterated Water Ice on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, M. Ryleigh Davis, Swaroop Chandra
Figure caption: JWST spectrum of the leading hemisphere of Dione with an inset highlighting the 4.14 μm O–D stretch absorption and the 4.26 μm CO2 absorption.
Paper: Atomic-scale Insights into the Effects of Diffusion on the Binding of Adsorbed Sodium on the Surfaces of the Moon and Mercury
Authors: Anastasis Georgiou, Amanda Ricketts, Jason McLain, Sébastien Verkercke, François Leblanc, Menelaos Sarantos, Liam S. Morrissey
Figure caption: Mean squared displacement (MSD) of Na atoms in (a) crystalline anorthite, (b) crystalline albite, (c) crystalline silica, (d) amorphous anorthite, (e) amorphous albite, and (f) amorphous silica.
Paper: Atomic-scale Insights into the Effects of Diffusion on the Binding of Adsorbed Sodium on the Surfaces of the Moon and Mercury
Authors: Anastasis Georgiou, Amanda Ricketts, Jason McLain, Sébastien Verkercke, François Leblanc, Menelaos Sarantos, Liam S. Morrissey
Figure caption: Distribution of adsorbed Na atoms on (a) a crystalline and (b) an amorphous silica surface at 100 K. Red particles, O atoms; beige particles, Si atoms; purple particles, Na atoms.
Paper: Atomic-scale Insights into the Effects of Diffusion on the Binding of Adsorbed Sodium on the Surfaces of the Moon and Mercury
Authors: Anastasis Georgiou, Amanda Ricketts, Jason McLain, Sébastien Verkercke, François Leblanc, Menelaos Sarantos, Liam S. Morrissey
Figure caption: Mean binding energy (BE) of Na atoms and number of desorbed Na atoms with time. The shapes represent the BE, whereas the lines represent the desorbed Na atoms.
Paper: Atomic-scale Insights into the Effects of Diffusion on the Binding of Adsorbed Sodium on the Surfaces of the Moon and Mercury
Authors: Anastasis Georgiou, Amanda Ricketts, Jason McLain, Sébastien Verkercke, François Leblanc, Menelaos Sarantos, Liam S. Morrissey
Figure caption: Binding energy and depth location of Na atoms on amorphous silica at (a) 700 K and (b) 300 K at the beginning and end of the simulation.
Paper: Atomic-scale Insights into the Effects of Diffusion on the Binding of Adsorbed Sodium on the Surfaces of the Moon and Mercury
Authors: Anastasis Georgiou, Amanda Ricketts, Jason McLain, Sébastien Verkercke, François Leblanc, Menelaos Sarantos, Liam S. Morrissey
Figure caption: Binding energy distribution of Na atoms at 100 K for the different silicates.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Comparison of different topographic shapes for the ramparts. Left column: flat topography. Middle column: hill-shaped ramparts (reference run, simulation R). Right column: lake in a depression. Top row shows the horizontal wind at 2 a.m. Bottom row shows the CH4 mixing ratio at 2 a.m. Note the position of the lake breeze front around 75 km for the hill-shaped ramparts, 85 km for the flat topography, and 95 km for the lake in a depression, materialized by a steep change in horizontal wind and methane mixing ratio.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Reference simulation: evolution with time of the (a) latent heat flux to the surface and (b) surface temperature and air temperature at different locations (0, 5, and 9 km: above the lake; 10, 25, and 295 km: above land). (c) Horizontal wind at 2 m above the surface, i.e. the first horizontal level of the model (positive values indicate wind blowing to the right), (d) vertical wind at ≈200 m above the surface (positive values indicate upward wind), and (e) turbulent kinetic energy (TKE) at ≈200 m above the surface. The time axes start at the end of the 4th tsol, at midnight. The blue bar at the bottom of the plots shows the location of the lake. The orange bars show the location of the ramparts.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Effect of the surface properties of the ramparts on the lake breeze (winds, methane, temperature, and turbulence). We compare the reference simulation (in which ramparts have the same surface properties as the rest of the land) with the high-roughness case (see Section 3.3.1), the high-albedo case (see Section 3.3.2), and the high-thermal-inertia case (see Section 3.3.3). Row 1: horizontal wind at 2 a.m. Row 2: horizontal wind evolution at 2 m (the horizontal dashed lines show the location of the slices presented in Row 1). Row 3: TKE at 2 p.m.. Row 4: difference of latent heat flux compared to the reference (positive means more evaporation). Row 5: difference of surface temperature compared to the reference. Row 6: difference of air temperature at 2 m above the surface compared to the reference.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Top left: fluxes to the surface, in W m−2, at 10 km from the center of the domain (i.e., at the foot of the rampart) and at 25 km from the center of the domain (i.e., at the top of the rampart.). Top right: virtual potential temperature at 2 p.m. Bottom: mechanisms explaining the upslope winds on Titan. The gradient of potential temperature on the slopes is created by the difference of infrared flux emitted by the surface, which is colder in altitude and thus emits less infrared. Note the negative vertical gradient in potential temperature at the rampart surface. We observe upslope winds 24 hr a day.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Dry simulation. Left column: horizontal wind. Right column: vertical wind. Top row: circulation at 2 p.m. Bottom row: evolution of horizontal wind at 2 m above the surface (c) and evolution of vertical wind at 200 m above the surface (d). The orange bars below the plots show the ramparts’ location.
Paper: Ramparts around Lakes on Titan Impact Winds and Methane Evaporation
Authors: Enora Moisan, Audrey Chatain, Scot Rafkin, Alejandro Soto, Shannon MacKenzie, Aymeric Spiga
Figure caption: Wind circulation in the reference simulation. Left column: at 2 a.m. Right column: at 2 p.m.. Top row: horizontal wind. Bottom row: vertical wind. The blue bar under the plots shows the position of the lake. The orange bar corresponds to the rampart position.