adsabs/AstroCLIMB huggingface dataset:
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Our derived phase functions compared to the phase functions of nine water-ice crystal geometries frequently observed in terrestrial cirrus clouds, with appropriately Mars-like particle sizes.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: Native resolution integrated G395H (nrs2) spectrum of Callisto (R ∼  3000 at 4.3 μm, black) and a smoothed version of the same spectrum (R =  500, cyan), both of which were flux calibrated using P330E, with no thermal correction applied. Error bars have been suppressed for clarity. Features that are identified in both the P330E and solar-model-calibrated versions are bolded (see Figure 4 for solar-model-calibrated disk-integrated spectra). Features that are not detected in the solar-model-calibrated spectra are highlighted by question marks. The signal-to-noise is lower in this version likely because P330E (Vmag ∼  13) is considerably fainter than Callisto (Vmag ∼  6), making assessment of subtle features more challenging than in the higher-quality versions shown in, e.g., Figure 4.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: Band depth map for the “peak” component of the 4.38 μm 13CO2 band, highlighting the minor concentration of this component at low latitudes on Callisto's trailing hemisphere. The band center of this feature shows minimal variation, and it is very close to 4.38 μm in all spaxels where it was detected. Some spaxels do not show a peak component (black).
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: Continuum-divided, integrated G395H spectra of Io (purple) and non-Io-subtracted (orange) and Io-subtracted (cyan) integrated G395H spectra of Callisto. Each continuum-divided spectrum has been binned to an R of 500, and error bars have been suppressed for clarity.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: 4.57 μm band depth (top) and band center (bottom) error maps for data shown in Figure 8.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: 4.38 μm 13CO2 band depth (top) and band center (bottom) error maps for data shown in Figure 7.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Energy distribution of particles sputtered from enstatite (MgSiO3) irradiated by He ions at normal incidence  α  in = 0° and at 80° with respect to the surface normal. The legend contains the element-specific characteristic binding energy E 0, whereas E 0  ≈  2E peak.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Characteristic energy E 0 of the energy distributions of particles sputtered from enstatite (MgSiO3) irradiated by He ions at incident angles αin. For all species the E 0 is nearly constant but increases rapidly at grazing incident angles  α  in > 80°.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Sputter yields of Fe and S from troilite irradiated by SW ions in the model introduced in Jäggi et al. (2023) compared to the same model with a damage-driven diffusion coefficient of 7.5 × 102 Å4 at−1 (Christoph et al. 2022; HB-CD). Note that sputter yields become stoichiometric when they reach an equilibrium, which is not the case if surface S is depleted by diffusion in addition to being sputtered.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Polar angular distribution of normalized mass yield Y norm sputtered from enstatite (MgSiO3) by 4 keV He+ at increasing incident angles (αin) compared to experimental data (black; Biber et al. 2022) with errors of 2 standard deviations.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: SW IS data for Mercury’s southern hemisphere and northern low-Mg composition from McCoy et al. (2018) and Peplowski & Stockstill-Cahill (2019), respectively (Table 2). Energy and angular distributions are shown for an incident angle of 45°.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: SW IS data for a typical Lunar mare and Lunar highland composition (Heiken et al. 1991). Energy and angular distributions are shown for an incident angle of 45°.
Paper: Titan’s Atmospheric Albedo Asymmetry and Seasonal Variability Observed through the Cassini Imaging Science Subsystem
Authors: C. Snell, D. Banfield
Figure caption: Sample images from before (N1567440863_1), during (N1786775340_1), and after (N1852202278_1) the NSA reversal show how the NSA evolves over time. The north angle for each image is oriented toward the top of the figure (though the actual north pole may point somewhat into/out of the page), and the tilt in the NSA boundary is clearly visible in the top panel.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: The accretion rates for the three dust distributions at t = 0. The orange lines are the accretion rates in the Hill regime, the magenta lines are the accretion rates in the Bondi regime, and the green lines are the accretion rates in the geometric/focusing regime. The scatter points are color-coded corresponding to the ice volume fraction of the pebble of most efficient accretion at the given protoplanet mass. Left: accretion rates of the power-law distribution, which accrete no silicates except for a small window in the transition from geometric to Bondi, where roughly 20% of the material being accreted is silicate. Middle: the bimodal distribution begins accreting roughly 50% ice and 50% silicates in the geometric regime but then accretes nearly 100% silicates upon entering the Bondi regime. As a planetesimal grows through Bondi accretion, it begins to favor larger pebbles, thereby increasing the ice volume fraction that is being accreted, finally accreting mostly ices in the Hill regime. Right: accretion rates for the constant distribution, where all pebbles being accreted have a 0% ice volume fraction.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Density distribution of KBOs. Small KBOs have density around 0.5 g cm−3 (with some dispersion), implying porosity, whereas larger bodies have increasingly higher density. Values are from Bierson & Nimmo (2019, and references therein), Morgado et al. (2023), and Pereira et al. (2023).
