adsabs/AstroCLIMB huggingface dataset:
Paper: Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Samantha N. Hasler, L. C. Mayorga, William M. Grundy, Amy A. Simon, Susan D. Benecchi, Carly J. A. Howett, Silvia Protopapa, Heidi B. Hammel, Daniel D. Wenkert, S. Alan Stern, Kelsi N. Singer, Simon B. Porter, Pontus C. Brandt, Joel W. Parker, Anne J. Verbiscer, John R. Spencer
Figure caption: Expected and observed New Horizons (NH)/MVIC I/F compared with the E. Karkoschka (1998) (K98) geometric albedo spectrum scaled to a phase of α = 43.°9 and α = 53.°4 with a Lambertian phase function. Squares indicate the expected NH/MVIC values, calculated by convolving the 43.°9 albedo spectrum with the MVIC filters. NH/MVIC observations are plotted with circles (for the 2023 scans), diamonds (for the 2019 scan), and plus signs (for the 2010 scan). Horizontal lines indicate the bandwidth of the blue, red, NIR, and CH4 filters. The disk-averaged I/F data from the HST/WFC3 support imaging have also been scaled to a phase of 43.°9 with a Lambertian phase function and are shown here with triangles for comparison.
Paper: Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Samantha N. Hasler, L. C. Mayorga, William M. Grundy, Amy A. Simon, Susan D. Benecchi, Carly J. A. Howett, Silvia Protopapa, Heidi B. Hammel, Daniel D. Wenkert, S. Alan Stern, Kelsi N. Singer, Simon B. Porter, Pontus C. Brandt, Joel W. Parker, Anne J. Verbiscer, John R. Spencer
Figure caption: Sample image submissions from the ground-based community observer campaign. Some images were processed more than others, and some were submitted as series of nights. All images are presented in their native pixel orientation as submitted by observers. Observations were collected in both the optical and NIR from 12 to 16 inch diameter telescopes around the globe. A list of individuals who submitted images for this campaign and included their names in their submissions can be found in the Acknowledgments Section. Some images were received without being able to identify the observer, though observational details were provided. We are very grateful all who contributed.
Paper: Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Samantha N. Hasler, L. C. Mayorga, William M. Grundy, Amy A. Simon, Susan D. Benecchi, Carly J. A. Howett, Silvia Protopapa, Heidi B. Hammel, Daniel D. Wenkert, S. Alan Stern, Kelsi N. Singer, Simon B. Porter, Pontus C. Brandt, Joel W. Parker, Anne J. Verbiscer, John R. Spencer
Figure caption:  I/F as function of subobserver longitude for each of the MVIC filters. The 2023 data are indicated by circles, the 2019 data by diamonds, and the 2010 data by plus signs. Error bars are 1σ. In the case of nondetections (such as in the NIR and CH4 filters), we show a 1σ upper limit. I/F values are also listed in Table 1, along with observation details.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: (a) Reiner Gamma swirl region. On the left is the 2.8 μm OH band depth. On the right is a color-IR composite using RGB bands 66, 37, and 2. Where swirls are bright, OH is low. Note the many small craters that have punched through the OH-bearing top layer, exposing OH-poor material. North is up. (b) Reiner Gamma swirl region. On the left is the 2 μm Tetracorder fit times pyroxene band depth. On the right is a color-IR composite using RGB bands 66, 37, and 2. The lowest OH-bearing areas have higher pyroxene band depths. North is up. (c) Reiner Gamma swirl region. On the left is the 1.9 μm water band depth times fit image. On the right is a color-IR composite using RGB bands 66, 37, and 2. The lowest water-bearing areas correlate with swirl brightness, low OH, and higher pyroxene. The color of the water band depth image indicates a longer-wavelength position. Such positions correlate with hydrated sulfates, although not uniquely. North is up. (d) Reiner Gamma swirl region. On the left is the band depth times the fit of phyllosilicates, carbonates, and other minerals with absorptions in the 2–2.5 μm region. The area shows weak detection of absorption in the 2.2 μm region typical of smectites (montmorillonite group). The spectral resolution of M3 is not high enough to provide a definitive detection of the montmorillonite group minerals, but the detection shows the presence of a weak feature near 2.2 μm that is commonly in Al–OH-bearing phyllosilicates of the montmorillonite group. On the right is a color-IR composite using RGB bands 66, 37, and 2. The lowest smectite-bearing areas correlate with swirl brightness, low OH, and higher pyroxene. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: (a) Apollo 15 landing site region; M3 targeted mode data at 70 m pixel−1. Left to right are NIR apparent reflectance, 1 μm band depth characteristic of pyroxenes and olivines, 2 μm band depth characteristic of pyroxenes, and derived temperatures. The magenta lines represent the tracks by the lunar rover. The dark zones in the temperature image are where temperatures could not be derived from the M3 data due to strong absorption at 3 μm due to water. All band depth images here and in Figure 23(b) have had a nonlinear stretch applied according to Equation (1) and with a max brightness at band depth = 0.2 as shown in Figure 23(c). Image cube M3T20090705T160210. North is up (left in the rotated image on this page). (b) Apollo 15 landing site region; M3 targeted mode data at 70 m pixel−1. Left to right are NIR apparent reflectance, 2.8 μm OH band depth, and 3 μm water absorption. The magenta lines represent the tracks by the lunar rover. The Apollo 15 site is low in hydroxyl and water. The rover tracks did reach the base of the Apennine mountains, where trace water is indicated. North is up (left in the rotated image on this page). All band depth images here and in Figure 23(a) have had a nonlinear stretch applied according to Equation (1) and with a max brightness at band depth = 0.2 as shown in Figure 23(c). (c) The nonlinear intensity scale for the band depths in Figures 23(a) and (b). The equation of intensities is given in Equation (1), where a band depth of 0.2 is set to a maximum brightness of 255 in the 8 bit image range (0–255).
