adsabs/AstroCLIMB huggingface dataset:
Paper: Polarimetry of Didymos–Dimorphos: Unexpected Long-term Effects of the DART Impact
Authors: Zuri Gray, Stefano Bagnulo, Mikael Granvik, Alberto Cellino, Geraint H. Jones, Ludmilla Kolokolova, Fernando Moreno, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: The polarimetric phase curves of Didymos–Dimorphos in the BVRI filters. The vertical blue line indicates the phase angle of the asteroid system at the time of the DART impact (∼53.2°). The SpPol data points refer to the spectropolarimetric measurements taken with the VLT by Bagnulo et al. (2023), while the ImPol data points refer to the imaging (aperture) polarimetric measurements taken with the VLT and NOT (this study). In each plot, the black symbols and curve represent pre-impact measurements and their best fit, while the colored symbols and curve represent post-impact measurements and fit. The shaded area around the curves (where applicable) represents 1σ of the fit. In the case of the ImPol measurements, the open and filled data points are measurements taken when the phase angle was increasing (d α/dt > 0) and decreasing (d α/dt < 0, after α peak at 76.34° on 2022 October 21), respectively.
Paper: Polarimetry of Didymos–Dimorphos: Unexpected Long-term Effects of the DART Impact
Authors: Zuri Gray, Stefano Bagnulo, Mikael Granvik, Alberto Cellino, Geraint H. Jones, Ludmilla Kolokolova, Fernando Moreno, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Polarimetric maps of VLT data of Didymos–Dimorphos in the B and R filters. The color of each pixel represents the value of polarization as given in the color bar. Pixels with values outside the (−2, 10)% range have been set to white. The phase angle, date of each observation, and value measured from aperture polarimetry (P  Q ) are indicated in each row. The north (N), east (E), anti-solar (−⊙), and velocity (v) directions are given in the panels to the left of the maps. Panels are left blank in cases where there is no data. Gaps in the tail and the spurious tail of 2022 October 20 (R filter) are due to background stars.
Paper: Polarimetry of Didymos–Dimorphos: Unexpected Long-term Effects of the DART Impact
Authors: Zuri Gray, Stefano Bagnulo, Mikael Granvik, Alberto Cellino, Geraint H. Jones, Ludmilla Kolokolova, Fernando Moreno, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: The difference between the calculated pre-impact curve and the measurements of the degree of linear polarization, i.e., the value of the pre-impact curve minus the value of data points between phase angles 30°–65°. The symbols are as those in Figure 2.
Paper: Polarimetry of Didymos–Dimorphos: Unexpected Long-term Effects of the DART Impact
Authors: Zuri Gray, Stefano Bagnulo, Mikael Granvik, Alberto Cellino, Geraint H. Jones, Ludmilla Kolokolova, Fernando Moreno, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: The ratio between measurements of the polarization of Didymos–Dimorphos (B and R filters) and the fit of the post-impact data at the corresponding phase angle, phased according to the rotation period of Didymos (2.26 hr). The left panels show the original, individual measurements compared to the fit, and the right panels show the weighted average of measurements grouped together in steps of 0.1 rotation fractions. The symbols are as in Figure 2, with the data points around phase angles 75°–76° highlighted in light blue and yellow.
Paper: Polarimetry of Didymos–Dimorphos: Unexpected Long-term Effects of the DART Impact
Authors: Zuri Gray, Stefano Bagnulo, Mikael Granvik, Alberto Cellino, Geraint H. Jones, Ludmilla Kolokolova, Fernando Moreno, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Polarimetric phase curve of Didymos compared to S-type asteroids. The MBAs are shown with filled, gray data points, while the NEAs are shown in open, gray points. Same as Figure 2, the black points and curve represent pre-impact data, while the blue, green, red, and pink points and fits represent the post-impact Didymos data (in the BVRI filters, respectively). The solid data points represent observations that were taken after the phase angle peak was reached on October 20. In the plot for the V filter, the majority of the Didymos–Dimorphos data points are values which have been converted from the R filter using Equation (6).
