adsabs/AstroCLIMB huggingface dataset:
Paper: Col-OSSOS: Evidence for a Compositional Gradient Inherited from the Protoplanetary Disk?
Authors: Michaël Marsset, Wesley C. Fraser, Megan E. Schwamb, Laura E. Buchanan, Rosemary E. Pike, Kathryn Volk, Nuno Peixinho, Susan Benecchi, Michele T. Bannister, Nicole J. Tan, J. J. Kavelaars
Figure caption: Spectral distribution of the TNO data set analyzed in this work, in parameter spaces of optical vs. NIR spectral slopes (left) and PC1 vs. PC2 values (right). The red line in the left panel corresponds to the one-to-one reddening line. The side histograms showing the distribution of spectral parameters highlight the bimodality of our data set in visible spectral slope and PC2. The dashed horizontal blue line in the right panel indicates the intersection of the two Gaussians fitted to the histogram of PC2 values, corresponding to the prime criteria used to classify our data set into the FaintIR and BrightIR classes. Objects close to that limit, with −0.14 < PC2 < −0.11, were conservatively considered as taxonomically ambiguous and were not included in our statistical analysis. See Section 2.2 for additional classification criteria of our data set.
Paper: Col-OSSOS: Evidence for a Compositional Gradient Inherited from the Protoplanetary Disk?
Authors: Michaël Marsset, Wesley C. Fraser, Megan E. Schwamb, Laura E. Buchanan, Rosemary E. Pike, Kathryn Volk, Nuno Peixinho, Susan Benecchi, Michele T. Bannister, Nicole J. Tan, J. J. Kavelaars
Figure caption: Left: absolute H-magnitude distribution of the complete TNO data set. The intervals indicated at the top correspond to the mean value of each orbital class, plus and minus the uncertainty on the mean. On average, FaintIR TNOs tend to be larger in our data set compared to BrightIR TNOs. This is an observational bias due to the fact that BrightIR TNOs tend to be located on dynamically more excited orbits with lower perihelion values than FaintIR TNOs (Figure 2). As such, smaller objects can be more easily detected from the Earth as they reach lower geocentric distances. Right: H-magnitude distribution of the subsample of objects with q > 35 au. Here, the average H value of the two classes is statistically similar.
Paper: Col-OSSOS: Evidence for a Compositional Gradient Inherited from the Protoplanetary Disk?
Authors: Michaël Marsset, Wesley C. Fraser, Megan E. Schwamb, Laura E. Buchanan, Rosemary E. Pike, Kathryn Volk, Nuno Peixinho, Susan Benecchi, Michele T. Bannister, Nicole J. Tan, J. J. Kavelaars
Figure caption: Orbital inclinations vs. optical spectral slope of individual dynamical subgroups. The legend is as in Figure 4. The left panel shows resonant populations located inward the classical belt, including the Plutinos (3:2), the 4:3, and one Neptune trojan (1:1). The middle panel shows objects occupying the classical belt and resonances within that region. The right panel shows the remaining objects located on large semimajor axes, including the scattering, detached, and resonators in high-order resonances, beyond 49 au.
Paper: Col-OSSOS: Evidence for a Compositional Gradient Inherited from the Protoplanetary Disk?
