adsabs/AstroCLIMB huggingface dataset:
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: North polar LOLA roughness (meters) on 50 m baselines (left panel), LOLA 1064 nm normal albedo (middle panel), and LROC WAC 321 nm reflectance (right panel; Lunar QuickMap, https://quickmap.lroc.asu.edu/). The black square outlines the 80°–90° N region covered by the color-composite image (Figure 4), which is overlaid on the right panel where the WAC mosaic has no data. Roughness rays and lineaments are labeled with arrows.
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Examples of crater chains visible in the hillshaded topographic map (left panel) that appear as roughness lineaments in the RGB composite (right panel).
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Left: roughness spectra of the six k-means classes. Error bars represent the standard deviation of 1 km pixels for each class and baseline. Right: box plots of the roughness spectral slope of the classes. Each box shows the median (horizontal line), mean (plus symbol), interquartile range (box edges), and 9th/91st percentiles (whiskers).
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Slope in degrees (left column) and roughness in meters (right column) for baselines of 200 m (top row) and 1600 m (bottom row). The roughness color scale ranges from the 2nd to the 98th percentile.
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: 1 km pix−1 map of the k-means classes with cold to hot colors representing low to high roughness spectral slope.
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Hillshade of old (left) and new (right) 20 m pix−1 LDEM.
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: LEISA optical fringes in calibration data. For both frames, the long-wavelength end is at the top and the short-wavelength end is at the bottom. The round feature near the center is caused by the calibrator scatter plate, and the inverted-V-shaped feature across the bottom filters is from reflections off the cold snout surrounding LEISA. (a) Internal filament calibrator data show significant optical fringing apparent as higher-frequency diagonal lines. (b) Fringing is greatly reduced after applying a fringe flat correction.
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: The L’Ralph focal planes to scale. LEISA and MVIC share the same optical path but have different fields of view and spatial resolutions. The instrument scan mirror is used to scan a target across the MVIC or LEISA filters to build up spectral image cubes.
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: The reaction rate corresponding to reaction R1 (O2 + hν ⟶  O(3P) + O(3P)) at a pressure level around ∼1 hPa for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere. The pressure level corresponds to relatively fast reaction rates in the vertical distribution in Figure 6(a).
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: The reaction rate corresponding to reaction R16 (NO3 + hν ⟶  NO + O2) at a pressure level of ∼290 hPa for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere. The pressure level corresponds to relatively fast reaction rates in the vertical distribution in Figure 6(i).
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: The reaction rate corresponding to reaction R9 (HO2 + O3 ⟶  OH + 2O2) at a pressure level of ∼500 hPa for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere. The pressure level corresponds to relatively fast reaction rates in the vertical distribution in Figure 6(e).
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: The reaction rate corresponding to reaction R6 (H2O + O(1D)  ⟶  2OH) at a pressure level of ∼500 hPa for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere. The pressure level corresponds to relatively fast reaction rates in the vertical distribution in Figure 6(c).
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: MVIC stellar calibrations from 2023 March and 2024 March. (a) Panchromatic, violet, and green channels; (b) orange, phyllosilicate, and NIR channels. Stars were chosen separately for each channel based on signal level, and all bands show stable radiometric performance ±5% over that time period.
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: LEISA Arcturus calibration. The LEISA stellar scans were used to compare calibrated radiance with an Arcturus reference spectrum; the calibration coefficients from TVac (red points) were adjusted (blue points) to match the known radiance.
Paper: Plume Particle Ejecta Can Trace Habitat-forming Gradients in Ocean Worlds: Insights from Planet Earth Geochemistry
Authors: Mustafa Yücel, Nimet Alımlı, Naim Yağız Demir, Hilal Cura
Figure caption: (a) Pelagic nanoparticles from the offshore Black Sea (132 m depth) analyzed with TOF-ICP-MS. (b) Vent nanoparticles from the Lau Basin Kilo Moana vent area analyzed with Scanning Electron Microscopy–Energy Dispersive X-Ray Spectroscopy. Modified from M. Yücel et al. (2011).