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: (a) Spectra of a pyroxene 1 μm band depth from a flat surface. Both the packed and fluffy surfaces show decreasing band depths with increasing incidence (zenith) angle. Emission angle = 0° to simulate a nadir-looking spacecraft. (b) Band depth for manufactured craters with rounded and flat bottoms of powdered basalt as a function of incidence (zenith) angle. The spectra were obtained of multiple craters in the field of view. In an imaging context, these would be subpixel craters. The image of round-bottomed craters is shown in Figure 24. Craters show decreasing band depth until very low incidence (zenith) angles when the lit high topography is small in area so that the signals from the filled-in shadow areas have a greater proportional signal. Emission angle = 0° to simulate a nadir-looking spacecraft. (c) Band depth for a manufactured large crater with a rounded bottom of powdered basalt as a function of incidence (zenith) angle. The field of view separated the lit from shadowed sides of the crater. In an imaging context, these results are for a resolved crater. Emission angle = 0° to simulate a nadir-looking spacecraft.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: (a) Region near 19°S, 119°E on the lunar farside and the Gerasimovich lunar swirls. (Left) NIR apparent reflectance. (Right) 2.8 μm OH map showing strange OH patterns. The classic region of the known swirls is at lower left, but weaker signatures in the OH map show similar patterns. Again, small craters have penetrated through the OH-rich regolith exposing OH-poor materials. Scale is 0.33 km pixel−1. North is up. (b) Closer view of the Gerasimovich swirls. On the left is the 2.8 μm OH band depth. On the right is a color-IR composite using RGB bands 66, 37, and 2. North is up. (c) Gerasimovich swirl region. On the left is the 2 μm pyroxene Tetracorder fit times band depth. On the right is a color-IR composite using RGB bands 66, 37, and 2. The lowest OH-bearing areas have higher pyroxene band depths. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Region near 4°S, 140°E on the lunar farside. (Top) NIR apparent reflectance. (Bottom) 2.8 μm OH map showing strange OH patterns. This area shows a higher development of diffuse OH patterns and diffuse crater rims than in Figure 18. As in the regions in Figures 17 and 18, small fresh craters have penetrated through the OH-rich regolith, exposing OH-poor materials. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Laboratory construction of a “cratered“ surface on powdered basalt and illuminated at an incidence (zenith) angle of 86° from the normal to illustrate how multiple reflections fill in shadowed areas in the bottoms of craters. The craters were created by pushing a test tube into the basalt. The test tube was ∼1.5 cm in diameter. Basalt powder was then sprinkled over the craters to create a fairy-castle regolith structure. The spectra of filled-in shadows will exhibit a reflectance squared spectrum, enhancing absorption bands.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Region near 22°S, 148°E on the lunar farside. (Top) NIR apparent reflectance. (Bottom) 2.8 μm OH map. Small fresh craters have penetrated through a surface layer of OH-rich regolith. The OH becomes more diffuse with time. This region shows more variation in OH signatures than the area shown in Figure 17. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Band depth vs. incidence (zenith) for an optically thick surface (black line) compared to a coating (red line). The kaolinite is on a powdered basalt flat surface (red line). Coatings show increasing band depth with increasing incidence angle. The emission angle = 0° to simulate a nadir-looking spacecraft.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: (a) Ingenii swirl area. This is a color-IR composite using RGB bands 66, 37, and 2. North is up. (b) Ingenii swirl area showing the 2.8 μm OH band depth. North is up. (c) Ingenii swirl area showing 2 μm Tetracorder fit times pyroxene band depth. North is up.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Context image of the south polar region of the Moon and CR1 and GR1. Locations of both CR1 on the Connecting Ridge and GR1 located on the de Gerlache crater rim are shown by the polygons and labeled in white. Elevation map (LOLA 5 m pixel−1) overlaid on hill shade derived from the LOLA elevation map.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Mapping features and density of craters at CR1. Base map is LOLA 5 m derived hill shade for (a)–(c). (a) NAC images across the CR1 region. (b) Boulders and craters mapped across the CR1 region. (c) Crater density map of CR1 with darker purple areas showing where there is the greatest density.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Topography at CR1. (a) Elevation map across the CR1 region LOLA 5 m pixel−1. (B) Slope map derived from the LOLA elevation map, 5 m pixel−1.
