adsabs/AstroCLIMB huggingface dataset:
Paper: Experimental Constraints on Deliquescence of Calcium Perchlorate Mixed with a Mars Regolith Analog
Authors: Rachel A. Slank, Edgard G. Rivera-Valentín, Vincent F. Chevrier
Figure caption: Evidence of deliquescence after Experiment 9 was removed from the chamber and exposed to ambient conditions. (a) Sample directly after the experiment ended and being removed from the Mars simulation chamber. (b) After 5 minutes, regolith darkening started to occur, as seen by the darker color around some salt crystals on the lower left quarter of the petri dish. Of note, regolith darkening around the salt was not apparently associated with crystal size. It occurred for both large and small exposed salt crystals. (c) Here ∼80% of the surface salt had deliquesced and had regolith darkening around the salt crystal after 30 minutes. Of note, there was an apparent preference for the location of deliquescence. Salts with associated regolith darkening are primarily located in the lower left corner of the petri dish. We did not observe an association between the preference in the petri dish and location/orientation in the chamber (e.g., proximity to the buffer).
Paper: Experimental Constraints on Deliquescence of Calcium Perchlorate Mixed with a Mars Regolith Analog
Authors: Rachel A. Slank, Edgard G. Rivera-Valentín, Vincent F. Chevrier
Figure caption: Measured (a) mass, (b) relative humidity with respect to liquid, and (c) temperature change over time for Experiment 11. This experiment was run for 50 hr at 5°C, with a sample of 2 cm of JSC Mars-1 mixed with 5.3 wt% of calcium perchlorate. For panels (b) and (c), blue represents the upper atmosphere, red the lower atmosphere, green the humidity buffer, and orange the sample. The sample had the highest relative humidity in the chamber. However, all three locations followed the same trend with humidity. For most of the experiment the sample and upper atmosphere were at similar temperatures. The buffer was cooler, and the lower atmosphere had the lowest temperature remaining at almost a constant −12°C.
Paper: Experimental Constraints on Deliquescence of Calcium Perchlorate Mixed with a Mars Regolith Analog
Authors: Rachel A. Slank, Edgard G. Rivera-Valentín, Vincent F. Chevrier
Figure caption: Evidence of deliquescence after Experiment 11 was removed from the chamber and exposed to ambient conditions. (a) Sample directly after the experiment ended and after being removed from the Mars simulation chamber. (b) Visible regolith darkening was observed within 6 minutes of being exposed to ambient condition. The large salt grain circled in red is wet and covered in a layer of wet regolith. There are a few smaller spots of darkening in the middle of the sample. (c) Here ∼90% of the salt on the surface had deliquesced and had regolith darkening around the salt crystal after 45 minutes. Almost all the salt that did not have regolith darkening surrounding it was near the edge of the petri dish in the upper left quadrant.
Paper: Experimental Constraints on Deliquescence of Calcium Perchlorate Mixed with a Mars Regolith Analog
Authors: Rachel A. Slank, Edgard G. Rivera-Valentín, Vincent F. Chevrier
Figure caption: Measured (a) mass, (b) relative humidity with respect to liquid, and (c) temperature change over time for Experiment 9. This experiment was run for 7.5 hr at 4°C, with a sample of 2 cm of JSC Mars-1 mixed with 5.5 wt% calcium perchlorate. For panels (b) and (c), blue represents the upper atmosphere, red the lower atmosphere, green the humidity buffer, and orange the sample. The sample had the highest relative humidity in the chamber. However, all three locations followed the same trend with humidity. For most of the experiment the sample and upper atmosphere were at similar temperatures. The buffer was cooler, and the lower atmosphere had the lowest temperature remaining at almost a constant −12°C.
Paper: NASA’s Double Asteroid Redirection Test (DART): Mutual Orbital Period Change Due to Reshaping in the Near-Earth Binary Asteroid System (65803) Didymos
Authors: Ryota Nakano, Masatoshi Hirabayashi, Harrison F. Agrusa, Fabio Ferrari, Alex J. Meyer, Patrick Michel, Sabina D. Raducan, Paul Sánchez, Yun Zhang
Figure caption: (a) Nominal orbital element evolution over the first 3 days (∼six orbital periods) of the 180 day simulation. The blue, red, and yellow lines indicate F2BPFEM, GUBAS fourth, and GUBAS eighth results, respectively. (b) Angular position difference relative to GUBAS fourth.
