adsabs/AstroCLIMB huggingface dataset:
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: The weighted mean density (red) and weighted density gradient/km (blue) for the four PSRs from Table 2 and the Shackleton PSR (M. T. Zuber et al. 2012) against the ice area% (J. Ando et al. 2025). The mean density decreases with increasing ice area, and the density gradient decreases as the ice area% decreases.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: (a) Bouguer gravity, 148 < L < 936, at a radius of 1743.4 km; (b) Bouguer gravity for 148 < L < 936, at a radius of 1738.0 km. Panel (a) is close to the average radius of the three highest sites; panel (b) is the reference level of the gravity model and more representative of the radii of the other 17 sites.
Paper: The Adjacency Effect at Kivu Lacus
Authors: Shannon M. MacKenzie, Jason W. Barnes, William J. Miller
Figure caption: SRTC++ simulated images of Kivu Lacus as a function of photon scattering history for scenarios B and C (land albedo = 0.1, lake albedo = 0). (First column): the total I/F; column (1): the fraction of photons that scatter only in the atmosphere; column (01): the fraction that scatter off the surface (lake or land) and then in the atmosphere; column (101): the fraction that scatter in the atmosphere, then the surface, then the atmosphere; column (011): the fraction that scatter off the surface, then twice in the atmosphere; and column (010): the fraction that scatter off the surface, in the atmosphere, then off the surface. (Top) At 5 μm, the BRDF modifies the directionality of the adjacency effect. (Bottom) At 2 μm, directionality is a <1% effect. North is up.
Paper: The Adjacency Effect at Kivu Lacus
Authors: Shannon M. MacKenzie, Jason W. Barnes, William J. Miller
Figure caption: (a) Distance of the adjacency effect (σ); (b) amplitude of the bright/dark contrast (a); and (c) goodness of fit of the logistic model (R2) to SRTC++ simulations of the entire shore of Kivu Lacus. Means are represented as points with bars representing 95% confidence intervals.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Initial angle α0 of the illuminated slope (top) and angle β0 on the shadowed side (bottom) over pressure for intensities of 4670 ± 690 W m−2 (triangles) and 1850 W m−2 (circles). Open symbols: wet sample. Filled symbols: dry sample. Dashed and solid blue lines mark the mean from all measurements for the wet and dry samples, respectively. Error bars mark the variety (standard deviation) of an individual slope. The systematic error of 5% is also included in this error bar (added to the standard deviation).
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Sketch of the experimental setup. Top: overview of the setup. The cameras are placed outside the vacuum chamber, with observations made through a vacuum viewport (not shown) for the visible-light camera and an IR window (not shown) for the thermal camera. Bottom: the part of the setup inside the vacuum chamber. Left: before the measurement. The bottom part of the funnel is in contact with the sandpaper and forms part of the sample container. Right: before the measurement begins, the funnel is raised, and a pile of particles forms.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: The definition of angles α and β.
Paper: Survivability of Amino Acids in Lunar Soil
Authors: Li Hsia Yeo, Hannah McLain, Sophia Westerkamp, Danielle Simkus, Jennifer Holt, Jason McLain
Figure caption: Survivability of amino acids in lunar soil exposed to 1 hr of vacuum, hydrogen gas, and UV/plasma conditions. Recovered amino acids were extracted from the “dust” (JSC 1A removed from the treatment test tube) as well as the “wash” (where the emptied treatment test tube was flushed with ultrapure water, which was then analyzed). Each experimental trial was conducted in triplicate with error bars reflecting standard error.
Paper: Survivability of Amino Acids in Lunar Soil
Authors: Li Hsia Yeo, Hannah McLain, Sophia Westerkamp, Danielle Simkus, Jennifer Holt, Jason McLain
Figure caption: Survivability of amino acids in lunar soil exposed to different amounts of radiation. Five minutes of irradiation time in the laboratory is equivalent to the Lyα dose on the lunar surface for 10.8 lunations. Each experimental trial was conducted in triplicate with error bars reflecting standard error.
Paper: Survivability of Amino Acids in Lunar Soil
Authors: Li Hsia Yeo, Hannah McLain, Sophia Westerkamp, Danielle Simkus, Jennifer Holt, Jason McLain
Figure caption: Apparatus used to expose amino acids in lunar simulant to lunar-like conditions alongside a close-up schematic of the treatment region. Lunar simulant soil and amino acid samples are placed in a glass test tube and evacuated to 10−7 Torr. Hydrogen gas is then precision-leaked into the test tube, and a microwave cavity is set up over the test tube to generate hydrogen plasma/UV radiation inside.