Paper: Polarimetry of Didymos–Dimorphos: Unexpected Long-term Effects of the DART Impact
Authors: Zuri Gray, Stefano Bagnulo, Mikael Granvik, Alberto Cellino, Geraint H. Jones, Ludmilla Kolokolova, Fernando Moreno, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Imaging maps of VLT data of Didymos–Dimorphos in the B and R filters. The phase angle and date of each observation are indicated in each row. The north (N), east (E), anti-solar (−⊙) and velocity (v) directions are given in the panels to the left of the maps. Panels are left blank (black) in cases where there is no data. Background stars appear as aligned and sometimes elongated bright spots (e.g., 2022 October 20, B filter).
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Example of the image format used for visual inspection of our candidates. The detection shown in this figure is a synthetic source with an r-band magnitude of 27.0. The left panel is what we call an MCMC plot. The black teardrop-shaped region is the boundary of the space of possible KBO rates of motion. The gray region at slow rates represents the rate cut we made on our detections. The points are sampled from our MCMC, with colors corresponding to the S/N of the object in the stack (this object had a peak S/N of 8). Each point represents a targeted stack at the given rate. As a stack approaches the correct rate, causing the source to appear optimally point-like, the S/N increases in this characteristic manner. The inset labeled “Diff Coadd” is the stationary stack; the image shows no discernible signal. The inset labeled “Best Stack” is the stack at the best rate, as determined by the MCMC. In this image the KBO is quite apparent. The right panel shows a grid of stacks centered at the best rate, and offset in increments of 1 pixel hr–1 in R.A. rate and decl. rate.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: The DEEP “B1” TNO search fields used in this analysis. Each hexagonal shaded area represents the DECam focal plane with its 61 active CCDs. The B1a–c fields were observed with integrated exposure times of ∼3.5 hours in 2019 August (left), and reobserved at suitably shifted positions (not plotted) in 2019 September. In 2020 October we observed the B1a–f fields (center). In 2021 October we observed the B1b–f, h, and i fields. The larger areas in 2020 and 2021 account for diffusion of the 2019 detections. The plotted points represent our putative KBO detections. Note that Neptune is near the B1 fields, meaning that there should be relatively few resonant objects among our detections.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Rate vectors for all detections resulting from the forward (black) and reverse (red) shift-and-stack, prior to human vetting. There is a clear excess of detections in the forward shift-and-stack, corresponding to the Kuiper Belt.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Correlations between vetters’ votes on detections from the reverse stack (top left), implanted sources in the forward stack (top right), and candidate sources in the forward stack (bottom). The numbers in each square tabulate the number of times the square’s outcome occurred. Note that yes votes on sources from the reverse stack are not strongly correlated.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Sample grid for a 4 hr exposure sequence with 1″ seeing. The black teardrop-shaped boundary encompasses the space of possible bound orbits with topocentric distance between 35 and 1000 au. The red points are the sample rates computed using the procedure described above.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Number of sources resulting from the forward and reverse shift-and-stack as a function of S/N, both prior to human vetting, and after applying weights from human vetting and various cuts. It is clear that false positives drop off quickly with increasing S/N, and that our vetting procedure was highly effective at removing false positives.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Sky moving rates of our candidate detections. The size of each marker is proportional to its weight, as calculated by Equation (4). The dense cloud of points corresponds mostly to CC detections (see Section 8).
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Mosaic of DEEP B1 detections with weights ≥ 0.4.
