adsabs/AstroCLIMB huggingface dataset:
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Map of total backscatter power (i.e., S 1) in dB scale around the region of Wiechert J crater, annotated as B following Figure 2. The color map scales from 1.5× the interquartile range below the lower quartile (blue) to 1.5× the interquartile range above the upper quartile (yellow) and as such follows a box plot from the lower and upper whiskers. The radar image is draped over a terrain hillshade model (Barker et al. 2023). Magenta arrows point out craters that exhibit asymmetric, extended ejecta deposits that point downrange from Tycho. The image ranges from 88°S, 205°E (top left) to 84°S, 159°E (bottom right). A high-resolution LRO NAC image for the secondary craters noted by the magenta box is shown on the right.
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Arecibo S-band SC radar backscatter in dB scale. Radar backscatter intensity increases from cool colors to warm colors. The magenta arrows point to the Tycho ray, and the letter A denotes the location of Newton crater. The Artemis III Haworth candidate landing site is noted with a white square. Image resolution is 0.08 km pixel−1.
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Diffusive CPR (left) and CPR (right) as a function of ((a) and (d)) distance along the ray in terms of Tycho crater radii (42.5 km), as well as distance from north to south for the ((b) and (e)) left and ((c) and (f)) right sides of the ray. Values were calculated over 15 km × 15 km square elements, shown as filled points with corresponding uncertainty for CPRdiff (purple) and CPR (orange). Some error bars are smaller than the point size. The 2σ prediction interval for the LSF line, shown in black, is the shaded gray area.
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Map of m-χ decomposition over the Newton crater group, annotated following Figure 2, where A denotes Newton crater. The image is formed by combining two orthorectified Mini-RF zoom mode (0.03 km resolution) collects. Magenta arrows note examples of craters with extended ejecta deposits. The image ranges from 77°S, 343°E (top) and 81°S, 338°E. North is up.
Paper: The History of Eruptions at Acala Fluctus, Io: Source of Multiple Outbursts
Authors: Julie A. Rathbun, Madeline Pettine, Moses Milazzo, Christian Tate
Figure caption: Brightness of Acala as measured by IRTF occultation lightcurves showing two outbursts and a lower level of activity before, after, and in between. The data used for this figure are available in associated data.(The data used to create this figure are available.)
Paper: The History of Eruptions at Acala Fluctus, Io: Source of Multiple Outbursts
Authors: Julie A. Rathbun, Madeline Pettine, Moses Milazzo, Christian Tate
Figure caption: Similar to Figure 2, showing the same information plus all of the locations determined from occultation curves shown in Figure 4. The dates of each observation are listed at left in the same colors as the plotted lines.
Paper: The History of Eruptions at Acala Fluctus, Io: Source of Multiple Outbursts
Authors: Julie A. Rathbun, Madeline Pettine, Moses Milazzo, Christian Tate
Figure caption: Occultation lightcurves used to determine the brightnesses shown in Figure 3. Lightcurves are plotted offset from each other for clarity. The dotted vertical lines are the occultation phase of Acala.
Paper: The History of Eruptions at Acala Fluctus, Io: Source of Multiple Outbursts
Authors: Julie A. Rathbun, Madeline Pettine, Moses Milazzo, Christian Tate
Figure caption: The lightcurve from 2019 September 11, as an example of measuring Acala’s brightness. The plus signs are the measured brightness of Io, while the diamonds and dashed line are our fit to the measurements.
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Modeled mixtures of magnesium-rich pyroxenes and olivines plotted alongside the spectrum of 267 Tirza and 1268 Libya. The addition of pyroxene to the olivine mixtures changes the behavior of the spectrum at long wavelengths, broadening this emission feature from the distinct emission peak(s) seen in the spectra of olivine and pyroxene alone. Spectral features of olivine are marked in light green, and those of pyroxenes are marked in dark purple to highlight commonalities with the asteroid spectra. The feature at 19.5 μm is common to both olivine and pyroxene. The spectrum of 267 Tirza in particular shows evidence of both olivine and pyroxene. All mixtures shown here contain both amorphous and crystalline silicates mixed in a 3:1 ratio, while the proportion of olivine and pyroxene is varied. The shaded gray box highlights the location of a known artifact in the SL Spitzer data (the SL teardrop). Spectra of crystalline silicates are sourced from Chihara et al. (2002) and Koike et al. (2003), and spectra of amorphous silicates are derived from optical constants from Jäger et al. (1994, 2003) and Dorschner et al. (1995) (see text for modeling details and silicate compositions).
