adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Comparisons of the parameter values defining each of the K-means clusters for each of the three study areas. There is significant overlap in parameter values, but the graphs display a grading of clusters into each other from unit A (red) to unit B (black/gray) to unit C (blue) to unit D (green).
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: (Left) Images of each study area (top to bottom: area I, area II, and area III) with a red square (highlighted by a red arrow) denoting the region used for calculating the standard reflectance. (right). Histograms of area I (top), area II (center), and area III (bottom) showing the percent differences between the normalized reflectance from the actual image and the normalized reflectance from the model images, summed over all images used to model the reflectance behavior in each area. The histograms show the fraction of pixels from the total in each percent difference category. Histograms for the individual images are shown in the supplementary materials (Figures A13–A15).
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Schematic of the initial formation of halos through the popcorning of grains and the subsequent evolution and development of hollows. The sublimation of the volatile portion of intermixed grains removes regolith particles along ballistic trajectories (orange lines) to form deposits categorized as halos. As material is removed, depressions are formed and with time grow to become hollow features, making halo formation the initial stage of hollow development, a precursor to the “Stage 1” hollow development (e.g., A. N. Deutsch et al. 2025). This scenario depicts halo and hollow formation within the peak ring, which also experiences mass wasting due to glacier-like flows described by J. A. P. Rodriguez et al. (2023). The peak ring is uplifted material that forms a distinct surface feature.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Comparisons of the parameter values defining each of the MLC clusters (basin floor, flow, hollows, and halos) for each of the three study areas (area I shown in circles, area II top shown in squares, area II bottom shown in diamonds, and area III shown in triangles). There is significant overlap in the parameter values, with some MLC clusters displaying linear trends between some parameters.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: The K-means cluster unit maps for areas I (top), II (center), and III (bottom) using the four-cluster solutions. The first column shows gray-scale reflectance images of each area, the central column shows the K-means cluster unit maps with morphologic boundaries shown in white, and the right column is a transparent overlay of the K-means cluster unit maps on top of the reflectance images. For the central and right columns: red = cluster A, black = cluster B, blue = cluster C, green = cluster D. Refer to Table 2 for details on the parameter value ranges for each cluster unit.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Hapke’s “hockey-stick” relationship (B. Hapke 2012b) between the scattering function amplitude (b) and the scattering function partition (c) parameters from the four MLC units from each study area compared to other Mercury studies and the laboratory measurements of A. McGuire & B. Hapke (1995) and the remodeling of those measurements by B. Hartman & D. Domingue (1998). Note that the “c values” have been converted to match the formalism in B. Hapke (2012b) due to the different formulation of the single-particle scattering function, as discussed in Section 4. This diagram has been converted to match that in B. Hapke (2012b).
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Example images from area II. Top left is NAC image N1025853427M. The top center image is a synthetic image of the image on the left based on the Hapke model parameters shown in Figure A7. The top right is a ratio of the observed image (left) to the model image (center). Bottom left is WAC image W0231179208G. The bottom center image is a synthetic image of the image on the left based on the Hapke model parameters shown in Figure A7. The bottom right is a ratio of the observed image (left) to the model image (center). The observed and synthetic images in the top row are displayed on a gray scale of 0–0.08, and those on the bottom row are displayed on a gray scale of 0–0.09. Both ratio images are displayed on a gray scale of 0–2.5. The black areas in the ratio image are regions in shadow in the observed image based on the SPC shape model.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Histograms of area I (top), area II (center), and area III (bottom) showing the percent differences summed over all images used to model the reflectance behavior in each area in terms of the fraction of pixels from the total in each percent difference category. Histograms for the individual images are shown in the supplementary materials (Figures A10–A12).