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: Io’s volcanic heat flow pre-Juno: the thermal emission as a function of longitude for 242 dark paterae, dark flows, and other volcanic features on Io as determined by Veeder et al. (2015). The long arrows indicate the longitudes of maximum heat flow predicted using an asthenospheric heating model (Segatz et al. 1988; Ross et al. 1990). The shorter arrows are the locations of secondary maxima. 30° bins are used. Loki Patera (not binned) is plotted to show its position and average thermal emission (9600 TW; Matson et al. 2006). The total thermal emission shown excludes outbursts. Figure from Davies et al. (2015). The data here compare well with a plot of longitudinal power output derived from Keck and Gemini telescope data (de Kleer & de Pater 2016a; see below).
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: Hot spot total power estimates (transient outburst eruptions are not plotted) in GW derived from nearly 30 yr of observations, including from the Juno spacecraft, overlaid on end-member models of interior heat flow (graphics from Matsuyama et al. 2022). Upper left: I—deep-mantle heating, favoring enhanced polar heating. Upper right: II—shallow, asthenospheric heating, with main heat flow located at sub- and anti-Jovian longitudes and equatorial to midlatitudes. Lower left: III—magma ocean model (Matsuyama et al. 2022), with peak heat flow offset eastward from the asthenospheric model. This Mollweide projection is centered on the anti-Jovian point (180°W). The Io reference image (lower right) is the Voyager–Galileo mosaic (Becker & Geissler 2005).
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: Orthographic projections of the volcano distribution and estimated total hot spot heat flow in Io’s northern hemisphere (left) and Io’s southern hemisphere. As a suitable heat flow model discriminator, 60° latitude is used to demarcate Io’s polar regions. This latitude was chosen because this was where the greatest changes in heat flow occurred when comparing models, and previous works used this latitude (Milazzo et al. 2005; Davies et al. 2024) to demark the polar boundary, allowing direct comparison of results.
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: Hot spot detections cataloged by Veeder et al. (2015) and mapped by Davies et al. (2015) are shown as white circles. Post-2015 detections, including JIRAM detections up to 2023 March (PJ49, inclusive), are shown as black circles. Portions of hot spots in other colors reflect probable changes of hot spot thermal emission location at a given volcano where the nearest pre-Juno hot spot thermal emission is preferentially used, in most cases where hot spot power is derived from Galileo NIMS spectra. A large cluster of post-2015 hot spots is found in the northern hemisphere at longitudes between 0°W and 60°W, a region poorly covered by Galileo.
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: Latitudinal distribution of volcanic thermal emission from 343 volcanic sources (up to and including JIRAM data obtained through orbit PJ49, 2023 March 1). This figure compares the new global hot spot list (incorporating Keck, Gemini, and JIRAM data analyses and the updated Veeder et al. 2015 hot spot power list using the values in Table 2) to the thermal emission curve published by Veeder et al. (2015). Most added thermal emission is at latitudes below 60°.
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: Longitudinal distribution of volcanic thermal emission from all sources. This figure compares the updated hot spot list incorporating recent AO and JIRAM detections with the updated Veeder et al. (2015) hot spot power list (Table 2) and the distribution mapped by de Kleer & de Pater (2016a) from observations from 2013 to 2015. All three analyses show broad agreement.