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: 386 Haidea is distinguished from other asteroids in our sample by its shortward skew and lack of an 11 μm olivine shoulder, which could be due to a relatively olivine-poor composition. The 10 μm plateau in the pyroxene and phyllosilicate spectra is also skewed to shorter wavelengths and provides a closer match to the shape of 368 Haidea’s 10 μm feature than either forsteritic or fayalitic olivine does. Either of these minerals may be able to account for 386 Haidea’s unusual spectrum and could point to a geochemical history different from the olivine-dominated spectra of the other asteroids in our sample. Pyroxene and olivine spectra are modeled as 1:1 mixtures of amorphous and crystalline silicates based on optical constants from Jäger et al. (1994, 2003), Dorschner et al. (1995), and Chihara et al. (2002). The saponite spectrum is measured in relative absorbance as derived by Beck et al. (2014) via measurements originally made by Salisbury et al. (1991). The shaded gray box highlights the location of a known artifact in the SL Spitzer data (the SL teardrop). Spectra of crystalline silicates are sourced from Chihara et al. (2002) and Koike et al. (2003), and spectra of amorphous silicates are derived from optical constants from Jäger et al. (1994, 2003) and Dorschner et al. (1995) (see text for modeling details and silicate compositions).
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Modeled mixtures of magnesium-rich crystalline and amorphous olivine compared to the spectrum of 944 Hidalgo. Increasing the proportion of amorphous olivine in these mixtures dampens the spectral contrast of the smaller peaks superimposed on the 10 μm silicate plateau, suggesting a high proportion of amorphous silicates among the asteroids observed with Spitzer and SOFIA. The shaded gray box highlights the location of a known artifact in the SL Spitzer data (the SL teardrop). Spectra of crystalline silicates are sourced from Chihara et al. (2002) and Koike et al. (2003), and spectra of amorphous silicates are derived from optical constants from Jäger et al. (1994, 2003) and Dorschner et al. (1995) (see text for modeling details and silicate compositions).
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Comparison of the spectra of 588 Achilles from Martin & Emery (2023) to 944 Hidalgo and 368 Haidea (this study). In the VNIR, 588 Achilles, 944 Hidalgo, and 368 Haidea are all classified as D-types and have similar albedos, yet 368 Haidea lacks a strong peak or shoulder in the 11 μm region indicative of olivine (see highlighted region). Comparing the spectra of 944 Hidalgo and 588 Achilles, we can also see how the asteroids examined in this work have shallower continuum slopes and more leftward-skewed 10 μm features than the Trojans in Martin & Emery (2023).
Paper: Comparative Mid-infrared Spectroscopy of Dark, Primitive Asteroids: Does Shared Taxonomic Class Indicate Shared Silicate Composition?
Authors: Oriel A. Humes, Audrey C. Martin, Cristina A. Thomas, Joshua P. Emery
Figure caption: Graphical explanation of the band parameters of the 10 μm feature, with the spectrum of 87 Sylvia, normalized to an average emissivity of 1, as an example. Band parameters are measured as described in Martin (2022), except for skew (see text).
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Sensitivity of the gravity spectrum (left) and MOIF (right) to variations of the ocean depth. The shaded areas in the right panel represent the predicted uncertainty in the MOIF retrieval in the case of hydrostatic equilibrium (yellow area) and nonhydrostatic equilibrium (blue area).
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Common parameters: estimated posterior distributions in the Case 6 scenario; comparison of the posterior distributions of the Bayesian inversion showing only the parameters to which both methods are sensitive. The brown quantities are relative to the MOI-only case, while the blue quantities are relative to the combination of MOI, Mass, and gravity spectrum. The solid black lines show the true value of the parameters used as input to the whole process.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Bayesian inversion results for the nonhydrostatic case in the MMS and MM scenarios. The tables report the outcome of the two metrics in colors (green = Pass, yellow = Marginal, red = Fail). The numerical values for Metric 1 report the estimation error (as defined in the text, true value – estimated value), and the Metric 2 numerical values report the width of the 68.7% HDI interval, corresponding to the width of ±1σ for a normal distribution).