Paper: Parameter Space Exploration of Low-to-moderate-temperature Hydrothermal Systems on Ocean Worlds Using a Monte Carlo Framework
Authors: Ryunosuke Akiba, Andrew T. Fisher
Figure caption: Diagrams illustrating the conceptual and theoretical basis for coupled fluid-heat calculations shown in this study, as may apply to an ocean world (variables discussed in text and defined in Table A1). (a) The cartoon shows a two-dimensional slice through a three-dimensional flow system, with depth profile oriented parallel to net fluid transport within a hydrothermal siphon and fluid entering and exiting the seafloor through permeable channels (presented here as “outcrops” but could be fractures or other heterogeneities in properties). A porous and saturated aquifer below the seafloor is heated from below, with buoyant fluid consequently discharging through one outcrop and recharging through another. Cartoon adapted from A. Fisher & R. Harris (2010). (b) Examples of thermal profiles at the discharge side of the siphon comparing conductive conditions (no flow; green dashed line) with rapid isothermal upflow (solid red line) and slower, less rapid upflow (orange dashed curve) during which fluid partly cools during ascent. Similar profiles occur at the recharge site but with maximum curvature at the base. (c) Top-down perspective view of flow between recharging and discharging sites (blue and red, respectively), forming a geothermal dipole that functions as a heat exchanger between the fluid and silicate solid body.
Paper: Parameter Space Exploration of Low-to-moderate-temperature Hydrothermal Systems on Ocean Worlds Using a Monte Carlo Framework
Authors: Ryunosuke Akiba, Andrew T. Fisher
Figure caption: Comparison of analytical calculations (this study) and numerical results (A. Fisher et al. 2024; triangles) for d = 600 m and zaq = 1.05 km, with a background heat flux of qB = 98 mW m−2. Combinations of F and kaq that produce a siphon are plotted for gravity as appropriate for (a) Earth, (b) Europa, and (c) Enceladus. Each panel on the left comprises results from testing ≈104 parameter sets. The region of excess pressures between 50% and 90% of driving pressures is shaded cyan and used in this study as an additional criterion for siphon sustainability. (d) Discharge temperature, TD; (e) advective heat output, Qadv; and (f) driving pressure, ΔP, for varied F and kaq under Earth gravity are plotted against F. Aquifer permeability is colored for points lying in the cyan region of (a). Numerical simulations that failed to sustain a siphon are indicated by an open symbol.
Paper: Parameter Space Exploration of Low-to-moderate-temperature Hydrothermal Systems on Ocean Worlds Using a Monte Carlo Framework
Authors: Ryunosuke Akiba, Andrew T. Fisher
Figure caption: Selected regions of sustained siphons and properties for Europa models (parameters as listed in Table 1). Trends in discharge temperature TD with (a) aquifer permeability kaq, (b) depth to aquifer zaq, and (c) flow rate F. Dependence of flow rate F with (e) kaq, (f) zaq, (g) outcrop separation DRD, and (h) recharge outcrop surface area. The subset of siphons with power output greater than that of the characteristic flow region between outcrops (APR) is colored magenta (highlighted in panel (d), discussed in text).
Paper: Parameter Space Exploration of Low-to-moderate-temperature Hydrothermal Systems on Ocean Worlds Using a Monte Carlo Framework
Authors: Ryunosuke Akiba, Andrew T. Fisher
Figure caption: Comparison of hydrothermal siphons sustained at low heat flux qB = 10 mW m−2 for different gravity values: 2 × Earth (gSE), Earth (gEa), Europa (gEu), and Enceladus (gEn). Successful model runs are plotted as a bounding region for each gravity value, representing the extent of many individual model runs. The largest space is covered by high gravity, and there is considerable overlap between results with different gravity values.
Paper: Parameter Space Exploration of Low-to-moderate-temperature Hydrothermal Systems on Ocean Worlds Using a Monte Carlo Framework
Authors: Ryunosuke Akiba, Andrew T. Fisher
Figure caption: Comparison of MC analytical and numerical results (this study and A. Fisher et al. 2024, respectively). Each panel shows results from ≈104 simulations for which a siphon was sustained, with the cyan band showing calculations for which Psiph is ≥50% and ≤90% of ΔP (Equation (11). Results and comparison to A. Fisher et al. (2024, Table 3) are shown for three gravities for a selection of geometries and basal heat fluxes: (a) “deep-thin” (zaq = 1050 m, aquifer thickness 600 m) at 49 mW m−2, (b) “shallow-thin” (zaq = 450 m, aquifer thickness 600 m) at 196 mW m−2, and (c) “shallow-thick” (zaq = 450 m, aquifer thickness 600 m) at 196 mW m−2.