Authors: Michaël Marsset, Wesley C. Fraser, Megan E. Schwamb, Laura E. Buchanan, Rosemary E. Pike, Kathryn Volk, Nuno Peixinho, Susan Benecchi, Michele T. Bannister, Nicole J. Tan, J. J. Kavelaars
Figure caption: Orbital inclinations vs. optical spectral slope of the BrightIR class of TNOs, divided into individual surveys. The gray lines have the same meaning as in Figure 4. The trend of decreasing inclination values with increasing spectral slopes is found in all three data sets, whether or not cold classicals are included in the data set.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Ratio between aerodynamical and geometrical size. Particles with values smaller than 1 are slower than expected for their geometrical size. The dashed blue line represents aggregates with 50% porosity (50% of the aggregate volume is devoid of solid material). The black error bars represent the error caused by measurements of the geometrical size and the red error bars show the error for a + 5% shift in time.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Sedimentation velocity over geometrical size (measured particle diameter) of the 92 observed particles. The dashed blue line is the freefall velocity from the dust bed height. For small geometrical sizes, the measured sedimentation velocity varies by up to a factor of 5 between nearly same-sized particles, while it decreases for increasing geometrical sizes.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Ratios of the longest to smallest axes of particles from optical microscope images over surface equivalent diameter. The area between long axis-to-small axis ratios of 1 and 2 (highlighted in green) contains 86.6% of all particles, and the area between long axis-to-small axis ratios of 2 and 3 (highlighted in blue) contains 9.7% of all particles.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Sketch of the impact setup and acceleration unit (not to scale). (a) Experiment setup within the vacuum chamber in front view. The launcher is located behind the dust bed (not shown in the sketch). The brown lines schematically illustrate the sedimentation paths of the ejected particles. (b) Cross section of the launcher that launches saltators onto the dust bed.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: SEM images of captured particles. The black lines in the background are cracks in the adhesive coating. (a) A mostly intact aggregate of about 20–30 μm in diameter. Individual grains have sizes down to 1 μm and less. (b) An aggregate of about 100  μm that fragmented upon impact. (c) A monolithic particle of about 80 μm with a little micron-sized dust attached.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Histogram of the ratio of aerodynamical size to geometrical size for each particle mapped to the corresponding porosity.
Paper: Ejected Particles after Impact Splash on Mars: Aggregates and Aerodynamics
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, J. Merrison, G. Wurm
Figure caption: Compilation of all eight SEM images, with panels (a), (d), and (g) in the first row showing small aggregates, panels (b) and (e) in the second row showing what we think are aggregates shattered upon impact, and panels (c), (f), and (h) in the bottom row showing monolithic particles with clay-sized dust adhered to them.
Paper: Infrared Spectra and Vapor Pressures of Crystalline C2N2, with Comparisons to Crystalline HCN
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: The three strongest features in the mid-IR spectrum of crystalline C2N2 deposited and recorded at 100 K. Small peaks near 2148 and 2139 cm−1 are from 15NCCN and NC13CN, respectively. A weak, broad band near 820 cm−1 is from HCN. The ice thickness was 4.7 μm = 4.7 × 10−4 cm (channel fringes removed for clarity).
Paper: Infrared Spectra and Vapor Pressures of Crystalline C2N2, with Comparisons to Crystalline HCN
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: The three fundamental vibrational bands of crystalline HCN deposited and recorded at 120 K. The ice thickness was 0.47 μm = 0.47 × 10−4 cm (channel fringes removed for clarity); see also Gerakines et al. (2022).
Paper: Infrared Spectra and Vapor Pressures of Crystalline C2N2, with Comparisons to Crystalline HCN
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Vapor pressures of crystalline HCN and crystalline C2N2 from the literature. In the upper panel, six data points of Lewis & Schutz (1934) have been plotted, along with values at six temperatures from the vapor-pressure curve of Appleton & Van Hook (1982); see the text for sources of data for C2N2.
Paper: Infrared Spectra and Vapor Pressures of Crystalline C2N2, with Comparisons to Crystalline HCN
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Vapor pressures of crystalline HCN and crystalline C2N2 from the literature results and from the present work. The high- and low-temperature data in each panel are connected with a smooth curve, the Cox equation.
Paper: Infrared Spectra and Vapor Pressures of Crystalline C2N2, with Comparisons to Crystalline HCN
Authors: Reggie L. Hudson, Perry A. Gerakines
Figure caption: Optical constants for crystalline cyanogen at 100 K. The three regions are the same as in Figure 2.
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Comparison of the spectra of Jupiter irregular satellites Sinope and Pasiphae with laboratory spectra of carbonaceous chondrite meteorite Murchison samples prepared to different grain sizes, collected by Cloutis et al. (2018), which were digitized to display for the convenience of the reader. We note that the scale of the slope changes observed between these two members of the Pasiphae orbital family is consistent with the slope changes associated with grain size variation in laboratory samples, and therefore it cannot be assumed that compositional effects are the only mechanism to explain the spectral variation of these objects. The gray bars represent wavelength regions with significant telluric absorption features that cause increased scatter and sometimes introduce spectral artifacts in observations of faint objects.