Paper: Survivability of Amino Acids in Lunar Soil
Authors: Li Hsia Yeo, Hannah McLain, Sophia Westerkamp, Danielle Simkus, Jennifer Holt, Jason McLain
Figure caption: Extraction procedure: After plasma irradiation, all samples were (1) transferred to a centrifuge tube, (2) where 3 ml of water was added. (3) The sample was centrifuged. (4) Then, 500 μl was removed for initial analysis. (5) The remainder of the sample was sonicated at room temperature for 1 hr and (6) centrifuged. (7) An additional 500 μl aliquot was removed and dried down under vacuum. (8) Samples were AccQ·Tag derivatized for 10 minutes at 55°C and analyzed using an Acquity H-class plus connected to a Xevo TQ-S Micro triple quadrupole mass spectrometer.
Paper: Meteoroid Streams Sculpt the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina, A. R. Poppe, Karl Battams, D. J. McComas
Figure caption: Impact rates in 8 hr intervals (dots) from orbits 1–19 for each orbital group as a function of radial distance. The left portion shows the inbound, preperihelion arc of the orbit, and the right portion shows the outbound, postperihelion portion of the orbit. The average value is given by the solid black line, with 25% and 50% of the average value shown in gray. Each orbitally grouped rate is shown on the same logarithmic scale. The green shaded region indicates the portion of orbits 10–16 identified as being dominated by α-meteoroids (J. R. Szalay et al. 2024), and the green arrows indicate the expected peak impact rate location rk for α-meteoroids on perfectly circular orbits. PSP’s orbital period within each group is listed to the far right.
Paper: Meteoroid Streams Sculpt the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina, A. R. Poppe, Karl Battams, D. J. McComas
Figure caption: (a) Radial volumetric number density profile (G. Stenborg et al. 2021) for grains with radii >1 μm (J. R. Szalay et al. 2021) shown by the solid line and with 50% variability (gray circles). (b) Integrated line-of-sight column density for the volumetric densities in panel (a). (c) Residual between the analytic radial density profile and our simulated 50% variability density profile. Above panel (a) are the perihelion distances for all known comets and asteroids inside 1 au from the NASA/JPL Solar System Dynamics database.
Paper: Meteoroid Streams Sculpt the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina, A. R. Poppe, Karl Battams, D. J. McComas
Figure caption: (a) Time for dust grains to spiral into the Sun via PR drag. (b) Gyroradii of dust grains at 0.1 au and 1 au, where the width is dictated by the range of assumed grain pickup speeds (solar wind speeds) of 400−2400 km s−1. Green and gray shaded regions show the relevant size ranges for bound α-meteoroids detectable by FIELDS and WISPR, respectively, while the purple region in panel (b) shows the relevant size range for β-meteoroids.
Paper: Meteoroid Streams Sculpt the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina, A. R. Poppe, Karl Battams, D. J. McComas
Figure caption: Radial distance traveled by different grain size populations over a timescale representative of PSP’s orbital period, 100 days. The width of the Geminids is marked with a red rectangle, with a lighter factor of 2× uncertainty in pink (K. Battams et al. 2025), and PSP’s detectable impact size is shown with the gray region (J. R. Szalay et al. 2024).
Paper: Meteoroid Streams Sculpt the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina, A. R. Poppe, Karl Battams, D. J. McComas
Figure caption: (left) Top-down instantaneous snapshot of the dust density in the equatorial plane out to 1 au in linear (top quadrants) and logarithmic (bottom quadrants) scale. The left quadrants show the nominal, smoothly varying dust density distribution, while the right quadrants show a density profile with 50% fluctuations on spatial scales of 105 km. (right) Schematic showing the proposed mechanism for small-scale variations in the zodiacal cloud where meteoroid streams throughout the zodiacal cloud can collide and produce small-scale density depletions.
