adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Spectroscopy of a Blue Binary Cold Classical Kuiper Belt Object
Authors: Ian Wong, Bryan J. Holler, Wesley C. Fraser, Michael E. Brown
Figure caption: Comparison plot of spectra of the solar analog star SNAP-2 obtained from two JWST observations that utilized different dither patterns (blue and red curves). The CALSPEC model spectrum of SNAP-2 is overplotted in the solid black line. The difference between the two JWST spectra of SNAP-2 at short wavelengths is attributed to variations in sensitivity across the NIRSpec IFU detector that are not corrected by the current calibration pipeline. The solar standard spectrum from the PSG is also included (black dashed line), which shows a discrepant spectral slope at short wavelengths from the SNAP-2 model spectrum. All spectra have been renormalized to match the blue curve at 2.0 μm.
Paper: JWST Spectroscopy of a Blue Binary Cold Classical Kuiper Belt Object
Authors: Ian Wong, Bryan J. Holler, Wesley C. Fraser, Michael E. Brown
Figure caption: Median-averaged IFU image slices from the first dithered exposures of 2001 XR254 and 2016 BP81. A logarithmic stretch has been applied to the flux scaling to accentuate the PSF shapes and background variations. The black points and circles indicate the measured source centroid positions and spectral extraction apertures. The primary and secondary components of 2016 BP81 are well separated and labeled.
Paper: The Case for Continuing VIPER: A Critical Milestone on the Journey Back to the Moon
Authors: Benjamin Fernando, Clive Neal, Jack Kiraly, Brianna Fernandez, Ruby Patterson, Szilárd Gyalay, Myriam Lemelin
Figure caption: The VIPER landing site and mission area intersect two current Artemis III potential landing regions: “Mons Mouton” and “Mons Mouton Plateau.” The VIPER primary and extended mission areas (red rectangles), the VIPER landing site (black circle), as well as potential hematite (red) and water ice (white) detections by S. Li et al. (2018, 2020), are shown. The Mons Mouton Plateau sits nearly 6 km above the mean lunar radius in one the most well-illuminated south polar regions. The landing site of the failed Intuitive Machines second lander (IM-2) is also shown. The background map is from the Lunar Orbiter Laser Altimeter at a resolution of 80 m pixel−1.
Paper: The Case for Continuing VIPER: A Critical Milestone on the Journey Back to the Moon
Authors: Benjamin Fernando, Clive Neal, Jack Kiraly, Brianna Fernandez, Ruby Patterson, Szilárd Gyalay, Myriam Lemelin
Figure caption: Left: Schematic illustrating the operational modes of VIPER. The two modes of operation are prospecting (which includes waypoint operations) and drilling. Inset panels: depiction of the Nav cams (photo credit: NASA/Johnson Spaceflight Center/David DeHoyos) and the NSS instrument (photo credit: NASA/Dominic Hart). Top right: VIPER when nearly complete in May 2024, shown in the “stowed” position (wheels up and covers on; photo credit: NASA/Helen Arase Vargas). Bottom right: the instruments TRIDENT (photo credit: NASA/Honeybee), MSOLO (photo credit: NASA/Kim Shiflett), and NIRVSS (photo credit: NASA/Dominic Hart), which are stowed within the body of the rover. The instruments and their roles are defined in Section 2.1.
Paper: The Case for Continuing VIPER: A Critical Milestone on the Journey Back to the Moon
Authors: Benjamin Fernando, Clive Neal, Jack Kiraly, Brianna Fernandez, Ruby Patterson, Szilárd Gyalay, Myriam Lemelin
Figure caption: Institutions represented on the VIPER team, in the United States, Canada, and Switzerland. Ten states and five NASA centers are directly represented.
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 corresponding viscosity (panels (e)–(h)) and temperature (panels (i)–(l)) field for a case where the Theia fragment is 100 times more viscous than in 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: Snapshots of compositional (panels (a)–(d)) and corresponding viscosity (panels (e)–(h)) field for a model with Theia fragments having 100 times weaker viscosity 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: Snapshots of compositional (panels (a)–(d)) and corresponding viscosity (panels (e)–(h)) field for a case of lower initial temperature (T = 0.52) 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: Snapshots of compositional field in the reference case showing that asteroid-sized Theia fragments can survive as LLVP-like structures after 4.5 Gyr.
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: Temperature snapshots in the reference case showing that asteroid-sized Theia fragments can survive as LLVP-like structures after 4.5 Gyr.
