adsabs/AstroCLIMB huggingface dataset:
Paper: A Convolutional Neural Network–Based Approach for Detecting Solar System Objects in Wide-field Imaging
Authors: Aram Lee, J. J. Kavelaars, Hossen Teimoorinia, Wesley Fraser, Edward Ashton
Figure caption: Detectability as a function of the rate of motion for bright objects with 22 < m < 23. Orange diamonds show recall as a function of the rate of motion, using image pairs with at least a 1 hr separation. Violet circles show recall as a function of rate of motion, using image pairs with 4–8 minutes of separation.
Paper: A Convolutional Neural Network–Based Approach for Detecting Solar System Objects in Wide-field Imaging
Authors: Aram Lee, J. J. Kavelaars, Hossen Teimoorinia, Wesley Fraser, Edward Ashton
Figure caption: Subimages containing artificial sources not detected by our process. Orange circles indicate the position of the artificial source. (Left) A bright stationary object (a star) in the background obscures the moving object. (Right) Bad columns on the detector prevent the detection of the moving object.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Interior scenarios consisting of homogeneous and heterogeneous morphologies and resulting impact craters over time. (a) Homogeneous target with a weak cohesion (Y0 = 1 Pa), an internal friction of f = 0.5, and a porosity of ϕ = 30%. (b) Heterogeneous strong interior involving multiple layers without boulders. The outer layer has a weak cohesion (Y0 = 1 Pa) and a porosity of ϕ = 50%. The midlayer and the core have a cohesion of Y0 =  50 and 500 Pa and a porosity of ϕ =  30% and 10%, respectively. The internal friction is set to f = 0.5 for all three layers. (c) Same as panel (b), but with multiple boulders (same boulder arrangement in Figure 8(c)). (d) Same as panel (c), but with a slight modification in the boulder arrangement. The upper central boulder is slightly shifted upward to the burial depth of z/rb = −0.5, while the lateral exposed boulder is positioned half-buried in the target. The color bar indicates the density map in units of kg m−3. The light-blue sphere above the asteroid at r = 0 m represents the DART projectile before the impact (t = 0 s). The boulders in dark and light blue correspond to low (10%) and high (75%) porosity, respectively. Note that the target asteroid is a half spheroid, but only the topmost portion is shown in this close-up.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Effects of interior morphologies consisting of double layers: a loose outer layer with cohesion of Y0 = 1 Pa (colored by light gray) and an underlying core formation at a cohesion of Y0 = 50 or Y0 = 500 Pa (colored by dark gray) modeled as half spheroids. The depth of the loose outer layer increases as follows: (a) h = 0, (b) h = 2, (c) h = 5, (d) h = 20, (e) h = rb = 87 m. Momentum enhancement factor β over h/a (f) until t ≤ 9 s and (g) at t = 30 s post-impact, for double-layer configurations with either strong (purple solid line and markers) or weak (blue solid line and markers) core formations. Note that in panel (f), as convergence is achieved earlier for the scenario with outer layer/strong core at h/a = 0, the β value is plotted at the convergence time, t = 9.5 s. The vertical orange shading highlights the layering-sensitive zone with h/a ≤ 7.7. The gray shading and gray solid line indicate the reference β range and its mean value from A. F. Cheng et al. (2023).
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The boulder arrangement involving (a) two central, (b) two central + two lateral subsurface, and (c) two central + two lateral subsurface + two lateral exposed boulders, and the evolution of the impact crater at t = 0, 0.5, 2, 10 s. The color bar indicates the density in units of kg m−3. The light-blue sphere above the asteroid at r = 0 m represents the DART projectile before impact (t = 0 s). Boulders in dark and light blue correspond to the low (10%) and high (75%) porosity, respectively. The regolith is assumed to have low cohesion (Y0 = 1 Pa), 30% porosity, and an internal friction of f = 0.5, similar to case 02 in Table 2. Note that the target asteroid is considered a half spheroid, but only the topmost portion is shown in this close-up.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The time evolution of the simulated momentum enhancement factor, β, from DART-scale impacts on a curved asteroid for (a–b) homogeneous interior. (c, d) Same for heterogeneous three-layered interior ϕ = {50%, 30%, 10%} and ϕ = {40%, 30%, 20%} with multiple boulders. The colored solid lines illustrate simulation results of various interior configurations, with layering and boulder arrangements based on the setups shown in Figure 11. The gray shading and black solid line indicate the reference DART impact β range and its mean value from A. F. Cheng et al. (2023). (e) Simulated β values relative to the bulk density of Dimorphos, marked by colored stars representing different porosity values at selected time frames after impact.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Effects of multiple lateral boulders near the impact site, based on the setups shown in Figure 8. The time evolution of the simulated (a) momentum enhancement factor, β, and (b) crater diameter up to t = 15 s after impact. The variation of the cumulative ejecta mass normalized by the projectile mass along with (c) the ejecta velocity, V, normalized by the impact velocity, U, and (d) the radial position normalized by the impactor radius, r/a, at t = 15 s post-impact.