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Internal density (top panels) and ice volume fraction (bottom panels) of accreted pebbles for the three models. Left: the power-law distribution in which the smallest grains are pure silicates and the largest pebbles are pure ice, with the trend that larger solids are icier. Middle: the bimodal distribution in which pebbles between micron and millimeter size are pure silicates and pebbles above this size are increasingly icier, with pebbles at 1 cm being pure ice. Right: the constant distribution, in which pebbles of all grain sizes have a 0% ice volume fraction and a density of ρ • = 3 g cm−3.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Left: graph of Equation (29), the parameterization we adopt for porosity. Right: densities, for constant ice mass fraction F  i , calculated with Equations (29) and (32) are shown with solid lines. The dashed lines of the same color show the density of a fully compact body of the same ice mass fraction.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Comparison of the energy distribution of sputtered particles for varying impactor energy E in of SW ions. The shift in the energy distribution at low E in is fully attributed to H, which shows an identical behavior by itself and He on enstatite expressing negligible (<0.2 eV) shifts. The legend contains the element-specific characteristic binding energy E 0, whereas E 0  ≈  2E peak.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Angular distribution of sputter yield from anorthite (CaAl2Si2O8) from combined H and He data (left) compared to simultaneous irradiation by H and He (right). In both cases the H:He ratio is 96:4 and the incident angle is 45°. Note that the largest difference in tilt angle (ϕ) is for the least sputtered species, Ca, which is assumed to be less heavily depleted in the simultaneous irradiation, causing a larger surface concentration and a more forward-faced ( α  < 0) angular distribution as a consequence.
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Azimuthal angular distribution of mass sputtered from enstatite (MgSiO3) by 4 keV He+ at increasing incident angles (αin). Only one hemisphere of the symmetrical distribution is shown. The azimuth angle of the impinging ion (black arrow) is located at 0°. Note the small remaining fraction of back-sputtered particles at grazing incidence angles ( α  in > 45°).
Paper: SpuBase: Solar Wind Ion Sputter Database for Modeling Purposes
Authors: Noah Jäggi, Herbert Biber, Johannes Brötzner, Paul Stefan Szabo, Andreas Mutzke, Jonathan Gasser, Friedrich Aumayr, Peter Wurz, André Galli
Figure caption: Surface S:Fe ratio in irradiated troilite comparison between this work (blue line) and reference simulation data (orange line; data from Figure 8 in Christoph et al. 2022).
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: The geometry of the DART impact observations as viewed from Earth and the Lucy spacecraft. Left: centered on the Sun (yellow) and showing the orbit of Earth (blue), the path of the DART spacecraft (white), and partial views of Didymos’s orbit (orange) and the path of the Lucy spacecraft (cyan). Right: centered on Didymos and depicting the orbit of Dimorphos (orange) and the directions to the Sun, the Lucy spacecraft, and Earth at the time of the DART spacecraft impact into Dimorphos. The table in the lower right corner gives the distance to Didymos from Earth and the Lucy spacecraft (Δ) and the solar phase angle (ϕ) at the time of impact.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Moving averages of the uncorrected (flat phase function) opacity data, split between the previously published MY 32 and 33 ACB seasons and the newly analyzed MY 34–36 seasons from this paper. In the top panel, the MY 32 and 33 data are presented using the scattering angle at the center of the Navcam frame, while in the bottom panel, we apply a 20° correction, typical of the angular distance between the center and analyzed points in the MY 34–36 data. Once this correction has been applied, we see that the dependence of opacity on scattering angle caused by the assumption of a flat phase function is nearly identical between the two data sets. This suggests that the application of the flat phase function assumption in previous studies was inappropriate.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Frequency of the scattering angles where clouds were observed during MYs 34–36, in 10° bins. Nearly all observations took place at scattering angles between 20° and 120°, which is a much wider range than was previously explored by Kloos et al. (2016, 2018). The increased number of observations at small scattering angles (close to the Sun) relative to MYs 31–33 is of particular interest since that is the regime in which Cooper et al. (2019) and Innanen et al. (2024) suggest that the scattering phase function deviates significantly from the flat, constant assumption used in the past.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: HC opacities as a function of scattering angle if the assumption of a flat phase function is used. The red line is a moving average with the associated 95% confidence interval. There is a clear, nonphysical upward trend in opacities sunward of approximately 60°, indicating that the flat phase function assumption is inappropriate in this regime. We have also indicated the movie type of each measurement to show that ZMs are more likely to observe low scattering angles than SHMs.