Paper: NASA’s Double Asteroid Redirection Test (DART): Mutual Orbital Period Change Due to Reshaping in the Near-Earth Binary Asteroid System (65803) Didymos
Authors: Ryota Nakano, Masatoshi Hirabayashi, Harrison F. Agrusa, Fabio Ferrari, Alex J. Meyer, Patrick Michel, Sabina D. Raducan, Paul Sánchez, Yun Zhang
Figure caption: System with two arbitrary homogeneous rigid bodies.
Paper: Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid
Authors: John Weirich, Eric E. Palmer, Michael G. Daly, Olivier S. Barnouin, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Robert Gaskell, Dante S. Lauretta
Figure caption: Progress of optimized 3D rms deviation (left y-axis), FormU (left y-axis), and the ratio between them (right y-axis), through the simulated mission stages. Optimized 3D rms and FormU follow each other closely and are always within a factor of two. This shows that FormU (which can be measured in flight) is a close proxy for the optimized 3D rms error (which cannot be measured in flight). The tests show that overtiling (making higher-GSD maplets than the final DTM) improves the rms error of the model. We note a 37% improvement in rms for the “75 cm Model” when we create 35 cm GSD maplets with no additional data, and a further 8% improvement when we create 18 cm maplets for the 35 cm GSD model.
Paper: Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid
Authors: John Weirich, Eric E. Palmer, Michael G. Daly, Olivier S. Barnouin, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Robert Gaskell, Dante S. Lauretta
Figure caption: Top: the local radius from the truth model as a simple cylindrical projection. Sectors (a) and (c) represent rough truth model terrain with a medium density of craters and boulders, (b) represents smooth truth model terrain with a high density of craters and boulders, and (d) represents smooth truth model terrain with a low density of craters and boulders. Middle: the difference in radius from the CoF between the SPC model and the truth model, with the CoF drift removed. The maximum difference is 1.5 m, and in the majority of locations is less. Bottom: the radius difference from the middle panel displayed as a histogram.
Paper: Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid
Authors: John Weirich, Eric E. Palmer, Michael G. Daly, Olivier S. Barnouin, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Robert Gaskell, Dante S. Lauretta
Figure caption: The computer-generated synthetic asteroid (a.k.a. truth model) used for these tests is shown in (a) and (b), and the SPC model is shown in (c) and (d), both rendered with artificial lighting for clarity. The +y-axis points into the page in panels (a) and (c), and out of the page in panels (b) and (d). The overall shape of the SPC 35 cm model closely matches the truth model. Minor differences in the boulders, especially shape and height, can be seen. Additional processing of the boulders could have been performed, but was outside the scope of these tests.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Progress in the development of the Global DTMs of Bennu. (a) An image of Bennu collected by one of the OCAMS cameras. (b) Preliminary SPC Global DTM of Bennu. (c) Final SPC Global DTM of Bennu that was refined using higher-quality images collected while in close proximity to Bennu. (d) Final OLA Global DTM of Bennu (rendered without albedo). Panels (b)–(d) were rendered using the same image conditions present in the OCAMS image (panel (a)).
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Rocky terrain of the Nightingale sample collection site. (a) A mosaic of Nightingale and the surrounding area. (b) A close-up view of Nightingale, with the targeted sample site shown by a white circle. Both images are rotated so that Bennu's north is located at the bottom of the frame. Images were acquired by the OSIRIS-REx Camera Suite (OCAMS) PolyCam imager on 2020 March 3 (credit: NASA/Goddard/University of Arizona).
Paper: Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid
Authors: John Weirich, Eric E. Palmer, Michael G. Daly, Olivier S. Barnouin, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Robert Gaskell, Dante S. Lauretta
Figure caption: Top: the height difference between the truth model and local DTM of an arbitrary sampling site as a simple cylindrical projection. Topography is represented every 8 cm. The simulated image suite is ideal at 12 cm and sufficient at 5 cm. Bottom: the height difference from the top panel displayed as a histogram.