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The time evolution of the simulated (a) momentum enhancement, β, and (b) crater diameter, from head-on collisions on a curved asteroid. Colored solid lines depict the effect of varying numbers of centrally positioned subsurface boulders. The gray shading and black solid line indicate the reference DART impact β range and its mean value from A. F. Cheng et al. (2023). The variation of the cumulative ejecta mass normalized by the projectile mass along with (c) the ejecta velocity, V, normalized by the impact velocity, U, and (d) the radial position normalized by the impactor radius, r/a, at t = 15 s post-impact.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Illustration of a subsurface boulder positioned with lateral offset in the 2D axisymmetric configuration. R denotes the distance from the center of the lateral boulder, with a radius r to the symmetry axis. Blue spheres represent the lateral boulders, while the gray torus depicts boulders with a lateral offset.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Crater morphology at t = 60 s post-impact, from DART-scale impacts on a curved asteroid for (a) homogeneous interior with f = 0.5, Y0 = 1 Pa, ϕ = 30% (case 02) and (b) heterogeneous three-layered weak interior with multiple boulders (case 31). The color bar indicates the density map in units of kg m−3. Here the simulated diameters of impact craters are 63.9 and 65.1 m for case 02 (homogeneous interior) and case 31 (heterogeneous interior), respectively.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The normalized cumulative ejecta (a) mass–velocity and (b) mass–position at t = 20 ms post-impact for case 02 (see Table 2) to test the mesh dependency of simulation results with regridding functionality of the iSALE-2D model. The percentage relative difference in (c) the momentum enhancement factor, β, and (d) the crater diameter as a function of the model resolutions represented by CPPR.
Paper: Asteroids Fail to Retain Cometary Impact Signatures
Authors: Sarah Joiret, Guillaume Avice, Ludovic Ferrière, Zoë M. Leinhardt, Simon Lock, Alexandre Mechineau, Sean N. Raymond
Figure caption: The 134Xe/132Xe vs. 136Xe/132Xe diagram showing the composition of Tatahouine (#13349) and Shalka (#6766_C) measured at different heating steps, including those of T. Michel & O. Eugster (1994) and O. Eugster & T. Michel (1995) for comparison. The 238U and 244Pu fission Xe data are from D. Porcelli et al. (2002). Q-Xe (Q phase is the main carrier of heavy noble gases in chondrites) is from H. Busemann et al. (2000), SW-Xe (SW stands for solar wind) is from A. Meshik et al. (2020), U-Xe is from R. O. Pepin & D. Porcelli (2002), and Air (corresponding to Earth’s atmosphere) is from M. Ozima & F. A. Podosek (2001). Error bars are at 1σ.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: Data taken on Day 1 are shown on the left, and Day 2 is on the right. Each track is roughly 35 s in length. Time is encoded in color starting in purple at the beginning and ending in yellow at the end of the trace. Day 1 shows the path of the single bacterium that was in the field of view. The bacterium swims within a single, well-constrained vertical path, and in wide, sweeping arcs in the plane. It reverses direction during part of its swimming trajectory.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: The bacterial sampling team and small, gray Son of SHAMU DHM instrument are shown in the Boulby Mine on the left, and the instrument in operation by our coauthor, Dr. Scott Perl and his team, are shown on the left with him sampling in the Mars analog brine pool on the right. All brine samples were taken directly from subsurface brine pools with no sample manipulation done from extraction to optical analysis.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: The spaceflight instrument above illustrates the digital holographic microscope architecture for exploration of the icy moons of our solar system. This DHM instrument adopted many of core design choices of the field instrument described in this paper, including an entirely enclosed optical system, use of microfluidic sample chambers, use of a digital camera with small pixel size to reduce instrument size, and use of fold mirrors for packaging.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: Examples of a raw hologram (left) and numerically refocused frame (right) are illustrated above. The inset image shows the fringe pattern resulting from the interference of the object and reference beams.
Paper: Activity-induced Near-infrared Spectral Variability at 29P/Schwassmann–Wachmann 1, 2017–2022
Authors: Theodore Kareta, Charles A. Schambeau, Megan Firgard, Yanga R. Fernández
Figure caption: The four low-resolution near-infrared spectra of SW1 are shown as black open circles compared against the two classes of models described throughout Section 3, shown as solid colored lines. As before, the light gray regions indicate areas of significant telluric absorption. The models for the 2022 February 8 spectrum are those derived from fitting the data excluding the uncorrected telluric feature near ∼2.0 μm. The light blue models, labeled as “Hapke/Linear Mixing” models, assume large porous dust grains modeled by B. Hapke’s (2012) theory, while the single-sized ice grains are pure and described by Mie theory. The orange-red models, labeled as “Mie Scattering” models, assume a power-law distribution of dust grains and a single size for ice grains, both described by Mie theory. More details on the modeling are available in the text.
