adsabs/AstroCLIMB huggingface dataset:
Paper: Gauss-Radau Small-body Simulator (GRSS): An Open-source Library for Planetary Defense
Authors: Rahil Makadia, Davide Farnocchia, Steven R. Chesley, Siegfried Eggl
Figure caption: Keyhole map for (101955) Bennu during its Earth close encounter in 2135. The left ordinate shows the probability distribution of the ζ coordinate on the Öpik B-plane. The right ordinate shows the width of the keyholes plotted using vertical bars. Keyholes with a width greater than 1 km are labeled with their corresponding impact years. In addition, keyholes with an impact probability greater than 10−5 are highlighted as filled squares. Note the different scales on the two ordinates.
Paper: Gauss-Radau Small-body Simulator (GRSS): An Open-source Library for Planetary Defense
Authors: Rahil Makadia, Davide Farnocchia, Steven R. Chesley, Siegfried Eggl
Figure caption: Impact location over central Europe (52﹩\mathop{.}\limits^{^\circ }﹩585 north, 12﹩\mathop{.}\limits^{^\circ }﹩357 east) at 100 km altitude for 2024 BX1 (red circle, left panel) and a comparison of the impact locations (middle panel) and impact times (right panel) computed by JPL and GRSS.
Paper: Gauss-Radau Small-body Simulator (GRSS): An Open-source Library for Planetary Defense
Authors: Rahil Makadia, Davide Farnocchia, Steven R. Chesley, Siegfried Eggl
Figure caption: Results of the 250 yr round-trip propagation errors of Didymos in GRSS. The error magnitude in the final position compared to the initial conditions is less than 30 m.
Paper: Gauss-Radau Small-body Simulator (GRSS): An Open-source Library for Planetary Defense
Authors: Rahil Makadia, Davide Farnocchia, Steven R. Chesley, Siegfried Eggl
Figure caption: Results of the 250 yr propagation of Didymos in GRSS compared to the results of the same propagation in the ASSIST orbit propagation library. The maximum position magnitude difference between the two integrators is less than 5 m.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Input temperature (left) and static stability parameter (right). The model’s vertical layers are shown with the blue lines. We apply this profile at a latitude of 23° north, which we found to produce the most stable configuration.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: The vertically integrated ammonia (left) and water (right) clouds in the model 70 days into the simulation after adding the perturbations. Note the increase in both the ammonia and water cloud density with the increase in wind shear.
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Top: I/F from CH4-band (889 nm) Hubble observations and the corresponding cloud-top location used in our wind initialization. Bottom: the input zonal wind speed applied at the corresponding pressure level. Both from J. Tollefson et al. (2017).
Paper: Wind Shear and the Role of Eddy Vapor Transport in Driving Water Convection on Jupiter
Authors: Ramanakumar Sankar, Michael H. Wong, Csaba Palotai, Shawn Brueshaber
Figure caption: Shear profile for different values of m used in the model.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Photochemical calculations for a TRAPPIST-1 e anoxic atmosphere for a wide variety of CO2 pressure logarithmically spaced between 10−3 (1000 ppmv) and 0.5 bars (50% v/v) and CH4 flux logarithmically spaced between 0.1 and 100 Tmol yr−1 (approximately between 4 × 109 molecules cm−2 s−1 and 5 × 1011 molecules cm−2 s−1). The left panel shows surface CH4 mixing ratios. The contour lines correspond to CH4 mixing ratios of 1, 10, 100, 1000, and 10,000 ppm (left to right). The right panel shows the column density of hydrocarbon haze particles in cm2. The dashed red line indicates the approximate τ = 1 extinction contour at 550 nm. Only at the highest CH4 does haze become significant. Calculations assume a 1-bar atmosphere with N2 as the filling gas and include the formation of fractal hydrocarbon hazes.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: QMC selection of points from the photochemical model parameter space. The total sequence of 32 points is separated into three samples: the first 8 cases (left), the next 8 cases (middle), and the remaining 16 cases (right).