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Bayesian inversion results for the hydrostatic case in the MMS and MM scenarios. The tables report the outcome of the two metrics in colors (green = Pass, yellow = Marginal, red = Fail). The numerical values for Metric 1 report the estimation error (as defined in the text, true value – estimated value), and the Metric 2 numerical values report the width of the 68.7% HDI interval, corresponding to the width of ±1σ for a normal distribution).
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Parameters specific to the MMS method: estimated posterior distributions in the Case 6 scenario; comparison of the posterior distributions of the Bayesian inversion showing the parameters to which only the MMS method is sensitive. The solid black lines show the true value of the parameters used as input to the whole process.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing β on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: The Moon’s gravity field (GRGM1200A) amplitude spectrum and associated uncertainty.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing d crust on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing d ice on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing ρ water on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Full results for the MMS-Hydrostatic case. The numbers and colors follow the same definition as Figures 8 and 9.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing δ h topo on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing ρ mantle on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing ρ crust on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing d ocean on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing R core on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing ρ core on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Effect of changing T e on the gravity spectrum (left) and on the MOIF (right). The shaded areas have the same meaning as Figure 7.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. II. Effective Observation Geometry for Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: The two truth DTMs were used for testing. (a) The truth DTM, Shape 3, that was used for most tests. Its entire surface is rough with large boulders. These roughness attributes were generated according to observations at asteroids Eros and Itokowa (see Barnouin et al. 2020, for details). The width of the entire DTM is 500 m. (b) The simplified terrain, created to elucidate the effects of craters and hills on the performance of SPC. The slopes were well delineated, making deviations between this truth model and the SPC-derived DTM easily quantifiable. The width of simplified DTM is only 50 m.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. II. Effective Observation Geometry for Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: Polar plot of the positions of the simulated images as viewed from the surface. The positions of the spacecraft are gray squares, and the Sun is the orange circle. This was a result of test F3C-X6, in which we identified a suite of images that provided a good data set for SPC. Topography is determined by the spacecraft at cardinal directions, with the Sun on each side of the location. Albedo is determined by the Sun at a low incidence angle and, in this case, with the spacecraft south of the location.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. II. Effective Observation Geometry for Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: Imaging geometries for the Expanded Observational Conditions test. The polar plot shows the position of the spacecraft (gray filled squares) and the position of the Sun (orange filled circles). Both plots are viewed from the surface, looking up. The radial gridlines indicate azimuth, where north is 0° and east is 90°. The concentric gridlines indicate the zenith angle, with 0° being straight up.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. II. Effective Observation Geometry for Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: The results of input data and processing on the DTM quality. Each image was rendered with a 1 cm pixel size and only differed in the amount of processing applied. The DTMs represented by panels (a), (b), and (c) were generated using the same imagery but had different maplet GSDs. One can see the improvement in DTM quality due to better image data. Panels (c) and (d) show the improvement in DTM quality with higher-resolution images even if the maplet GSD does not change. The quality of terrain that SPC can generate is a function of both the pixel size of the imagery and the GSD of the desired DTM.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. II. Effective Observation Geometry for Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: (a) DTM produced using four images. The rms was 7.1 cm, and the normalized cross-correlation score was 0.9373. (b) DTM produced using 140 images. The rms was 7.5 cm, only about half a centimeter better than the four-image DTM, and the normalized cross-correlation score was 0.9416. One can see that there is only a small improvement from (a) to (b), with the latter having slightly sharper edges.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption:  Full results for the MM-Nonhydrostatic case. The numbers and colors follow the same definition as Figures 8 and 9.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption:  Full results for the MMS-Nonhydrostatic case. The numbers and colors follow the same definition as Figures 8 and 9.
Paper: Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission
Authors: G. Cascioli, E. Mazarico, A. J. Dombard, F. Nimmo
Figure caption: Full results for the MM-Hydrostatic case. The numbers and colors follow the same definition as Figures 8 and 9.
Paper: The History of Eruptions at Acala Fluctus, Io: Source of Multiple Outbursts
Authors: Julie A. Rathbun, Madeline Pettine, Moses Milazzo, Christian Tate
Figure caption: Io base map image with hot-spot locations overlaid. The circle is the location of the outburst from sunlit images obtained on 2019 June 25. The curved lines are the 1D locations of the outbursts observed in occultation curves on 2019 May 8 and June 25. The dark feature to the left and near the crossing of those curves is Acala Fluctus, which is also outlined in white.