Paper: Plume Particle Ejecta Can Trace Habitat-forming Gradients in Ocean Worlds: Insights from Planet Earth Geochemistry
Authors: Mustafa Yücel, Nimet Alımlı, Naim Yağız Demir, Hilal Cura
Figure caption: The conceptual scheme outlines the primary prerequisites for habitability in ocean worlds, highlighting the importance of water, energy, CHNOPS, and TMs. The horizontal bar on the bottom denotes our assessment of the extent of exploration of each subject area indicated in the top bar. Ocean worlds are not to scale. The Europa image is modified from the NASA Photojournal PIA01295, credit NASA/JPL/University of Arizona. The Titan image is modified from the NASA Photojournal PIA20016, credit NASA/JPL/University of Arizona/University of Idaho. The Callisto image is modified from the NASA Photojournal PIA03456, credit NASA/JPL/German Aerospace Center (DLR). The Enceladus image is modified from the NASA Photojournal PIA06187, credit NASA/JPL/Space Science Institute. The Ganymede image is modified from the NASA Photojournal PIA01972, credit NASA/JPL. The Pluto image is modified from the NASA Photojournal PIA11709, credit NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute. The Triton image is modified from the NASA Photojournal PIA01994, credit NASA/JPL.
Paper: Plume Particle Ejecta Can Trace Habitat-forming Gradients in Ocean Worlds: Insights from Planet Earth Geochemistry
Authors: Mustafa Yücel, Nimet Alımlı, Naim Yağız Demir, Hilal Cura
Figure caption: Illustration of possible formation processes of nanoparticles on ocean worlds. Red circles indicate plumogenic nanoparticles. Yellow circles signify pelagic nanoparticles. Green circles are for hydrothermal fluxes.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Trajectory error for each flyby. Both plots show the rms trajectory error for different cases. The top panel reports the trajectory error normalized by the trajectory uncertainty (indicated by σ and computed via Equation (A3)) together with its standard deviation (error bars), while the bottom plot shows the absolute value. The red, yellow, and green lines show the error when no calibration strategy is employed, using different models to simulate the IPT behavior (Phipps+18t B, Phipps+18t G, and Moirano+21t, respectively). The black line shows, for comparison, the error that one would obtain if the IPT were fully calibrated (or, equivalently, there was no IPT perturbation; this is equivalent to the uncertainty in the trajectory reconstruction, which strongly depends on orbital geometry and tracking opportunities). The horizontal black line in the top panel highlights the 3σ level.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Doppler perturbation computed from different IPT models for one Europa Clipper flyby (shown in Figure 2). The horizontal axis reports the time from the closest approach (C/A). The abrupt peaks visible in the signals in the left panel are due to discontinuities in the underlying models. The right panel shows the signal computed on the same flyby with the models modified using a nonlinear taper (see Appendix B). It can be clearly seen that the spurious peaks have been mitigated.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: rms perturbation of the IPT on the two-way Doppler tracking signal of Europa Clipper. The rms perturbation is computed only on the tracking data collected 10,000 km from the surface and lower. Different markers indicate different IPT electron density models; namely, Phipps+18 B and G refer to the B and G models in P. H. Phipps et al. (2018, 2021), Moirano+21 refers to the model defined by A. Moirano et al. (2021) using its central values, while the Moirano+21 (sample) indicates the same model but with model parameter values drawn from a normal distribution compatible with the uncertainty of the parameters reported in the manuscript. The horizontal line shows the approximate value of the expected data noise of Europa Clipper (∼0.1 mm s−1). All the models considered here have been smoothed with a nonlinear taper (hence the name suffix “t”; see Section 2.1 and Appendix B).