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: The left panel plots the global mean surface temperature vs. CO2 mixing ratio for all 32 ExoCAM simulations. Circles are color-coded via their CH4 mixing ratio. The right panel similarly shows the global mean temperatures, but plotted vs. CH4 on the x-axis and with circles color-coded by the CO2 mixing ratio.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Transmission spectra for our four representative cases.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Each panel shows global mean climate quantities plotted against the global mean surface temperature on the x-axis, with data points color-coded by the CH4 volume mixing ratio. While quantities generally display dependencies that can be linked to the surface temperature, high-CH4 cases are outliers.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Haze column mass from case 23. The left panel shows the haze mass integrated through the whole atmospheric column. The right panel show the haze mass integrated from 1 mbar to the top of the model.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Vertical profiles of temperature, haze mass, and haze effective radii for our three hazy cases (7, 23, 26). In the left panel, dashed lines indicate the temperature profile when no haze is assumed to form and with all else being equal. In the right panel, solid lines show the fractal aggregate radii and dashed lines show the radii if each aggregate were condensed into a solid sphere.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Contour plots of surface temperature, cloud water column, albedo, and OLR for our four representative climate states.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: The TRAPPIST-1 spectral energy distribution (top panel) compared against the haze mass absorption coefficient for a ∼1 μm particle (bottom panel). The light-yellow histogram in the top panel shows the GCM gridded stellar spectrum. The bottom panel illustrates differences between the optical properties of fractal aggregates vs. equivalent-mass Mie particles.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Vertical structure of temperature, specific humidity, and cloud water for our four representative cases. Note that case 23, which includes haze, was run with a higher model top than the nonhazy cases. Solid, dashed, and dotted lines show the global mean, substellar hemisphere mean, and antistellar hemisphere mean, respectively.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Polar plot showing the Henyey–Greenstein scattering phase function at 0.86 μm for the fractal (orange) and Mie (green) haze optical properties assuming an effective radius of 0.5 μm. The Rayleigh scattering phase function (purple dashes) is also display for comparison.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Transmission spectra for case 23 considering fractal aggregate haze, Mie haze, and no haze.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Kriging interpolation of the 32 ExoCAM simulations. The black circles show the ExoCAM simulations. Panels are shown and labeled for the global mean surface temperature, albedo, ice fraction, and OLR.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Kriging interpolation of the number of transits needed to detect CO2 and CH4 at 5σ.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Kriging interpolation of the 32 ExoCAM simulations. The black circles show the ExoCAM simulations. Panels are shown and labeled for the column-integrated water vapor, liquid water clouds, ice water clouds, and cloud fraction.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Kriging interpolation of surface temperature for the 32 ExoCAM simulations, with separate interpolations shown for Sample 1, Sample 2, Sample 1+2, and Sample 3. The black circles show the ExoCAM simulations. With each additional sequence the emulation of the parameter space is refined.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Root of the kriging variance across the parameter space from the kriging interpolation of the 32 ExoCAM simulations. Panels are shown and labeled for the column-integrated water vapor, liquid water clouds, ice water clouds, and cloud fraction.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Root of the kriging variance across the parameter space from the kriging interpolation of the 32 ExoCAM simulations. Panels are shown and labeled for the global mean surface temperature, albedo, ice fraction, and OLR.
Paper: Chemistry, Climate, and Transmission Spectra of TRAPPIST-1 e Explored with a Multimodel Sparse Sampled Ensemble
Authors: Eric T. Wolf, Edward W. Schwieterman, Jacob Haqq-Misra, Thomas J. Fauchez, Sandra T. Bastelberger, Michaela Leung, Sarah Peacock, Geronimo L. Villanueva, Ravi K. Kopparapu
Figure caption: Root of the kriging variance across the parameter space from the kriging interpolation of the number of transits needed to detect CO2 and CH4 at 5σ.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the single-scattering albedo for a range of wavelengths for ROI #1 (top) compared to a representative spectrum from the area from cube e6e007ci (bottom; modified from G. Cruz Mermy et al. 2023). The large absorption bands of the reference spectrum (bottom) are clearly visible in the reconstructed single-scattering spectrum (top). The data shown in the top panel are available in machine readable format.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Spectral (top) and angular coverage (bottom) of the NIMS data set on Europa. For each 1° × 1° range in longitude and latitude, the color represents the number of unique wavelengths (top) and the number of 5° phase-angle bins between 0° and 180° with at least one value for all the cube pixels that fall within that geographical area. No scaling is applied. The black boxes represent the ROIs that will be discussed in this paper (see Section 2). Basemap: Björn Jonssón (B. Jónsson 2015).