Paper: Meteoroid Streams Sculpt the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina, A. R. Poppe, Karl Battams, D. J. McComas
Figure caption: Expected variation in encountered dust density due to the location of the solar system barycenter (SSB). (a) The ratio of dust density assuming a radial distance calculated with either the SSB or the center of the Sun. (b) The difference between these two distances for PSP. (c) PSP’s perihelion qPSP in ecliptic J2000 coordinates, along with the SSB location for each perihelion time colored by orbital group.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: Correlation of gravity with gravity from topography (top left), and degree strength both for the south pole (top right) and globally (bottom). The locations of the 20 sites are marked on the polar projection; black is for the 13 Artemis sites and the south pole, while white is for the 5 PSRs and the floor.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: Comparison of free-air (FA) and gravity from topography (GT) using a crustal density of 2500 kg m−3. The figure shows the influence of the gravity from topography on the free-air gravity, and the close agreement of several profiles suggests that 2500 kg m−3 is a good approximation of the density for many sites.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: Mean clone error as a function of L, showing that the density error of the higher degrees is significantly greater than that of the lower degrees. The red data points are the mean clone value of all 20 sites; the blue data points are the mean of the six “cold” sites, and the green data points are the mean of the 13 Artemis sites and the south pole.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: Bouguer gravity for all sites using a crustal density of 2500 kg m−3. The Bouguer gravity is evaluated at the surface elevation, except for those sites with negative elevations (sites 15–20), which were evaluated at 1738 km.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: Comparison of Bouguer gravity for densities of 2000 and 3000 kg m−3 showing the effect of density of the crust on Bouguer radial gravity.
Paper: Shallow Crustal Density in the Lunar South Polar Region
Authors: Sander J. Goossens, David E. Smith, Maria T. Zuber, James W. Head
Figure caption: Topography of the south polar region showing the 20 sites that were studied.
Paper: The Adjacency Effect at Kivu Lacus
Authors: Shannon M. MacKenzie, Jason W. Barnes, William J. Miller
Figure caption: VIMS observations of Kivu Lacus: (a) orthographic projection of T85 cube C1721854264_1 atop T93 cube C1753530947_1 for context (generated with the pyvims package; B. Seignovert et al. 2023); (b) the eight surface windows of the T85 cube analyzed in this work; (c) examples of transects through the shorelines and the logistic fit; and (d)–(e) comparison of the fit parameters σ and a from the VIMS data to SRTC++ output. The SRTC++ results shown here are a subset of Figure 3, including only the southeastern shore of Kivu captured in T85, and thus are more uniform. Each degree of latitude on Titan spans 45 km.
Paper: The Adjacency Effect at Kivu Lacus
Authors: Shannon M. MacKenzie, Jason W. Barnes, William J. Miller
Figure caption: Examples of SRTC++ modeled observations of Kivu Lacus at 5 μm (top; low atmospheric opacity, τ), 2 μm (middle; τ ∼ 1), and 1.3 μm (bottom; high τ). Radial I/F transects (left column; dots) are drawn from a line through the pixel indicated in the simulated image (right column) to the center of the lake; only a subset of the shoreline transects, chosen to span the area imaged in T85, is shown here. Logistic fits are shown as lines with fit parameters σ (extent of the adjacency effect) and a (amplitude of the contrast) given in the legend. Kivu Lacus is 100 km wide from left to right in this unprojected synthetic image.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Average angles α (filled red circles) and β (open blue circles) as defined in Figure 2 and temperature (black squares) over time for the experiments shown in Figures 4 and 5, wet sample. The pressure is 3.4 mbar (top) and 10 mbar (bottom). Left axis: angles. Right axis: temperature. The dashed black line indicates the time when the light is switched off. For visibility, and since the data refer to single piles, variations in slope at a given time and systematic errors are not shown.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: RSL site (latitude −41﹩\mathop{.}\limits^{\unicode{x000b0}}﹩98, longitude 202﹩\mathop{.}\limits^{\unicode{x000b0}}﹩29, Ls 341°, MY 28; A. S. McEwen et al. 2011). Surface temperature (solid line) and pressure (dotted line) (F. Forget et al. 1999, 2025; J.-B. Madeleine et al. 2011; E. Millour et al. 2018, 2022).
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Ratio α/α0 over pressure at 4670 ± 690 W m−2 for the wet sample (top) and the dry sample (middle) and at 1850 ± 230 W m−2 (bottom). The bottom figure contains data for both the dry and the wet samples. Dashed blue line: a ratio of 1, which implies no changes. Red squares: before the light is switched off. Black triangles: after the light is switched off. Overplotted are lognormal functions fitted to the data.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Pressure dependence of the duration of the erosion to reach the final equilibrium angle while the light is on at 4670 W m−2 (squares) and 1850 W m−2 (triangles) light intensity. Open symbols: wet sample. Filled symbols: dry sample. Only the measurements where the slope erosion is observed are shown.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Slope angle α (illuminated side) at 4670 ± 690 W m−2 (top) and 1850 ± 230 W m−2 (bottom) over pressure. Blue circles: initial angle α0. Blue lines: mean initial angle for the wet sample (dashed) and the dry sample (solid). Red squares: the angle right before the light is switched off. Black triangles: the angle after the light is switched off. Filled symbols represent the dry sample, while open symbols represent the wet sample. For better visibility, the error bars are not displayed, and the black symbols are slightly shifted to the right. The variation of a single data point ranges between 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 and 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Estimate for the temperature inside the soil for the RSL site (latitude −41﹩\mathop{.}\limits^{\unicode{x000b0}}﹩98, longitude 202﹩\mathop{.}\limits^{\unicode{x000b0}}﹩29, Ls 341°, MY 28) on a crater slope (A. S. McEwen et al. 2011), 14 hr local time.