Paper: Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid
Authors: John Weirich, Eric E. Palmer, Michael G. Daly, Olivier S. Barnouin, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Robert Gaskell, Dante S. Lauretta
Figure caption: Albedo of the truth model, plotted as a simple cylindrical projection and scaled to an average albedo of 4%.
Paper: Quality Assessment of Stereophotoclinometry as a Shape Modeling Method Using a Synthetic Asteroid
Authors: John Weirich, Eric E. Palmer, Michael G. Daly, Olivier S. Barnouin, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Robert Gaskell, Dante S. Lauretta
Figure caption: The left panel shows the initial stages of a maplet-based SPC model before the topographic integration phase. The initial maplets poorly represent the topography. The right panel shows the final shape after the maplets have seamlessly flexed into the proper shape.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Example renderings for NFT Feature 11 on the asteroid wall. (a) Subsection of one of the test images containing the feature. (b) A rendering using the truth scan DTM with uniform relative albedo. (c) A rendering of the SPC feature model. The truth scan (panel (b)) is a 1.5 mm GSD scan taken by a tripod-mounted lidar. It has no albedo information; all shading comes from simulated sunlight. The SPC rendering (panel (c)) includes both terrain and albedo. Features defined from the truth model were located close to the SPC model but not necessarily at the exact location, which is why panel (b) is shifted slightly from panels (a) and (c).
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Asteroid wall and features used for testing. Yellow circles represent individual features tested, labeled with white feature ID numbers. The nine white points around the edges and in the center of the wall are the fiducials used to create a local wall coordinate frame during imaging.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Percent passing comparison for best-performing methods using strongest-performing features. Each line represents the percent of results that scored above the 0.6 correlation score threshold as a function of incidence angle. Results shown are for the five strongest-performing features, using the two control methods and the two best-performing methods. These results show that most features failed to meet the correlation score threshold for both albedo methods at low incidence angles.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: NFT Feature 11 correlation results from the SPC Asteroid Wall Test. “Scan” refers to correlation results generated using features rendered directly from the truth scan data (i.e., Figure 16(b)), while “SPC” refers to correlation results generated using SPC features (i.e., Figure 16(c)). All results were evaluated against the correlation score threshold of 0.6.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Features tested for the SPC Stress Test. These were generated from Shape 4 in the region where the truth model has terrain data at 1 cm pixel−1 GSD. The strong features (denoted by green boxes) have terrain that can be well modeled by the SPC software.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Comparison of correlation performance using different OLA scan configurations for a low-scoring feature from the OLA Thread Test. No relative albedo feature data were available for this test, so both NFT feature and truth image renderings used a uniform relative albedo.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Validated feature performance for SPC Thread Test Monte Carlo runs. (a) Minimum, maximum, and mean number of validated features per image, where at least three features were validated in every image on average. (b) Minimum, maximum, and mean pixel error of the validated features, where the mean pixel error was always less than the 6 pixel (3σ) requirement.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Example high-scoring OLA MLN from the OLA Thread Test. No relative albedo feature data were available for this test, so both the NFT feature and truth image renderings used a uniform relative albedo. The OLA feature models topography very well, with this feature having a resulting correlation score of 0.738.
Paper: Ground Testing of Digital Terrain Models to Prepare for OSIRIS-REx Autonomous Vision Navigation Using Natural Feature Tracking
Authors: C. E. Mario, C. J. Miller, C. D. Norman, E. E. Palmer, J. Weirich, O. S. Barnouin, M. G. Daly, J. A. Seabrook, D. A. Lorenz, R. D. Olds, R. Gaskell, B. J. Bos, B. Rizk, D. S. Lauretta
Figure caption: Simulated NFT TAG performance using SPC Thread Test features from processing images 1–11. Results show that SPC Thread Test features enabled NFT to meet the mission's original 25 m accuracy TAG requirement for all 258 Monte Carlo runs.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Error in the secular rates of NEOs as obtained by linear regression of the propagation using Laplace–Lagrange secular theory and compared to numerical integration of the three-body problem in percent. Secular rates in ascending node (left) and argument of perihelion (center) shown as a function of the initial conditions of semimajor axis and inclination. Secular rates in the angles as obtained with the two methods as a function of the initial semimajor axis (right). The dashed lines indicate the region in which we compute the average errors. This region includes the initial conditions used throughout the paper, indicated with crosses.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Chaotic dynamics of (35107) 1991 VH as obtained from numerical integration. Each axis represents the variation from the initial value of element pairs: semimajor axis–eccentricity (left), semimajor axis–inclination (middle), and argument of the node–argument of perihelion in degrees (right). The orbital evolution is shown at four instants of time: initial (first row), after 500 yr (second row), after 5000 yr (third row), and after 1 million years (bottom).