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: Influence of model parameters on LLVP formation time from Theia mantle fragments. Compared to the reference case, the bins on the right represent models with modified parameters, including a buoyancy number twice as high, a buoyancy number half as large, Theia fragments that are 100 times stronger or 100 times weaker, a higher activation energy (A = 10.51), higher (T = 0.8) and lower (T = 0.52) initial mantle temperatures, and a slightly reduced Rayleigh number (Ra = 7 × 107), as described above.
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 viscosity field in the reference case showing that asteroid-sized Theia fragments can survive as LLVP-like structures after 4.5 Gyr.
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: Incremental size distribution of Theia fragments used in geodynamic simulations. The size distribution follows the incremental main-belt SFD after W. Bottkejr et al. (2005).
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 a half-dense Theia case (B = 0.5) compared to the reference case.
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: DIP as a function of host-rock CaO content. Host-rock CaO is increased by shifting plagioclase feldspar from albite to anorthite. Blue to red lines represent increasing initial porewater [Ca2+]; the reference value is [Ca2+] = 1 × 10−12 mol kg−1 (darkest-blue line). Note the linear steps in [Ca2+] between 1 × 10−2 mol kg–1 and 1 × 10−1 mol kg−1. Vertical dashed lines for Earth MORB are ±2σ wt% CaO for MAR basalt from PetDB (https://search.earthchem.org/).
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: Precipitate and carbonate system plots to explain trends in Figure 3. (a) Precipitated fluorapatite, Ca5(PO4)3F, vs. host-rock CaO; (b) precipitated calcite, CaCO3, vs. host-rock CaO; (c) DIP vs. porewater pH; (d) DIP vs. porewater carbonate alkalinity. Blue to red lines represent increasing initial porewater [Ca2+] (reference value is [Ca2+] = 1 × 10−12 mol kg−1; darkest-blue line). Note the linear step changes in [Ca2+] between 1 × 10−2 mol kg–1 and 1 × 10−1 mol kg−1.
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: Conceptual model of seafloor weathering reactions via an aqueous geochemical thermodynamic equilibrium model. Step 1 depicts unreacted host rock and porewater, whose compositions are varied in the sensitivity tests listed in Table 2. During reaction, dissolution of the primary minerals and precipitation of secondary minerals occur, altering porewater chemistry (step 2). Step 3 represents the system at equilibrium, where the final porewater concentrations and amount/type of authigenic minerals are reported as results. Figure created with BioRender (https://BioRender.com).
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: Comparison of (a) a simplified cartoon of the modern Earth marine P cycle with (b) a conceptual model of a possible pelagic planet P cycle. Due to anoxic conditions in the ocean and the absence of subaerial continents, the P cycle of a pelagic planet must differ from that of Earth. Figure created with BioRender (https://BioRender.com).
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: Histograms of calculated exocrust Ca-to-P ratios for hypothetical nearby (<200 pc) HZ terrestrial planets (derived from R. J. Spaargaren et al. 2023; see Section 4.3). Endmember crustal Ca enrichment factors (﹩f﹩) and Ca/P thresholds (﹩\alpha ﹩) are shown: (a) ﹩{f}_{\min }﹩ with minimum, maximum, and Earth ﹩\alpha ﹩; (b) ﹩{f}_{\max }﹩ with minimum, maximum, and Earth ﹩\alpha ﹩. The area to the left of a given ﹩\alpha ﹩ under the histogram represents the number of stars that could host DIP-rich pelagic planets. As an example, the gray shaded region corresponds to the number of stars for ﹩{f}_{\max }\,﹩ and ﹩{\alpha }_{\min }﹩ (∼4% of total population). The highest number of stars, ∼63% of the population, corresponds to ﹩{f}_{\min }﹩ and ﹩{\alpha }_{\max }.﹩
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: DIP as a function of host-rock CaO for different authigenic mineral scenarios. (a) Dolomite precipitation instead of calcite (see top of panel (b)). (b) Top of panel has calcite precipitation turned on (same data as Figure 3); gray shaded region has calcite precipitation (and all other Ca/Mg-bearing carbonates) turned off. Blue to red lines are increasing initial porewater [Ca2+] (reference value is [Ca2+] = 1 × 10−12 mol kg−1).