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Diurnal coverage of the cloud observation campaign over the first five MYs of the mission. The ZM keepout window from local noon is clearly visible, as is the introduction of dedicated AM science time at the beginning of MY 33. Also visible are the gap in coverage around 10:00 LTST caused by the rover’s uplink schedule and the gaps that have opened up in MYs 35 and 36 as a result of the rover’s age restricting when science block time can be allocated. The ACB season is indicated by the yellow shaded regions, and the red shaded region is the MY 34 GDS.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Four frames from a high-quality ZM at three stages in the processing pipeline. In the top row are the raw frames, where the clouds are barely visible. In the middle row, MFS has been applied. The clouds are clearly visible here, but the contrast is still not great. In the bottom row, the middle 98% of the pixel values have been stretched, creating much better contrast between the high- and low-radiance points of each frame.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Looking for diurnal variability in the scattering phase function by comparing AM and PM phase functions for MYs 34–36. The shaded regions represent the 95% confidence interval of the moving average. There does not appear to be any significant difference between the AM and PM phase functions in any year, consistent with the findings of Innanen et al. (2024).
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Qualitative movie quality values, averaged across 50 bins of solar longitude and true solar time. Two quality peaks are visible: the ACB between L s = 50° and 170° and the height of the dusty season near L s = 300°.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: The evolution of the cloud observation campaign over the course of the MSL mission. The ZMs/SHMs and SPENDI/SuperSPENDI observations are taken at all times of year, while the CAO and PFSS are only executed during the ACB season, indicated by the yellow shaded regions. The temporal extent of the MY 34 GDS event is indicated by the red shaded region.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Comparative FOVs of MSL’s Navcams (NCAM) and the two Mastcams (MCAM-34 and MCAM-100). Also included for context is the FOV of the Phoenix Surface Stereo Imager (SSI), which Moores et al. (2010) used to observe polar clouds.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: (A) Voyager frame (vg-iss-2-u-c2683649; best resolution: ∼4.6 km pixel−1) cropped and contrast-adjusted. The black dots are control points. (B) Same as (A), but reprocessed to reduce camera motion blur. Note the improvement in image sharpness. (C) New geologic mapping in the same orientation as (A) and (B), based on reprocessed images of (B) with a legend. Triangles point in the downslope direction for scarps. Black regions were too poorly illuminated to map. More details on the definition of map units and explanation of map symbols, along with examples of terrain types, can be found in the Appendix (Tables A2–A3 and Figures A4–A5). The diameters and coordinates for all officially named features are listed in Table A1.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: Examples of features of interest identified in the updated mapping of Titania. Individual feature images have been contrast-adjusted. Outlines on reference images show the extent and context of the feature images. The base image of Titania is the same as Figure 4(B). Subpanels (A)–(C) are taken from the base image of Titania. (A) Example of a branching fracture on Titania. (B) A crater chain on Titania. (C) Valeria (59 km diameter) is a crater with a central peak.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: Test of result sensitivity to specific EM MAP probability estimate nonuniform blind deconvolution used. The results produced in panels (B) and (C) are nearly identical; the primary difference is the treatment of noise from bad pixels in the original image. (A) Voyager frame (vg-iss-2-u-c2683649) cropped and contrast-adjusted. The black dots are control points. (B) The same as (A), but reprocessed using the Shake Reduction tool in Adobe Photoshop CC 2018. (C) The same as (A), but reprocessed using the MATLAB codes from Levin et al. (2011).
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: (A) Voyager frame (vg-iss-1-j-c1638930) of Acala Fluctus, Tiermes Patera, Fuchi Patera, and the surrounding area on Io. The black dots are control points. (B) The same as (A), but reprocessed using a nonuniform blind deconvolution to reduce camera motion blur. (C) Unprocessed Voyager frame (vg-iss-1-j-c1638928) of a similar region as (A) and (B).
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: (A) Voyager frame (vg-iss-2-u-c2684539) of Ariel. The black dots are control points. (B) The same as (A), but reprocessed using a nonuniform blind deconvolution to reduce camera motion blur.