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Comparison of the radio beam path in the case of Juno (green lines) and Europa Clipper (light blue lines). In the background the electron density computed from Moirano+21 is shown to highlight that in certain geometries the radio beam of Europa Clipper might cross the discontinuity of the model (thin dark ring at ∼5 RJ), producing spurious spikes in the IPT Doppler perturbation computed from the model (see also Figure 3(a)). Horizontal and vertical axes denote the distance from Jupiter normalized by the Jupiter radius RJ. The white circle shows the orbit of Europa. All the quantities are drawn in an inertial reference frame aligned with the centrifugal equator.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Electron density distribution given by different models. Panels (A) and (B) show the Phipps B and Phipps G models, respectively (P. H. Phipps et al. 2018). Panels (C), (D), (E) and (F) show four time snapshots of the Moirano model (A. Moirano et al. 2021). The horizontal and vertical axes of all panels correspond to the x- and z-axes of the IPT centrifugal reference frame normalized by Jupiter radius RJ. All panels show a vertical slice of the electron density field at centrifugal longitude λ = 0.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Gravity field spherical harmonics coefficients’ reconstruction error normalized by their formal uncertainty (σ). Each panel reports the ratio between the estimation error and the formal uncertainty for all the solved-for coefficients in the classical tree representation; the vertical axis corresponds to the degree of the gravity field, the horizontal axis the order (with orders on the left representing C coefficients and S on the right). Panel (a) reports, for comparison, the expected estimation error in the fully compensated case; panel (b) shows the same quantity when the IPT is computed from the Phipps+18 B model and no calibration technique is applied. Phipps+18t G and Moirano+21t are shown in panels (c) and (d), respectively.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Formal uncertainty evolution of key geophysical parameters measured by the G/RS investigation. The curves represent the retrieved uncertainty on the parameters as a function of the number of flybys included in the analysis. All curves are normalized to the uncertainty attainable when analyzing the whole mission (49 flybys). The vertical line denotes the transition from EC1 to EC2, when the impact of the IPT will become substantial.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Spatial expansion of the gravity anomaly error, after normalization by the uncertainty. The four maps show the estimation error (in units of formal uncertainty σ) for the same cases discussed in Figure 8.
Paper: The Effect of the Io Plasma Torus on Precise Orbit Determination and Gravity Recovery: Application to Europa Clipper
Authors: Gael Cascioli, Erwan Mazarico, Flavio Petricca, Andrea Magnanini, Dustin R. Buccino, Martina Ciambellini, Antonio Genova, Luis Gomez Casajus, Marco Zannoni, Paolo Tortora
Figure caption: Radial electron density profiles obtained with two different models when applying a nonlinear taper to remove the discontinuities in the models (see Appendix B).
Paper: An Assessment of Organics Detection and Characterization on the Surface of Europa with Infrared Spectroscopy
Authors: Ishan Mishra, Nikole Lewis, Jonathan Lunine, Kevin P. Hand
Figure caption: Results of a BMC analysis of the data in Figure 10 are presented here. Top: retrieved posterior distributions of the abundance of the trace species (in log10 scale). The dashed purple lines are the median values along with the 2σ upper and lower bounds (95% confidence intervals). The solid vertical red lines indicate the true abundance of the trace species (0.01 for all) used as inputs to generate the data in Figure 10. Bottom: the columns from left to right show the detection significance (σbmc) and retrieved logarithmic and regular abundance estimates (median ± 2σ) of each trace species.
Paper: An Assessment of Organics Detection and Characterization on the Surface of Europa with Infrared Spectroscopy
Authors: Ishan Mishra, Nikole Lewis, Jonathan Lunine, Kevin P. Hand
Figure caption: Sensitivity of the water + HCN spectrum to physical parameters in our model. From the top left and clockwise, a set of spectra for varying values of incidence angle, phase angle, porosity, and grain size (of trace species) are shown. Emergence angle sensitivity has not been shown here since it is equivalent to the incidence angle sensitivity. Phase angle and porosity have the effect of changing the overall amplitude of the spectrum. Incidence (and emergence) angle changes the amplitude of the features, with smaller values (less extreme geometry) more desirable for prominent features. Larger grain size of the trace species also leads to deeper and prominent features.