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: DIP as a function of host-rock CaO for various porewater compositions. (a) Porewater Al3+ sensitivity test (reference value is [Al3+] = 1 × 10−12 mol kg−1); (b) porewater SiO2 sensitivity test (reference value is [SiO2] = 1 × 10−12 mol kg−1); (c) porewater F− sensitivity test (reference value is [F−] = 7 × 10−5 mol kg−1). Note that the activity of F− is held constant for each experiment. For each panel, blue to red lines are increasing initial porewater [Al3+], [SiO2], and [F−], respectively.
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: DIP as a function of host-rock CaO for various physical parameters. (a) Same sensitivity test as in Figure 3, but at low pressure (1 bar) instead of high pressure (1000 bars). Blue to red lines are increasing porewater [Ca2+] (reference value is [Ca2+] = 1 × 10−12 mol kg−1). (b) Temperature sensitivity test. Blue to red lines are increasing ﹩T﹩ (reference value is ﹩T﹩ = 25 °C). (c) Water–rock mass ratio sensitivity test. Blue to red lines are increasing ﹩w/r﹩ (reference value is ﹩w/r﹩ = 10).
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: DIP as a function of two host-rock solid solutions. (a) DIP vs. host-rock CaO (albite-anorthite solid solution) with varying initial porewater [Fe2+]; (b) DIP vs. host-rock FeO (forsterite-fayalite solid solution) with varying initial porewater [Fe2+]; (c) DIP vs. host-rock FeO (forsterite-fayalite solid solution) with varying initial porewater [Mg2+]. Blue to red lines are increasing initial porewater [Fe2+] and [Mg2+] (reference values are [Fe2+] = 1 × 10−12 mol kg−1 and [Mg2+] = 1 × 10−12 mol kg−1).
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: DIP as a function of porewater pH. Increasing [CO2(aq)] (blue to red lines; reference value is [CO2(aq)] = 1 × 10−4 mol kg−1) decreases pH. The upper right and lower left triangles on each line are the albite and anorthite endmembers, respectively. Note that the activity of CO2(aq) is fixed (i.e., held constant) for each model run.
Paper: Lithological Controls on Aqueous Phosphorus on Ocean-covered Exoplanets
Authors: Adam T. Stone, Bradford J. Foley, Benjamin M. Tutolo, Kimberly V. Lau
Figure caption: Magnesium sensitivity test along the albite-anorthite solid solution. (a) DIP vs. host-rock CaO; (b) equilibrium porewater Ca2+ vs. Mg2+ concentrations are positively correlated, except when clinochlore precipitation occurs at high [Mg2+] (triangles); (c) precipitated calcite, CaCO3, vs. host-rock CaO. Blue to red lines represent increasing initial porewater [Mg2+] (reference value is [Mg2+] = 1 × 10−12 mol kg−1).
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: A slice in the X–Z plane of the simulated water molecule gas torus with a gas production rate of 1 × 1028 H2O s−1. Enceladus is located at X ∼ 3.95 RS. Panels illustrate the torus distribution at (a) detailed-scale, (b) intermediate-scale, and (c) large-scale near Enceladus. The dashed rectangle in (b) marks the region magnified in (a), while the dashed rectangle in (c) marks the region magnified in (b).
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Lifetimes of H2O molecules at the equator as a function of distance from Saturn. The blue line shows the lifetime due to neutral/ion reactions, the red line shows the lifetime due to electron impact dissociation and ionization, and the green line shows the lifetime due to photodissociation and ionization.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Column density distributions of neutral gas torus for (a) H2O, (b) OH, and (c) O, viewed along the Y-axis.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Neutral gas torii of (a) H2O, (b) OH, and (c) O number density distribution in the X–Y plane.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Average number density of neutral gas species (H2O, OH, and O) on the ring plane. Solid lines represent model results (H2O: blue, OH: red, and O: green), while dashed lines represent observational data (OH from HST and O from Cassini UVIS) by H. Melin et al. (2009).
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Impact flux distributions of water-group molecules onto Saturn’s main rings for (a) H2O, (b) OH, and (c) O. The regions of the A, B, and C rings are also marked in each panel.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Charge-exchange rates (ν) at the equator as a function of relative velocity (ur) for different L-shell values ranging from 2 to 10. The left panel shows charge-exchange rates for water-group neutrals interacting with water-group ions, while the right panel shows interactions with H+ ions.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Neutral gas torus of (a) H2O, (b) OH, and (c) O number density distribution in the Y–Z plane.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: The plasma environment around Saturn between 2.4 and 10 of L-shell from A. M. Persoon et al. (2020), including (a) electron density, (b) water-group ion density, and (c) hydrogen ion density.
