adsabs/AstroCLIMB huggingface dataset:
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Axis ratio (a/b) vs. absolute magnitude (left) and rotational period (right). The same legend as Figure 20 has been used. Orange and black lines are linear fits to the entire sample (full and partial lightcurves) and to the full lightcurves only, respectively.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Distribution of absolute magnitudes (H) and diameters for the NEOs included in the photometric study. Diameters were calculated from the absolute magnitudes and the mean geometric albedo of the photometric sample (P  V  = 0.25).
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: NIR spectra of NEOs included in the spectroscopic study.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Full lightcurves of NEOs included in the photometric study. The highest peak of the Lomb periodogram is the single-peaked rotational period with the highest confidence level. The 99.9% confidence level is indicated with a solid line, while the confidence level at 99% is the dotted line, and the dashed line corresponds to a confidence level of 90%. On the right, the lightcurves corresponding to the highest confidence level peak are plotted. The lightcurves have been fitted with a Fourier series fit (black curves).
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Maps showing the likely damage swath due to the hypothetical impact of 2023 DZ2 for Epoch 1 (top panel) and Epoch 2 (bottom panel). In both panels, a subset of the possible results is shown along the impact corridor. For the subset of points, yellow represents a serious damage level, dark yellow represents a severe damage level, orange represents a critical damage level, and dark red represents an unsurvivable damage level.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Collage of delay-Doppler images of 2023 DZ2 obtained on March 25 using the DSS-14 antenna at Goldstone to transmit and DSS-13 to receive. In each panel, time delay (range) increases downward and Doppler frequency increases to the right, so rotation is counterclockwise. Each row corresponds to 3.75 m (0.025 msec). The resolution in Doppler frequency is 1.0 Hz. Each image is an integration spanning 10 s and corresponds to about 10° of rotation.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: The affected population risks for Epoch 1 (top panel) and Epoch 2 (bottom panel). The most likely cause of damage remains the blast, but 86% of the cases result in no damage given the small diameter of 2023 DZ2.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Monostatic echo power spectrum of 2023 DZ2 obtained at Goldstone on March 27. The resolution is 1.0 Hz, and the figure shows a weighted sum of 59 runs using JPL/Horizons solution 14. Notation is the same as in earlier figures.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Examination of the Reiner Gamma swirl and the study area based on the Clementine mission camera measurements. The white box, centered at 7.11°N and 301.18°E, in each panel identifies the study area, contour lines show approximate boundaries between on- and off-swirl based on albedo in Panel (A). Panel (A) displays the LROC image mosaic extracted from the LROC Quickmap. Panel (B) displays the Clementine color ratio (red channel represents 750 nm/415 nm ratio, green channel represents 750 nm/950 nm ratio, blue channel represents 415 nm/750 nm ratio). Panel (C) displays the FeO abundance, scale bar below the panel, and Panel (D) denotes the OMAT values as derived from the Clementine 750 and 950 nm band images (Lucey et al. 2000a, 2000b), with the scale bar below the panel. All maps are from the LROC Quickmap.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Reiner Gamma swirl study area (left) is centered at 7.11°N and 301.18°E. The image on the right displays the center “eye” region of the Reiner Gamma swirl. The box on the left shows the region examined by Weirich et al. (2023) for elevation and examined in this study for photometrically derived surface properties.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Examination of the Reiner Gamma swirl and the study area based on the M3 observations (Clark et al. 2024). The region outlined by the white square box (centered at 7.11°N and 301.18°E) in all panels corresponds to the region shown in Figure 3(A) and the contour lines within the white box show approximate boundaries between on- and off-swirl based on albedo in Panel (A) in Figure 3. Panels (A) and (B) map the OH and H2O abundance, respectively, and Panel (C) maps the pyroxene abundance each as described by Clark et al. (2024).
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Distributions of the number of data points (brighter indicates more data) across the surface of the study region in the near-opposition regime (left), backward-scattering regime (center), and forward-scattering regime (right). The range of data counts are 188–700, 68–1700, and 0–100 in the near-opposition, backward-scattering, and forward-scattering regimes, respectively. The gray scales correspond to the data count ranges, with black the lowest and white the highest. In the case of the forward-scattering regime coverage the number of data points is nearly binary, with black representing zero counts and the gray and white ranging from ∼95 to 100 points. The region shown corresponds to the region delineated by the white box in Figures 1 and 3–5, centered at 7.12°N and 301.18°E.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Examination of the Reiner Gamma swirl and the study area based on the Kaguya Multiband Imager reflectance observations. The white box, centered at 7.11°N and 301.18°E, in each panel identifies the study area, contour lines show approximate boundaries between on- and off-swirl based on albedo in Panel (A) in Figure 3. Panels (A) and (B) display the plagioclase and olivine weight abundances, respectively (Lemelin et al. 2019). Panel (C) displays the FeO weight abundance (Lemelin et al. 2019). Panels (D) and (E) display the orthopyroxene and clinopyroxene weight abundances, respectively (Lemelin et al. 2019). All maps were extracted from the LROC Quickmap.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Spatially coregistered LROC NAC images (image numbers in red) covering the study region (shown in Figure 1) and used in the photometric analyses (this study) and topographic study of Weirich et al. (2023). The spatial coregistration results in the same location in each image corresponding to the same physical location on the lunar surface.
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: The DoLP observations of the Didymos system in B and R filters, and the fitted trigonometric DoLP phase curve model. The dependence is plotted as a function of phase angle (top row) and time (bottom row), expressed in days after the DART impact. The pre- and post-impact data have been fitted with separate models.