Paper: An Assessment of Organics Detection and Characterization on the Surface of Europa with Infrared Spectroscopy
Authors: Ishan Mishra, Nikole Lewis, Jonathan Lunine, Kevin P. Hand
Figure caption: Maximum likelihood (ML) solutions for two models and the residuals of their fit to the simulated data from Figure 10 are shown. Note that the Hapke model has been used to generate simulated data (see Figure 2), as well as for the model fits. The model on the left has all 10 trace species (and water) from Table 1. The model on the right has all of them as well, except HCN. While the random distribution of the residuals on the left signifies a good fit, the residuals on the right clearly show systematic trends caused by the removal of HCN. This signifies the effect of HCN on the continuum of the total spectrum, just like in Figure 8, resulting in a strong detection of HCN (>8σ) when the two models shown here are compared. The reduced χ2 values of the fits also show how the fit suffers by excluding HCN from the model.
Paper: Seasonal Evolution of Titan’s Stratospheric Tilt and Temperature Field at High Resolution from Cassini/CIRS
Authors: Lucy Wright, Nicholas A. Teanby, Patrick G. J. Irwin, Conor A. Nixon, Nicholas A. Lombardo, Juan M. Lora, Daniel Mitchell
Figure caption: Example fits to averaged CIRS FP4 spectra and retrieved temperature profiles at some selected times and latitudes. Left panels show the fitted spectrum (solid lines) and measurement plus forward modeling error envelope (shaded regions). Middle panels show the retrieved atmospheric temperature profile (solid lines) and error envelope (shaded regions). The a priori temperature profiles are also plotted (dashed lines). Right panels show the corresponding contribution functions. Contribution function peaks indicate the pressure region that our nadir observations are most sensitive to. Examples are shown in Titan northern midwinter (top panels) and late northern spring (bottom panels). Winter polar latitudes are shown in dark blue, winter midlatitudes in light blue, and spring/summer midlatitudes in yellow. The contribution function shown, ﹩{\tfrac{dR}{dT}}_{\mathrm{total}}﹩, is ﹩\frac{dR}{dT}﹩ summed over the fitted spectral range (1240–1360 cm−1), where R is radiance and T is temperature. Observations probe higher altitudes (lower pressures) near the winter pole (dark-blue lines).
Paper: Seasonal Evolution of Titan’s Stratospheric Tilt and Temperature Field at High Resolution from Cassini/CIRS
Authors: Lucy Wright, Nicholas A. Teanby, Patrick G. J. Irwin, Conor A. Nixon, Nicholas A. Lombardo, Juan M. Lora, Daniel Mitchell
Figure caption: Observation sequences used in this study. Spectra are binned in 2° latitude bins. Points are plotted at the central latitude of the bin and at the average longitude of the bin. Color indicates the acquisition date of the observation.
Paper: Seasonal Evolution of Titan’s Stratospheric Tilt and Temperature Field at High Resolution from Cassini/CIRS
Authors: Lucy Wright, Nicholas A. Teanby, Patrick G. J. Irwin, Conor A. Nixon, Nicholas A. Lombardo, Juan M. Lora, Daniel Mitchell
Figure caption: Latitude variation of retrieved temperature at the 1 mbar pressure level. A stratospheric tilt correction is applied in the Saturn-, solar-, and inertial-fixed reference frames using the optimal tilts determined by J. Sharkey et al. (2020, their Table 2). The points are colored according to the mean longitude of the observation sequence, to distinguish observations. A typical retrieved temperature error bar is shown for each 2 yr period. The tilt-corrected distributions generally exhibit less spread; this is particularly clear at around ±40° north (depending on the time of year), where the meridional temperature gradient is greatest.
Paper: Seasonal Evolution of Titan’s Stratospheric Tilt and Temperature Field at High Resolution from Cassini/CIRS
Authors: Lucy Wright, Nicholas A. Teanby, Patrick G. J. Irwin, Conor A. Nixon, Nicholas A. Lombardo, Juan M. Lora, Daniel Mitchell
Figure caption: Grid search for optimal tilt magnitude and direction in the Saturn-fixed reference frame. χ2 contours are shown. The location of the minimum χ2 value is indicated with a red cross, and the 1σ (red) and 3σ (orange) confidence bounds are plotted. χ2 quantifies the spread of temperature–latitude distributions at the 1 mbar pressure level, in each 2 yr bin. The number of observation sequences, Nobs, used in each bin is given.