Paper: Parameter Space Exploration of Low-to-moderate-temperature Hydrothermal Systems on Ocean Worlds Using a Monte Carlo Framework
Authors: Ryunosuke Akiba, Andrew T. Fisher
Figure caption: Selected panels (a), (b), and (c) from Figures 4(a), (b), and (e), respectively, colored to identify temperatures TD = 80°C–120°C and W/R Gy–1 < 100 (orange), as highlighted in panel (d).
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Cumulative and probability density functions for the perihelion (top left), cosine of inclination (top right), and velocity at infinity (bottom) for ISOs discovered in LSST. Comparisons are made to the observed ISO sample (colored dashed curves) for perihelion and the Ōtautahi–Oxford model (black dashed curve) for inclination and velocity. Vertical dotted black lines indicate the corresponding values for the two known ISOs.
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Same as Figure 8, but for discovery date relative to the start of the survey (left) and to the time of perihelion passage (right). The dashed lines indicate a uniform discovery rate (left), the time of perihelion passage (right; vertical line), and the 50% cumulative density (right; horizontal line).
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Same as Figure 8, but for the properties of ISOs at the time of their discovery in the main survey of LSST. Top left to bottom right: heliocentric distance, on-sky velocity, geocentric distance, and apparent r-band magnitude mr. Vertical dotted black lines indicate the corresponding values for the two known ISOs at the time of their discovery; note that 1I/‘Oumuamua was discovered by NEO discovery survey Pan-STARRS, while 2I/Borisov was discovered at low solar elongation and was cometary.
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Probability density functions for the Galactic velocity distributions of the LSST discovered ISOs from the qs = 2.8 intrinsic absolute magnitude distribution. The gray scale is normalized such that the sum of all (U, V) or (V, W) cell of probability density is equal to 1; the darkest cells are the most probable. The yellow square denotes the local standard of rest. The structures predicted by M. J. Hopkins et al. (2025) are still apparent in the velocity distribution the discovered ISOs will be drawn from, including the overdensity at the Sun’s velocity ﹩\left(U,V,W\right)=\left(0,0,0\right)﹩ due to gravitational focusing; this is less discernible in (V, W) than (U, V) due to being washed out in the distribution marginalized over U.
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Two-dimensional illustrations for the on-sky locations (α, δ) for the first, discovery, and last images of the LSST discoveries with 13 ≤ H ≤ 14 for qs = 2.8 for all years (top row), odd rolling years (middle row), and even rolling years (bottom row). This excludes ISOs discovered in Year 2 of the simulation, which only deploys a rolling cadence over half of the survey footprint. R.A. α increases to the right in each projection, from –180° to 180°. The white star indicates the solar apex, and the thin white line indicates the Galactic plane. The last column shows the set of observations (first, discovery, last) for 10 randomly selected discovered ISOs. The observations are connected by straight lines of random color, which may appear curved due to the spherical projection, and the last observation is marked by a white dot to indicate the ultimate direction of motion.
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Two-dimensional illustrations for the on-sky locations (α, δ) for the first, discovery, and last images of the LSST discoveries for qs = 2.8 for all years of the survey. R.A. α increases to the right in each projection, from −180° to 180°. The white star indicates the solar apex, and the thin white line indicates the Galactic plane. Other absolute magnitude slopes also show similar trends.
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Comparison of the difference in slope qs of the two compared model Hr distributions to the number of discoveries required to reject models. The blue horizontal dashed lines indicate sample sizes of 5, 10, 50, and 100 ISOs. Fewer discovered ISOs are needed to distinguish between slope values that are further apart. The size of each data point is proportional to the product of the compared slope values: for the same Δqs, steeper slopes require more discoveries in order to be distinguished.
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Same as Figure 8, but for argument of perihelion (left) and R.A. of the ascending node (right). The dashed black curves indicate the cumulative and probability density functions for the intrinsic model (the Ōtautahi–Oxford population).