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the macroscopic roughness ﹩\bar{\theta }﹩ for a range of wavelengths for ROI #1. The values estimated from the mean posterior pdf are shown in blue; red points represent the values with the highest likelihood.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Example of phase curves extracted from the NIMS database (T. Cornet et al. 2022; T. Cornet et al. 2024) for four different wavelengths in ROI #1.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Map of Europa (credit: B. Jónsson 2015) highlighting the ROIs in this study—ROI #1 covers Rhadamanthys Linea and Harmonia Linea, ROI #2 is centered on crater Pwyll, and ROI #3 is to the southeast of Argadnel Regio. They were chosen for the scientific interest, as well as for the relative quality of the available photometric data set.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Variation of the macroscopic roughness ﹩\bar{\theta }﹩ vs. the single-scattering albedo ω estimated for the mean posterior pdf’s.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Phase curve for ROI #1 at λ = 1.72 μm. In black are the data points; in blue, the phase curve modeled from the estimated Hapke parameters by the mean posterior pdf; in red, the phase curve modeled from the estimated Hapke parameters by the maximum likelihood of each distribution.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Corner plot showing 1D and 2D histograms of the posterior pdf’s for each Hapke parameter for ROI #1 at λ = 1.72μm. The diagonal plots represent the single posterior pdf per parameter, which allows us to visualize how constrained the solution is. The 2D histograms allow us to examine any possible correlation between a given parameter and all the others. In this example, the posterior distribution for the asymmetry parameter b in the upper left corner of the figure is quite narrow and illustrates how well b is constrained and that only one value is highly probable based on the data provided. On the other hand, in the lower right corner we find the posterior distributions for the opposition parameters, h and B0, to be wide ranging, almost uniform. This illustrates that hardly any relevant information could be derived from the available data for these two parameters.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the backscattering fraction b vs. the asymmetry parameter c for ROI #1 superimposed with the hockey stick relation (B. Hapke 2012).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Corner plot showing 1D and 2D histograms of the posterior pdf’s for each Hapke parameter for ROI #1 at λ = 2.48 μm. The diagonal plots represent the single posterior pdf per parameter, which allows us to visualize how constrained the solution is. The 2D histograms allow us to examine any possible correlation between a given parameter and all the others. In this particular example, the posterior pdf’s almost all remained uniform. This is because we did not have a lot of data points for this wavelength—the only parameter where any information can really be gathered is the single-scattering albedo.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Illustration of the physical significance of two-parameter Henyey–Greenstein particle phase function.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the macroscopic roughness ﹩\overline{\theta }﹩ for a range of wavelengths for ROI #2.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the single-scattering albedo ω for a range of wavelengths for ROI #2.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Detailed phase coverage for every 40 nm wavelength interval in ROI #1. In particular, it is clear that the coverage is not equivalent for all wavelengths and that this is directly impacting the constraints we can derive for the different photometric parameters in the model.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Variation of the macroscopic roughness ﹩\bar{\theta }﹩ vs. the single-scattering albedo ω for ROI # 2.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the backscattering fraction b vs. the asymmetry parameter c for ROI #2 superimposed with the hockey stick relation (B. Hapke 2012).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the backscattering fraction b vs. the asymmetry parameter c for ROI #3 superimposed with the hockey stick relation (B. Hapke 2012).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)