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Top: spectrum of Neptune Trojan 2006 RJ103, with a linear fit to the spectral continuum along either side of the drop in reflectance detected near 0.7 μm. Each of a sequence of five wavelength bins appears inconsistent with this continuum at the ∼1σ–2σ level. As with our discussion of the spectrum of Sycorax, this feature is not dominated by a single wavelength bin or near an area with significant telluric contamination or the edge of the effective range of the red channel. Bottom: continuum-removed reflectance spectrum for Neptune Trojan 2006 RJ103. We note a drop in reflectance from ∼0.65 to 0.75 μm, with a minimum near 0.64 μm. We find the detection to be robust over a wide wavelength range. Absorption features in this wavelength region are often associated with Fe2+ charge transfer features in hydrated silicate materials.
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Comparison of Uranian satellites Sycorax (top) and Caliban (bottom) with laboratory spectra of CI chondrite Alais (Cloutis et al. 2011). While spectral variation in the laboratory spectra was found due to textural, packing, and phase angle effects, the spectral similarities between Alais and Sycorax suggest that CI-like material may be a relevant analog for objects in the Uranian system. Spectra are scaled to have the same average value from 0.5 to 0.8 μm.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Column-integrated mass of stratosphere HCN vapor (solid orange), HCN condensate (solid blue), total HCN (dashed green), and cumulative HCN condensate flux (dotted red) just above the tropopause (51 km). Gray lines and labels on the right mark (from bottom to top) the minimum HCN vapor column, minimum HCN column, maximum condensed HCN column, and net HCN precipitation at 51 km over 1 Titan yr. Vertical black dotted lines indicate L s = 24°, 30°, 36°, 45°, and 65°.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: (Upper) HCN precipitation flux at 51 km and (lower) cumulative 51 km HCN precipitation. Colors indicate ΔT, where blue is ΔT = 50 K, orange is ΔT = 40 K, and green is ΔT = 30 K. Line style indicates the flux and nucleation supersaturation, where solid is f = f 0, dashed is f = 0.1 × f 0, dashed–dotted is f = 10 × f 0, and dotted is f = f 0 with s nuc = 5%. Vertical black dotted lines indicate L s = 24°, 30°, 36°, 45°, and 65°.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Same as Figure 3 but for f = 0.1 × f 0.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Same as Figure 4 but for f = 0.1 × f 0.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: (a) Images with a phase angle of <70° used to study swirl area II shown in Figure 1. The black box denotes the total area examined, where black space indicates no coverage by the image in that portion of the study area. The range in reflectance for the region imaged is shown under the image ID. Photometric angle values across each image are listed in Table 1. (b) Images with phase angles between 70–90 used to study swirl area II shown in Figure 1. The black box denotes the total area examined, where black space indicates no coverage by the image in that portion of the study area. The range in reflectance for the region imaged is shown under the image ID. Photometric angle values across each image are listed in Table 1. (c) Images with phase angles > 90 used to study swirl area II shown in Figure 1. The black box denotes the total area examined, where black space indicates no coverage by the image in that portion of the study area. The range in reflectance for the region imaged is shown under the image ID. Photometric angle values across each image are listed in Table 1.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: The median values with standard deviations are plotted for the subareas shown in Figure 7. Off-swirl regions are plotted with blue circles, and on-swirl regions are plotted with red circles. There is a linear correlation (dotted line) between the single scattering albedo and phase function amplitude. There is no apparent correlation between the single scattering albedo and roughness parameter. The roughness parameter displays little variability within the errors across swirl area I.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: These images show subareas within swirl area I mapped on (upper left) image mosaic, (upper right) single scattering albedo, (lower left) phase function amplitude, and (lower right) roughness parameter. The subareas are divided into off-swirl (blue) and on-swirl (red) regions. The fifth off-swirl region is a line. The median values of the model parameters and their standard deviations are shown in Figure 8.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: Single particle scattering functions corresponding to the median phase function amplitude parameters for the subareas shown in Figures 7 and 8. The blue and teal lines represent off-swirl subareas (higher backscattering peak, lower forward scattering peak), and the red and orange lines represent on-swirl subareas (lower backscattering peak, higher forward scattering peak). The differences between the on- and off-swirl scattering functions are commensurate with those expected if off-swirl subareas contained a higher concentration of agglutinates, radiation-damaged material, or multimineralic grains.