Paper: The Visibility of the Ōtautahi–Oxford Interstellar Object Population Model in LSST
Authors: Rosemary C. Dorsey, Matthew J. Hopkins, Michele T. Bannister, Samantha M. Lawler, Chris Lintott, Alex H. Parker, John C. Forbes
Figure caption: Same as Figure 8, but for discovery date relative to first detection. The dashed gray vertical lines indicate 380 and 745 days, respectively, corresponding to integer years plus 15 days.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Simulated topography of a 100 km diameter crater comparing the importance of the strengths and thermal properties of ice and clathrate. Here, the mechanical properties of ice (not clathrate) are used in all cases, and we vary the thermal profiles. First, we compare the relaxation of craters in an ice shell with (a) a very warm 5 km clathrate crust thermal profile and (b) a warm 20 km clathrate crust thermal profile, with (c) minimal relaxation in a significantly colder pure water-ice shell (thermal profiles from K. Kalousová & C. Sotin 2020). Line colors correspond to times 0, 10 million yr, and 1 billion yr.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: SARTopo profile of Hano crater vs. simulated topography of a 100 km diameter central pit crater (teal lines) and a flat-floored crater (black lines) in (a) 5 and (b) 10 km methane clathrate crusts. Dashed lines show simulated elevations; solid lines show simulated elevations after being subjected to the “artificial averaging” effect of SARTopo measurements. Error bars on the SARTopo profile represent the along-track resolution and estimated random error in height.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Stereo profiles of (a) Ksa, Ihi, and (b) Soi plotted with the final shape (1 billion yr) of simulated craters using the thermal properties of an ice shell with a 5 km clathrate crust and (1) the mechanical properties of ice and clathrate (solid lines) and (2) the mechanical properties of a pure ice shell (dashed lines). Profiles correspond to the lines crossing the craters in the stereo images (Figure 4).
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: SARTopo profile of Selk crater vs. simulated topography of an 85 km diameter central pit crater (teal lines) and a flat-floored crater (black lines) in (a) 5 and (b) 10 km thick methane clathrate crusts. Dashed lines show simulated elevations; solid lines show simulated elevations after being subjected to the “artificial averaging” effect of SARTopo measurements. Error bars on the SARTopo profile represent the along-track resolution and estimated random error in height.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Evolution of the 40 km diameter central peak crater (a) and an 85 km diameter central pit crater in an ice shell with a 5 km thick clathrate crust (b) with three different initial pit-rim widths (Dpr): (teal) a 60 km diameter pit-rim, (pink) a 40 km diameter pit-rim, and (black) no pit-rim.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Left: comparison of Himalia’s continuum-divided 3.0 μm band complex to laboratory samples of ammoniated Illite from S. De Angelis et al. (2021). Note that absorption band depths are rescaled to approximate Himalia’s 2.7 μm feature, as pure laboratory samples have very large band depths. Right: Himalia’s 3.0 μm band complex is well matched by a combination of the phyllosilicate band found in aqueously altered C2-chondrite Essebi and the absorption band on 67P’s nucleus, attributed to ammonium-bearing salts. These materials do not form in the same geological settings, but they demonstrate that relatively simple mixtures of phyllosilicates with NH4-bearing materials can provide a close spectral match to Himalia. The deep feature near 3.4 μm on Essebi is caused by aliphatic organics that are not present on Himalia and is unrelated to phyllosilicate composition.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Comparisons of 3 μm band complexes between irregular satellites Themisto, Sinope, and Carme to the Jovian Trojans Leucus and Patroclus. Band depths for all objects were normalized at 3.0 μm to aid comparisons of the relative strengths and shapes of the 3.0 and 3.4 μm bands for each object. Themisto, Sinope, and Leucus all belong to the “red” color taxon and display similar 3.0 and 3.4 μm absorption features. Carme’s band properties are intermediate between “red” and “less red” groups, with a deeper 3 μm feature that compares closer in shape and band center to the “less red” Trojan Patroclus, but a deeper 3.4 μm feature from aliphatic organics that compares closer to the “red” objects. Trojan spectra are reprocessed for methodological consistency and were originally reported and analyzed in I. Wong et al. (2024).
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: The 3.0 μm band shapes for irregular satellites Lysithea and Ananke, meteorites Murchison and DOM 10085, and Jupiter Trojans Eurybates and Polymele. Objects are sorted according to the central wavelength (λc) of their features, which is marked by a square on each curve. Ananke’s feature is positioned in between known petrologic type 2 meteorites that have experienced aqueous alteration. Lysithea is centered intermediate between Eurybates and Ananke. For ease of band shape comparisons, all bands are rescaled to the same arbitrary depth.