Paper: The DECam Ecliptic Exploration Project (DEEP). V. The Absolute Magnitude Distribution of the Cold Classical Kuiper Belt
Authors: Kevin J. Napier, Hsing Wen Lin, 省 文 林, David W. Gerdes, Fred C. Adams, Anna M. Simpson, Matthew W. Porter, Katherine G. Weber, Larissa Markwardt, Gabriel Gowman, Hayden Smotherman, Pedro H. Bernardinelli, Mario Jurić, Andrew J. Connolly, J. Bryce Kalmbach, Stephen K. N. Portillo, David E. Trilling, Ryder Strauss, William J. Oldroyd, Chadwick A. Trujillo, Colin Orion Chandler, Matthew J. Holman, Hilke E. Schlichting, Andrew McNeill
Figure caption: Weighted distribution of the apparent magnitudes of our detections (where the weights are given by Equation (4)).
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: The loci of the boulders observed by J+23 on the plane of the sky on 2022 December 29 (red symbols) together with the model calculations of the boulder positions using the RK4 code with SPICE kernels for the current DRA version 5.20, with the input model parameters of Table 1 (black dots). North is up and east to the left.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Small dots: the loci of the modeled boulders on the sky plane on 2022 December 29 (see Figure 2) but sorted in different colors according to the initial ejection speed as described in Table 4. The large filled circles of different colors correspond to the measured boulder positions by J+23.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: The loci of the boulders computed by MERCURY (black dots) and RK4 codes (small red open circles) in the HEJ2000 X–Y and X–Z planes on 2022 December 29. The speed range was 0.09–0.7 m s−1.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Example of a boulder in close orbit after 800 days of integration time. The boulder radius is 3.8 m, and the ejection velocity is the Dimorphos escape velocity, 0.09 m s−1.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Example of an orbit of a boulder of radius of 7.2 m ejected at a speed of 0.128 m s−1 integrated over a period of 83 days since impact. The left panel represents the orbit projected to the X–Y HEJ2000 plane and the right panel to the X–Z plane.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Histogram of the position angles of the modeled boulders (see Figure 2, upper panel), showing maxima at ∼280° and ∼120° of position angle.
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Cross sections through the targets used in the SPH simulations, with different boulder packings: (a) 0 vol%, (b) 30 vol%, (c) 40 vol%, and (d) 50 vol %. In each panel the outlines show the three target sizes simulated: 87.90 × 86.96 × 57.16 m, 58.60 × 57.97 × 38.11 m, and 29.30 × 28.99 × 19.05 m. In all simulations the impact is vertical along the y-axis. (e) Boulder size–frequency distributions (SFDs) for each boulder packing studied here. The 20 vol% packing SFD is plotted for comparison. Due to resolution constraints, boulders smaller than ﹩{R}_{\min }﹩ = 2.5 m are not explicitly modeled; instead, they are included in the matrix material and treated as a continuum.
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Bern SPH simulations of collisions between a 87.90 × 86.96 × 57.16 m target and impactor of R  p  = 1.84 m (M  p  = 2.6×104 kg), with a relative velocity of 6 km s−1 and a vertical impact angle. Targets with four different packings (0–50 vol%) are investigated. Top row: cross section of SPH simulations showing the velocity field in the target at T = 1 s. Bottom row: SPH simulations showing the degree of disruption at T = 500 s and the size of the largest remnant (M lr).
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Specific impact energy required for a catastrophic disruption per unit mass, Q, as a function of target radius, R, for targets with different boulder packing (0 vol% to 50 vol%). (A) Vertical impact and (B) oblique, 45° impact. The impact location is the same for both impact angles (see Section 4). The DART impact energy is plotted in both A and B. Results from Benz & Asphaug (1999), Jutzi et al. (2010), and Raducan & Jutzi (2022) are plotted for comparison for the respective impact angle. ﹩{Q}_{D}^{* }﹩ curves used by Bottke et al. (2020) are impact-angle independent and are plotted in both A and B.
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: (a) Map of m-χ decomposition over the Haworth candidate landing site region formed by combining two orthorectified Mini-RF zoom mode (0.03 km resolution) collects. The white outline notes the boundaries of the Haworth candidate landing site. The image ranges from 86°S, 331°E (top left) to 88°S, 354°E (bottom right). North is up. Zoom-in of the region noted by the magenta box for (b) m-χ and (c) CPR. Magenta arrows point to the in-text referenced crater’s (86.°6S, 331.°9E) extended ejecta deposit. To reduce speckle noise, more obvious in zoomed-in images, a Gaussian smoothing filter was applied to the m-χ while the CPR image was box averaged with a 5 × 5 filter.