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: Examples of observed DoLP for the Didymos system with S- and C-type asteroids from the Catalogue of Asteroid Polarization Curves (left) and with two size fractions of olivine particles from the Amsterdam-Granada Light Scattering Database (right).
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: Timeline of the VLT and NOT polarimetric observations of the Didymos system starting on 2022 August 19 and ending on 2023 January 19.
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: Eight example particle shapes from a random Voronoi polyhedral model.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Distributions of data coverage displaying the percent of angular bins with data across the study region, with lower to higher values represented by darker to lighter colors, respectively. Top row is the near-opposition regime (minimum to maximum percentage values are 3.3–67.8 for incidence, 4.4–68.9 for emission, and 13.3–40 for phase). Central row is the backward-scattering regime (minimum to maximum percentage values are 22.2–100 for incidence, 22.2–66.7 for emission, and 35.7–71.4 for phase). Bottom row is the forward-scattering regime (minimum to maximum percentage values are 0–38.9 for incidence, 0–44.4 for emission, and 0–5.6 for phase). Left column is incidence angle coverage, central column is emission angle coverage, and right column is phase angle coverage. The gray scales correspond to the data count ranges, with black the lowest and white the highest. In the case of the forward-scattering phase angle coverage the number of data points is nearly binary, with black representing zero percent and white representing 5.6%. The region shown corresponds to the region delineated by the white box in Figures 1 and 3–5, centered at 7.12°N and 301.18°E.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Hapke parameter maps of the study area. The single-scattering albedo (top left) displays values of 0.11 to 0.35, the surface roughness (top right) displays values of 0.01 to 40, the phase function amplitude (bottom left) displays values of 0.096 to 0.476, and the phase function partition (bottom right) displays values of −0.447 to 0.922. Note the high similarity in patterns in the amplitude and partition parameters, reflecting the hockey-stick relationship. The region shown corresponds to the region delineated by the white box in Figures 1 and 3–5, centered at 7.12°N and 301.18°E.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: The Hapke parameters mapped on a blue (low) to red (high) value scale overlaid with the swirl units determined by Chuang et al. (2021). The results are shown in pairs, with the K-means results on top and the MLC shown on bottom. From top to bottom, the maps are of the single-scattering albedo, surface roughness, phase function amplitude, and phase function partition parameters. On-swirl areas are mapped by a clear outline, the diffuse-swirl is mapped by a dotted pattern, and the off-swirl is mapped by a diagonal stripe. White areas indicate where craters were removed from the data set. The region shown corresponds to the region delineated by the white box in Figures 1 and 3–5, centered at 7.12°N and 301.18°E.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Comparison of single-particle scattering functions for the three swirl units, on-swirl (light-colored, yellow-toned solid lines), diffuse-swirl (blue-toned dashed lines), and off-swirl (gray-toned solid lines). The locations from which the values are extracted are marked in the color map with black “x”s denoting on-swirl, red “x”s denoting diffuse-swirl, and white “x”s denoting off-swirl. The region shown corresponds to the region delineated by the white box in Figures 1 and 3–5, centered at 7.12°N and 301.18°E.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: The surface roughness, single-scattering albedo, and phase function amplitude, mapped in the RGB color system, respectively. Colors correlate with the swirl units identified by Chuang et al. (2021) for this study region. The region shown corresponds to the region delineated by the white box in Figures 1 and 3–5, centered at 7.12°N and 301.18°E.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Hapke parameter maps compared to LROC NAC image M145205753L (top left) for the use of a single-term (c = 0) particle scattering function. The single-scattering albedo (top right) displays values from 0 to 0.36, the phase function amplitude (bottom left) displays values from 0.015 to 0.442, and the surface roughness (bottom right) displays values from 0° to 40°.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Example single-particle scattering functions for on-swirl (top), diffuse-swirl (center), and off-swirl (bottom) units within the study region. The locations corresponding to the scattering functions are shown in the color figure in the left column.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: The color map from the hockey-stick solution. Locations for examination of Bayesian solutions (shown in B2–B4) are marked by black “x”s for on-swirl locations, white “x”s for diffuse-swirl locations, and gray “x”s for off-swirl locations.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Bayesian solutions for the locations that fall within the off-swirl units masked area in the Chuang et al. (2021) maps. Values shown in red correspond to parameters that provide the lowest RMSE between the model and data. The values displayed in black are the convergent solution with the standard deviation errors.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Bayesian solutions for the locations that fall within the on-swirl units. Values shown in red correspond to parameters that provide the lowest RMSE between the model and data. The values displayed in black are the convergent solution with the standard deviation errors.
Paper: Photometric Properties within the Reiner Gamma Swirl: Constraining Formation Mechanisms
Authors: Deborah Domingue, John Weirich, Frank Chuang, Samuel Courville, Roger Clark, Amanda Sickafoose, Eric Palmer, Robert Gaskell
Figure caption: Bayesian solutions for the locations that fall within the diffuse-swirl units. Values shown in red correspond to parameters that provide the lowest RMSE between the model and data. The values displayed in black are the convergent solution with the standard deviation errors.
Paper: New Polarimetric Data for the Galilean Satellites: Io and Ganymede Observations and Modeling
Authors: Nikolai Kiselev, Vera Rosenbush, Ari Leppälä, Karri Muinonen, Ludmilla Kolokolova, Aleksandr Savushkin, Nikolai Karpov
Figure caption: Single-scatterer P 11 element modeled identically for all the moons (on the left). The single-scatterer −P 12/P 11 element (on the right) depicts the one used for the modeling of Io (red line) and the one used for both Europa and Ganymede (blue line).