Paper: Activity-induced Near-infrared Spectral Variability at 29P/Schwassmann–Wachmann 1, 2017–2022
Authors: Theodore Kareta, Charles A. Schambeau, Megan Firgard, Yanga R. Fernández
Figure caption: Photometric measurements of SW1 are shown from the ATLAS forced photometry server and the BAA, corrected for heliocentric and geocentric distances but not for phase angle, relative to the dates on which we obtained near-infrared spectra of the comet. Observations with IRTF/SpeX are shown as black lines in each of the three epochs, and our LDT/NIHTS observations are shown as a light blue line in the bottom panel. The top panel corresponds to a large ∼4 mag outburst in 2017 August (actually two outbursts in rapid succession), the middle panel corresponds to a period of a minimum of brightness of the comet in 2020 October, and the bottom panel shows a pair of observations before and after a moderate ∼1.3 mag outburst in 2022 February.
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Left: Tara (red, 1), Powys (purple, 2), and northern low-latitude (cyan, 3) regional spectra and 1σ errors shown in Figure 1 compared to a ground-based, disk-integrated Infrared Telescope Facility (IRTF) SpeX spectrum of Europa’s leading hemisphere (black, 4, originally presented in R. Cartwright et al. 2023a) and a global spectrum collected by Galileo/NIMS (black, 5, originally reported in T. McCord et al. 1998a). These empirical data are compared to spectral models (gray) that utilize linear mixtures of 100 μm diameter grains of H2O ice measured at 120 K (R. Mastrapa et al. 2008, 2009) with the following fractional abundances: (a) 100% crystalline H2O ice, (b) 75% crystalline H2O ice and 25% amorphous H2O ice, (c) 50% crystalline H2O ice and 50% amorphous H2O ice, (d) 25% crystalline H2O ice and 75% amorphous H2O ice, and (e) 100% amorphous H2O ice (see Section 2.1 for more detail on our modeling procedures). All spectra are normalized to 1 at 1.77 μm and offset vertically for clarity. The dotted lines show the central wavelengths of Europa’s 1.5 and 1.65 μm H2O ice bands, a weak 1.69 μm shoulder feature possibly resulting from salts, a potential hydrated salt or crystalline ice feature near 1.78 μm, and the varying central wavelength for Europa’s 2.0 μm H2O ice band, shifting from 1.986 μm (Tara) to 1.992 μm (Powys and northern low latitudes). Right: the same data and models, focused on longer wavelengths. The dotted lines show the central wavelengths of Europa’s 3.1 μm H2O Fresnel peak and the large wavelength shift in its 3.6 μm H2O ice continuum peak, ranging from 3.63 μm in the northern low-latitudes spectrum, 3.69 μm in the Powys spectrum, and 3.71 μm in the Tara spectrum.
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Left: mosaic of Europa’s leading hemisphere, made with images collected by Galileo’s Solid State Imager, overlain by mapping of previously defined geologic features (E. J. Leonard et al. 2024). Black polygons show the locations of JWST/NIRSpec spaxels incorporated into the spectra shown on the right. Geologic units are defined in the legend below (utilizing a similar color scheme to E. J. Leonard et al. 2024). Right: JWST/NIRSpec regional spectra and 1σ uncertainties of Europa, representative of southern/central Tara Regio (red, 1), southern Powys Regio (purple, 2), and a northern low-latitude region dominated by ridges and bright terrains (cyan, 3). These spectra were generated by median combining the four spaxels in each polygon shown in the map on the left, normalized to 1 between 1.77 and 1.78 μm and offset vertically for clarity. The inset figure shows the same data, between 3 and 5.3 μm, normalized to 1 between 3.14 and 3.15 μm and offset vertically. Confirmed absorption bands associated with H2O ice, solid-state CO2, and H2O2, and the 3.1 μm H2O ice Fresnel peak and 3.6 μm H2O ice continuum peak are labeled (bold text). Spectral features that might include contributions from hydrated minerals, such as sulfates (S. De Angelis et al. 2021), chlorides (e.g., S. De Angelis et al. 2022), and carbonates (e.g., S. De Angelis et al. 2019), are labeled “salts?” (italic text). Central wavelengths (μm) for these confirmed and possible features are listed vertically along each dotted line. Constituents labeled in gray font are shown here for completeness but were not measured by this study. Subtle spectral features between 4.7 and 5.1 μm could be artifacts, but we did not analyze them in this study.