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: Zoom-in of a portion of the Haworth candidate landing site (region is to the right of the white line, which indicates a portion of the bounding box) noting illumination and slopes relevant for human exploration of the surface. Areas in yellow correspond to regions that are illuminated a large fraction of the year (>40%), areas in dark turquoise indicate where slopes are less than 5°, and green areas are where both conditions are met. Regions in dark blue indicate areas in permanent shadow (Mazarico et al. 2011). The background image is a hillshade map derived from LOLA data (Barker et al. 2023). The magenta arrow indicates the corresponding crater noted in Figure 8. North is up.
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: Controlled polar mosaic of Mini-RF S-band S 1 (i.e., total backscattered power) images in dB scale for areas poleward of 70°S in grayscale. Here, the grayscale map ranges from 1.5× the interquartile range below the lower quartile to 1.5× the interquartile range above the upper quartile and as such follows a box plot from the lower and upper whiskers. This removes the effects of outliers.
Paper: Pwyll and Manannán Craters as a Laboratory for Constraining Irradiation Timescales on Europa
Authors: M. Ryleigh Davis, Michael E. Brown
Figure caption: Sulfuric acid, salt, and water-ice concentration maps for Pwyll and Manannán craters. Panels (a) and (e) show the Galileo/SSI images of Pwyll crater, with the estimated sulfuric acid abundance from the corresponding NIMS cubes displayed in panels (b) and (f), the salt abundance in panels (c) and (g), and the water-ice abundance in panels (d) and (h). The crater rim is shown as the dashed circle, the extent of the dark proximal ejecta is indicated by the solid circle, and the bright white ejecta blanket is outlined in solid black. Likewise, panel (i) shows the SSI image of Manannán crater and the corresponding sulfuric acid, salt, and water-ice maps are shown in panels (j), (k), and (l), respectively. The extent of the dark ejecta is indicated by the solid circle, and the bright white ejecta blanket is outlined in black. The maps report the percent contribution of sulfuric acid, salts, or water to the best-fit linear spectral model for each NIMS pixel. Note the different scale bars between the Pwyll and Manannán maps. Both Pwyll and Manannán craters and their ejecta appear to be depleted in sulfuric acid relative to nearby older terrains, suggesting that the radiolytic sulfur cycle has not yet had enough time to reach an equilibrium concentration of H2SO4 at either crater. At both Pwyll and Manannán, the crater and dark proximal ejecta appear to be enriched in salts relative to the bright white ejecta blanket, suggesting that the dark material exhumed by the impacts is relatively salt-rich. The dark albedo and reddish coloration seen in the SSI images of both craters suggests that this salty material has already been irradiation reddened. As seen in panels (j) and (k), the nearby triple band, Belus linea, is significantly enhanced in salts and depleted in sulfuric acid relative to the background terrain.
Paper: Pwyll and Manannán Craters as a Laboratory for Constraining Irradiation Timescales on Europa
Authors: M. Ryleigh Davis, Michael E. Brown
Figure caption: Abundance values for the best-fit spectral models of the average spectra of specific geologic units in the Pwyll and Manannán regions. These abundance values and estimated 1σ error bars are reported in Table 2 and correspond to the models shown in color in Figures 3 and 4. At both Pwyll and Manannán, the average spectra of the crater, proximal ejecta, and bright ray ejecta are all depleted in sulfuric acid relative to the background terrain. The dark material in both of the craters and proximal ejecta contain a higher abundance of salts than the bright ray ejecta, although the background terrains appear to have the highest concentration of salty material. Manannán crater and the surrounding region shows a higher concentration of both salts and sulfuric acid, and therefore less pure water-ice than Pwyll.