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Relative velocity at closest approach of flybys generated from the propagation of NEOs with semimajor axis smaller than 2 au for 50 yr. The symbol indicates the planet that the asteroid is encountering, and the horizontal axis shows respectively closest approach distance (au), inclination (deg), and eccentricity.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Logarithm of the errors in the computation of the final Keplerian elements given by pseudo-Öpik theory (PÖpik; first and second rows) and the quadrature of LPE (QLPE; third and fourth rows). The list of flybys used is shown in Figure 2 and generated as described in the text. The flybys are represented in the plane of relative velocity at closest approach V inf (km s−1) and distance of closest approach (au). The dashed area in the QLPE error plots separates the region in which the encounters are computed using an integration of the 3BP during the semi-analytical propagation.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Semi-equinoctial elements of the inner solar system planets obtained using three models. The analytical secular model derived is shown in blue, the integration of the 9BP of the main planets and the Sun is shown in red, and the ephemeris file DE431 is shown in gray. The initial conditions are obtained from the time average of the ephemeris file over the first orbital periods of the planets.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Top: potentially disruptive encounter time history in the most recent periods of close encounters of (35107) 1991 VH and (175706) 1996 FG3. In the most recent 50,000 yr, (35107) 1991 VH experiences Earth and Mars encounters. In the latest 10,000 yr, (175706) 1996 FG3 experiences Venus and Earth encounters. The close encounters below the line of mean variation in binary eccentricity of 0.1 are highlighted with a black circle, and the dashed line marks the radius of Earth. Bottom: probability of disruption based on the number of encounters found below thresholds of mean Δe = 0.1 for low disruption and Δe = 1 for high disruption. Confidence intervals on the probability of disruption prediction are shown with dashed lines.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Potentially disruptive encounters recorded by the 1000 virtual (35107) 1991 VH binaries during a million years into the past. The background contour represents the logarithm of the mean variation in binary eccentricity during a close encounter with a planet: Earth (blue, top) or Mars (red, bottom). The encounters found during the propagation in this threshold are shown by their closest approach distance (au) and V ∞ (km s−1). The radius of the planet is shown as a dashed line. The initial uncertainty distribution of (35107) 1991 VH is detailed in Appendix A.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Potentially disruptive encounters recorded by the 1000 virtual (175706) 1996 FG3 binaries during a million years into the past. The background contour represents the logarithm of the mean variation in binary eccentricity during a close encounter with a planet: Venus (green, top), Earth (blue, middle), or Mars (red, bottom). The encounters found during the propagation in this threshold are shown by their closest approach distance (au) and V ∞ (km s−1). The radius of the planet is shown as a dashed line. The initial uncertainty distribution of (175706) 1996 FG3 is detailed in Appendix A.
Paper: Semi-analytical Near-Earth Objects Propagation: The Orbit History of (35107) 1991 VH and (175706) 1996 FG3
Authors: Oscar Fuentes-Muñoz, Alex J. Meyer, Daniel J. Scheeres
Figure caption: Orbit history of (175706) 1996 FG3 in the past million years. Initial conditions are given in Table 2 as obtained from HORIZONS (Giorgini & JPL Solar System Dynamics 2021), and uncertainties in the distribution are obtained from JPL's SSD/CNEOS Small-Body DataBase (SSD/CNEOS API Service 2021) as described in Appendix A. Elements shown are perihelion distance, eccentricity, inclination, argument of the ascending node, argument of perihelion, and MOID with Venus, Earth, and Mars. Gray lines show individual simulations, and black lines are the median of the 1000 simulations of each parameter shown. Only 100 example runs and the median of the full distribution are shown in orbit elements (top two rows).