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: (Left) ADM values for swirl area II based on incidence angles on a gray scale of 0–0.35. (Right) ADM values for swirl area II (same as left panel), color coded to highlight regions of good (blue), moderate (green), and poor (red) data quality across the study area using the ADM metrics as applied to the incidence angle coverage. Good is defined as ADM values above 0.27, moderate as ADM values between 0.17 and 0.27, and poor as ADM values below 0.17.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: (Left) ADM values for swirl area I based on incidence angles on a gray scale of 0–0.61. (Right) ADM values for swirl area I (same as left panel), color coded to highlight regions of good (blue), moderate (green), and poor (red) data quality across the study area using the ADM metrics as applied to the incidence angle coverage. Good is defined as ADM values above 0.27, moderate as ADM values between 0.17 and 0.27, and poor as ADM values below 0.17.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: These images show the modeling values for the single scattering albedo (left), phase function amplitude (middle), and roughness parameter (right) for swirl area II. The range of values in the single scattering albedo image is 0.21–0.80, the phase function amplitude image is 0–0.95, and the roughness parameter image is 0°–30°. The images show different values for different regions within the data quality assessment (Figure 5).
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: These images show the modeling values for the single scattering albedo (left), phase function amplitude (middle), and roughness parameter (right) for swirl area I. The range of values in the single scattering albedo image is 0.15–0.45, the phase function amplitude image is −0.04 to 0.26, and the roughness parameter image is 0°–30°. The images display seams at boundaries with areas of different ADM values (Figure 4). The seams are most strongly seen in roughness parameter values.
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Difference between modeled and observed median rock abundance in each unit defined by Hiesinger et al. (2011). Negative values indicate units that are rockier than expected for their age.
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Median rock abundance (left) and H-parameter (right) in each unit defined by Hiesinger et al. (2011) vs. the model age of the unit. Gray bars indicate errors reported by Hiesinger et al. (2011). Red line indicates the best-fit linear relationship (Equation (1)).
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Mean (top left) and 95th percentile (bottom left) rock abundance, and mean (top right) and 95th percentile (bottom right) H-parameter all vs. unit age for all of the Hiesinger et al. (2011) units.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: The Didymos spectrum compared to the literature spectra of (433) Eros, (7) Iris (Vernazza et al. 2010), and (5407) 1992 AX (Marchis et al. 2012). Didymos’ behavior is at least qualitatively similar to these asteroids, and it has spectral behavior within the range seen in this population. The spectra of Didymos, Eros, and Iris are normalized to equal 1 near 9.3 μm, while that of 1992 AX is normalized to match Didymos’ spectrum near 14.5 μm.
Paper: Global Hall MHD Simulations of the Solar Wind Implantation Flux on the Lunar Surface
Authors: Lianghai Xie, Lei Li, Huizi Wang, Binbin Tang, Jindong Wang, Yiteng Zhang, Quanqi Shi, Bin Zhou, Yongyong Feng
Figure caption: Comparison between the global Hall MHD simulation and the observation. (a) 3D view of the simulation results, where the central sphere represents the lunar body with color contours, to show the relative number density to the solar wind density (N/N sw); the black dots show the trajectory of ARTEMIS P2 with magenta arrows, to indicate the velocity vectors extracted from the simulation results; the black circle on the lunar surface indicates the location of CE-4; and the gray lines show the streamlines of the solar wind. (b)–(e) Comparisons between the simulation results and the observations from ARTEMIS P2, in which the simulation results are shown as dashed lines, while the observation results are shown as solid lines: the lines with different colors indicate the results of different variables; the black dashed lines in (b) and (c) show the simulation results of the lunar wake with no crustal magnetic field; and the vertical magenta and gray dashed lines indicate the moments when the spacecraft encounters the shock and the magnetotail of the LMM, respectively. (f) Locations of ARTEMIS P2 in SSE coordinates, in which the red, green, and blue lines show the locations in the X-, Y-, and Z-directions, respectively, and the black line shows the altitude of ARTEMIS P2.