Paper: A Decrease in Slope Angles on Insolated Martian Slopes: Ground-based Experiments
Authors: Tetyana Bila, Gerhard Wurm
Figure caption: Particle size distribution of the JSC Mars 1a sample used.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Linearly mixed model (dashed), intimately mixed model (dotted), and laboratory (solid) spectra for 50%/50% volume mixtures of different grain sizes of water ice and epsomite. Differences between laboratory and modeled spectra are provided in the “Difference” plots below each corresponding spectrum. Similar to the pure epsomite spectra, the modeled data do not exhibit as fine structure in the absorption features that are expected, and observed, in the laboratory data. Differences generally remain within ∼15%.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Model (dashed) and laboratory (solid) spectra for individual grain sizes of epsomite are generally well matched, though not as well matched as the spectra for water ice. Dashed line appears solid shortward of 1.4 μm due to noise. Model grain sizes are two-thirds of the aliquot average, <D>. Differences between laboratory and modeled spectra are provided in the “Difference” plots below each corresponding spectrum, and generally remain within ∼10%.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Model (dashed) and laboratory (solid) spectra for individual grain sizes of water ice are generally well matched. Dashed line appears solid shortward of 1.4 μm due to noise. Model grain sizes are two-thirds of the aliquot average, <D>. Differences between laboratory and modeled spectra are provided in the “Difference” plots below each corresponding spectrum, and generally remain within ∼10%.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Linearly mixed model (dashed), intimately mixed model (dotted), and laboratory (solid) spectra for 50%/50% volume mixtures of different grain sizes of water ice. Differences between laboratory and modeled spectra are provided in the “Difference” plots below each corresponding spectrum, and generally remain within ∼10%.
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: Images of the Hamburg meteorite reprocessed using ImageJ to threshold olivine (left) and pyroxene (right) so as to estimate their abundances. The saturated red color in all images is olivine, while the darker red is pyroxene. (Top) Close-up of a chondrule map from P. R. Heck et al. (2020; their Figure 7, upper left image). (Middle) Slice of the Hamburg type sample ME6108.3 from P. R. Heck et al. (2020; resampled from their Figure 5(b)). (Bottom) A second slice through the type sample ME6108.3, resampled from P. R. Heck et al. (2020; their Figure 10, bottom).
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: Results of matching the Michigan H4 meteorite spectra to the meteorite and asteroid spectral libraries collected by M. D. Dyar et al. (2023).
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: Mössbauer spectra of the fusion crust (top) and interior (bottom) of the Hamburg (Michigan H4) meteorite. Sextets are assigned to Fe in metal (purple) and Fe carbide (orange). Doublets correspond to Fe3+ in pyroxene (blue) and Fe2+ in olivine + pyroxene (green) and pyroxene (brown).
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: Normalized Raman spectra of the interior (orange) and crust (blue) of the Hamburg meteorite.
Paper: Contrast Reversal and Emergent Features on Pluto
Authors: Jason D. Hofgartner, Bonnie J. Buratti, Will M. Grundy, S. Alan Stern, Anne J. Verbiscer
Figure caption: Cloud or surface coating hypothesis for Pluto’s CRs. S CR, NW CR, and NE CR correspond to the southernmost, northwesternmost, and northeasternmost example CRs, respectively, in Figures 1 and 4. SP1 corresponds to a Sputnik Planitia locality between the three example CRs. The 95% statistical confidence intervals are generally smaller than the filled circles, and the two P_LORRI (19° solar phase angle) measurements of each locality are indistinguishable. The Hapke+haze photometric function is shown using SP1 best-fit parameters and average incidence and azimuth angles (both angles are approximately constant; Table 1). Hapke+cloud+haze photometric functions are shown using best-fit SP1 surface/shallow subsurface and global haze and S CR, NW CR, or NE CR cloud parameters and average incidence and azimuth angles. Best-fit parameters for each locality, however, were determined using angles specific to each measurement, and residuals are generally smaller than they appear. Optically thin scattering between the surface and global haze, by a cloud or surface coating, satisfactorily fits differences of example CRs on Pluto from their surroundings.