Paper: New Global Map of Io’s Volcanic Thermal Emission and Discovery of Hemispherical Dichotomies
Authors: Ashley Gerard Davies, Jason E. Perry, David A. Williams, Glenn J. Veeder, David M. Nelson
Figure caption: The updated Io volcanic thermal emission map, combining nearly 30 yr of observations. This Mollweide projection is centered on the anti-Jovian point (180°W). Some prominent volcanoes are labeled. North is up.
Paper: Ejected Particles after Impact Splash on Mars: Electrification
Authors: T. Becker, F. C. Onyeagusi, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Sketch of the setup with the capacitor consisting of two copper plates to the left and right of the dust bed. The capacitor is operated at a voltage of 5 kV and a distance of 5 cm. The forces acting upon a (charged) particle are shown with a blue (electrostatic Force) and red arrow (gravity), respectively, on an exemplary particle.
Paper: Ejected Particles after Impact Splash on Mars: Electrification
Authors: T. Becker, F. C. Onyeagusi, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Experiment setup, where (a)) shows the vacuum chamber with the first and second dust bed, electric field, and positioning of the light source and (b)) shows the launching mechanism for the primary impactors in detail. The inset at the top left of (b)) shows the filling of the launcher and the arrow indicates the movement of the plunger.
Paper: Ejected Particles after Impact Splash on Mars: Electrification
Authors: T. Becker, F. C. Onyeagusi, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Example trajectory of an ejected particle, viewed as a stack of the raw image data. The horizontal bend shows that the particle is charged and influenced by the electric field.
Paper: Ejected Particles after Impact Splash on Mars: Electrification
Authors: T. Becker, F. C. Onyeagusi, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Absolute charge (top) and charge density of ejected grains (middle). Bottom: binned data.
Paper: Geophysical Observations of the 2023 September 24 OSIRIS-REx Sample Return Capsule Reentry
Authors: Elizabeth A. Silber, Daniel C. Bowman, Chris G. Carr, David P. Eisenberg, Brian R. Elbing, Benjamin Fernando, Milton A. Garcés, Robert Haaser, Siddharth Krishnamoorthy, Charles A. Langston, Yasuhiro Nishikawa, Jeremy Webster, Jacob F. Anderson, Stephen Arrowsmith, Sonia Bazargan, Luke Beardslee, Brant Beck, Jordan W. Bishop, Philip Blom, Grant Bracht, David L. Chichester, Anthony Christe, Jacob Clarke, Kenneth Cummins, James Cutts, Lisa Danielson, Carly Donahue, Kenneth Eack, Michael Fleigle, Douglas Fox, Ashish Goel, David Green, Yuta Hasumi, Chris Hayward, Dan Hicks, Jay Hix, Stephen Horton, Emalee Hough, David P. Huber, Madeline A. Hunt, Jennifer Inman, S. M. Ariful Islam, Jacob Izraelevitz, Jamey D. Jacob, James Johnson, Real J. KC, Attila Komjathy, Eric Lam, Justin LaPierre, Kevin Lewis, Richard D. Lewis, Patrick Liu, Léo Martire, Meaghan McCleary, Elisa A. McGhee, Ipsita Mitra, Amitabh Nag, Luis Ocampo Giraldo, Karen Pearson, Mathieu Plaisir, Sarah K. Popenhagen, Hamid Rassoul, Miro Ronac Giannone, Mirza Samnani, Nicholas Schmerr, Kate Spillman, Girish Srinivas, Samuel K. Takazawa, Alex Tempert, Reagan Turley, Cory Van Beek, Loïc Viens, Owen A. Walsh, Nathan Weinstein, Robert White, Brian Williams, Trevor C. Wilson, Shirin Wyckoff, Masa-yuki Yamamoto, Zachary Yap, Tyler Yoshiyama, Cleat Zeiler
Figure caption: Representative examples of infrasound and seismic sensors and their field installations. (a) Gem Infrasound logger developed by BSU (photo credit: J. Anderson); (b) infrasound installation (LANL; photo credit: C. Carr); (c) INF04 infrasound sensor (KUT; photo credit: Y. Nikishawa); (d) Sapphire infrasound sensor (SMU; photo credit: E. Silber); (e) TDA’s infrasound sensor (photo credit: D. Eisenberg); (f) Infrasound and seismic instruments (UM; photo credit: S. Bazargan).