Paper: Water Transport from Enceladus to the Rings
Authors: Ian-Lin Lai, Hua-Shan Shih, Wei-Ling Tseng, Wing-Huen Ip, Jong-Shinn Wu
Figure caption: Latitudinal distribution of the mean impact flux of H2O, OH, and O onto Saturn’s atmosphere.
Paper: JWST Spectroscopy of a Blue Binary Cold Classical Kuiper Belt Object
Authors: Ian Wong, Bryan J. Holler, Wesley C. Fraser, Michael E. Brown
Figure caption: Spectral comparison plot of 2001 XR254 and 2016 BP81 with the KBOs presented in N. Pinilla-Alonso et al. (2025). The latter are divided into panels based on their compositional class. All spectra are normalized to unity at 2.5 μm. The spectrum of 2016 BP81, shown in the black curve in each panel, has the greatest affinity to the H2O-type KBOs. Meanwhile, 2001 XR254 (purple line in the bottom panel) has a surface composition that is consistent with organics-type objects.
Paper: JWST Spectroscopy of a Blue Binary Cold Classical Kuiper Belt Object
Authors: Ian Wong, Bryan J. Holler, Wesley C. Fraser, Michael E. Brown
Figure caption: The reflectance spectra of the blue binary 2016 BP81 (black), Neptune Trojan 2011 HO277 (green), and the ETNO 2016 QV89 (purple), normalized to unity at 2.5 μm. All three objects show similar spectral shapes, including weak 2 μm H2O-ice absorption features, deep 3 μm H2O-ice bands without Fresnel peaks, and strong primary CO2-ice bands at 4.27 μm. 2011 HO277 shows an additional distinct absorption band at 3.3–3.6 μm due to aliphatic organics.
Paper: JWST Spectroscopy of a Blue Binary Cold Classical Kuiper Belt Object
Authors: Ian Wong, Bryan J. Holler, Wesley C. Fraser, Michael E. Brown
Figure caption: Grid plot of two-parameter distributions for the measured 2 H2O, 3 H2O, and 4.27 μm CO2 absorption bands among objects in the H2O-type KBO compositional class. Different colors and shapes denote the corresponding dynamical classes of the objects. Dashed black lines connect the blue binary 2016 BP81 with the Neptune Trojan 2011 HO277 and the ETNO 2016 QV89. The three objects’ spectra show comparable spectral properties, which appear to differ systematically from the rest of the H2O-type KBOs in the sample.
Paper: JWST Spectroscopy of a Blue Binary Cold Classical Kuiper Belt Object
Authors: Ian Wong, Bryan J. Holler, Wesley C. Fraser, Michael E. Brown
Figure caption: Reflectance spectra of 2001 XR254 and 2016 BP81, normalized to unity at 2.5 μm and offset for clarity. The individually extracted spectra of the primary and secondary components of 2016 BP81 are overlaid on top of one another and show identical spectral profiles.
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: Limb light distributions for a circular Titan. Case A (left panel) shows Titan as seen by an observer at mid-event with the star directly behind Titan’s disk. If Titan’s atmosphere is circularly symmetric, there will be a ring of light around the entire limb because the projected lines from the star to the limb are perpendicular to the isopycnal lines all around the disk. In case B, the star is offset from the center, and there are only two regions where the projected lines from the star are perpendicular to the isopycnal lines.
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 left panel shows the resolved image of Titan taken closest to mid-event, when the star is nearly directly behind Titan’s disk. The right panel is a diagram to show regions where the Δr level surface is perpendicular to the radial lines from star.
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: HazCam view of a wheel and tracks from the VIPER prototype vehicle, showcasing the front right wheel. The left image depicts the wheel in a straight position, while the right image shows the wheel steered at a 45° angle. The image has been processed using tone mapping based on Contrast Limited Adaptive Histogram Equalization (CLAHE) to enhance visibility. Note that the prototype camera used for this image has different distortion parameters than the flight configuration.
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: Laboratory test results collected on the VIPER MGRU test platform in the NASA SLOPE Lab. (a) Vehicle was driven uphill in loose GRC-1; (b) Vehicle was driven backwards downhill through tracks.
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: Illustration of wheelbase and track width parameters shown for three suspension ride height examples.
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 Module rendering with actuators denoted.
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: Rendering of VIPER on the lunar surface. The rover measures 2.5 m tall and 1.5 m in length and width.