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Spectral maps illustrating the distribution in the band centers, depths, and areas for (top) Europa’s 4.25 μm lobe (4.2–4.3 μm), (middle) 4.27 μm lobe (4.2–4.3 μm), and (bottom) 4.38 μm band (4.37–4.39 μm), each attributed to solid-state CO2. †The band areas of the 4.25 and 4.27 μm lobes are convolved, and we therefore report the same area measurements for both features. The 1σ uncertainties for the spectral contrast measurements range between 0.10%–0.90%, 0.38%–1.90%, and 0.40%–1.36% for the 4.25 μm region, 4.27 μm band, and 4.38 μm band, respectively. The 1σ uncertainties for the area measurements are 0.03–0.07 and 0.01–0.03 μm for the convolved 4.25 and 4.27 μm lobes and the 4.38 μm band, respectively. Spaxels where the 4.38 μm band was not detected (>3σ) are shown in light gray. The spatial extents of large-scale geologic units on Europa’s leading and anti-Jovian sides, including Tara (10°S, 75°W) and Powys (0°, 145°W) Regiones, are indicated and described in the included legend (see E. J. Leonard et al. 2024).
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Spectral maps illustrating the distribution in the centers, heights, and areas for (top) Europa’s 3.1 μm H2O ice Fresnel region (2.9–3.3 μm), (middle) its 3.1 μm H2O ice Fresnel peak (3.05–3.15 μm), and (bottom) its 3.6 μm H2O ice continuum peak (3.3–4.0 μm). The 1σ uncertainties for the spectral contrast measurements range between 0.58%–1.78%, 0.70%–1.00%, and 0.011%–0.79% for the 3.1 μm Fresnel region, 3.1 μm Fresnel peak, and 3.6 μm continuum peak, respectively. The 1σ uncertainties for the area measurements are 0.080–0.094, 0.08–0.26, and 0.08–0.14 μm for Europa’s Fresnel region, 3.1 μm Fresnel peak, and the 3.6 μm continuum peak, respectively. Spaxels where the 3.1 μm Fresnel peak was not detected (>3σ) are shown in light gray. The spatial extents of large-scale geologic units on Europa’s leading and anti-Jovian sides, including Tara (10°S, 75°W) and Powys (0°, 145°W) Regiones, are indicated and described in the included legend (see E. J. Leonard et al. 2024).
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Spectral maps illustrating the distribution in the band centers, depths, and areas for (top) Europa’s 1.5 μm band (1.48–1.74 μm), (middle) its 1.65 μm band (1.62–1.68 μm), and (bottom) its 2.0 μm band (1.86–2.24 μm), each primarily attributed to H2O ice. The 1σ uncertainties for the spectral contrast measurements range between 0.37%–0.57%, 0.75%–1.11%, and 0.10%–1.00% for the 1.5, 1.65, and 2.0 μm bands, respectively. The 1σ uncertainties for the area measurements are 0.12–0.32, 0.11–0.21, and 0.08–0.88 μm for the 1.5, 1.65, and 2.0 μm bands, respectively. The spatial extents of large-scale geologic units on Europa’s leading and anti-Jovian sides, including Tara (10°S, 75°W) and Powys (0°, 145°W) Regiones, are indicated and described in the included legend (see E. J. Leonard et al. 2024).
Paper: A Convolutional Neural Network–Based Approach for Detecting Solar System Objects in Wide-field Imaging
Authors: Aram Lee, J. J. Kavelaars, Hossen Teimoorinia, Wesley Fraser, Edward Ashton
Figure caption: Subimage series examples accepted as detected SSOs. The images are arranged in sequential order, from left to right. Top row: A bright, elongated source moves from left to right across the subimage. Second row: A fainter elongated source moves from left to right across the subimage. Third row: A very vain elongated source moves from the lower left to the upper right. The fourth row: A very faint point-like source moves from the lower left to the center right. Faint moving objects, such as the one on the fourth row, are easier to spot when images are inspected as animations rather than separate images. Based on their rate of motion, these objects are likely asteroids.
Paper: A Convolutional Neural Network–Based Approach for Detecting Solar System Objects in Wide-field Imaging
Authors: Aram Lee, J. J. Kavelaars, Hossen Teimoorinia, Wesley Fraser, Edward Ashton
Figure caption: A subimage series accepted as a detected solar system object (not an artificial source). The time interval between each image is 248 s. The images are arranged sequentially, from left to right and top to bottom. This nonplanted candidate returned the highest score using our method. The pixel scale is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩185 pixel−1. Based on the observed rate of motion of ∼3﹩\mathop{.}\limits^{\unicode{x02033}}﹩3 hr−1 and the circumstances of the observation, this object is at a distance of ∼40 au and is a Centaur or a TNO.