adsabs/AstroCLIMB huggingface dataset:
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: Images used for latitudinal scans in the F395N filter. All images are scaled over the same brightness range; the 2010 June image shows saturation near the center.
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: F395N brightness scans (left) and Lomb–Scargle periodogram (right).
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: Images used for latitudinal scans in the F275W filter. All images are scaled over the same brightness range.
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: Images used for latitudinal scans in the F631N filter. All images are scaled over the same brightness range.
Paper: Brightness Behavior of Distant Oort Cloud Comets
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Tim Lister, Quanzhi Ye, 泉志 叶, Colin Snodgrass, Cyrielle Opitom, Rosita Kokotanekova, Megan E. Schwamb, Matthew M. Dobson, Michele T. Bannister, Marco Micheli, Stefanie N. Milam, Derek C. Richardson, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: The activity indices for the sample vs. heliocentric distance, where each color is an individual comet with multiple n values. The error bars show the range of heliocentric distance (horizontal) and the 1σ error on the activity index (vertical). Circular markers are returning comets, while the plus signs are DNCs. The activity index is observed to decrease (flatten) with decreasing heliocentric distance for individual comets and the entire sample. The trend is highlighted using a gray shaded region between n = r h + 1.25 and n = r h − 3. Two objects that do not fall into this trend are C/2019 L3 and C/2022 A2, which experienced a “surge” in brightness near perihelion. These comets (as well as C/2023 A3) are outside of the gray shaded region preperihelion.
Paper: Brightness Behavior of Distant Oort Cloud Comets
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Tim Lister, Quanzhi Ye, 泉志 叶, Colin Snodgrass, Cyrielle Opitom, Rosita Kokotanekova, Megan E. Schwamb, Matthew M. Dobson, Michele T. Bannister, Marco Micheli, Stefanie N. Milam, Derek C. Richardson, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: The bottom figure shows the distribution of 1/a 0 values of our sample from two different sources, Nakano Note (orange) and MPC (green), which we compared to results for all comets from the CODE Catalog (P. A. Dybczyński & M. Królikowska 2016; top). The distributions are presented as a kernel density estimate plot. Rather than using discrete bins, a kernel density estimate plot smooths the measurements with a Gaussian kernel, producing a continuous probability density estimate. The lines at the bottom of the figure represent the individual values that make up the kernel density estimate and are present for all future kernel density estimate figures. The data points are weighted by their 1σ uncertainty, and the kernel bandwidth is selected according to Scott’s rule (D. W. Scott 1992). The Nakano Note distribution is more similar to the distribution from P. A. Dybczyński & M. Królikowska (2016), with nearly all of the objects having 1/a 0 > 0 compared to the MPC distribution.
Paper: Brightness Behavior of Distant Oort Cloud Comets
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Tim Lister, Quanzhi Ye, 泉志 叶, Colin Snodgrass, Cyrielle Opitom, Rosita Kokotanekova, Megan E. Schwamb, Matthew M. Dobson, Michele T. Bannister, Marco Micheli, Stefanie N. Milam, Derek C. Richardson, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: Lightcurves for six objects. For each comet, the upper panel(s) show the variation of ﹩m{{\prime} }_{\mathrm{helio}}﹩ with heliocentric distance using a 5″ aperture. The red squares represent the r magnitudes, and the green circles represent the g magnitudes shifted by the g − r color, which is listed in Table 3. The solid lines represent the best-fit activity index n to the r and scaled g magnitudes for each section, determined by the least-squares method. The bottom panel(s) show the residuals of the fit, and the shaded region is the median 2σ magnitude error. Perihelion is the vertical line separating preperihelion (left panels) and postperihelion (right panels), and the x-axis is in log scale.
Paper: Brightness Behavior of Distant Oort Cloud Comets
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Tim Lister, Quanzhi Ye, 泉志 叶, Colin Snodgrass, Cyrielle Opitom, Rosita Kokotanekova, Megan E. Schwamb, Matthew M. Dobson, Michele T. Bannister, Marco Micheli, Stefanie N. Milam, Derek C. Richardson, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: A visualization of the heliocentric range of observations for each comet discussed in this paper. Each black point represents one visit. The shaded regions show the preperihelion range (gray) and postperihelion range (blue), where the yellow stars are the perihelion distance for each comet. The asterisks represent comets that disintegrated. Observations are continuing for all nondisintegrated comets.
Paper: Brightness Behavior of Distant Oort Cloud Comets
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Tim Lister, Quanzhi Ye, 泉志 叶, Colin Snodgrass, Cyrielle Opitom, Rosita Kokotanekova, Megan E. Schwamb, Matthew M. Dobson, Michele T. Bannister, Marco Micheli, Stefanie N. Milam, Derek C. Richardson, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: Lightcurves for seven objects as described in Figure 3.
Paper: Brightness Behavior of Distant Oort Cloud Comets
Authors: Carrie E. Holt, Matthew M. Knight, Michael S. P. Kelley, Tim Lister, Quanzhi Ye, 泉志 叶, Colin Snodgrass, Cyrielle Opitom, Rosita Kokotanekova, Megan E. Schwamb, Matthew M. Dobson, Michele T. Bannister, Marco Micheli, Stefanie N. Milam, Derek C. Richardson, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: Lightcurves for eight objects as described in Figure 3.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption:                         (a). EMIT scene emit20220831t171631_o24311_s000_l2a_rfl_b0106_v01 Tetracorder color map for Fe2+- and Fe3+-bearing mineral electronic absorptions in the visible to very near-infrared spectral range. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene over Chile. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce this image, and others in Figures 12(b)–(d). (b). EMIT scene emit20220831t171631_o24311_s000_l2a_rfl_b0106_v01 Tetracorder color map for vibrational absorptions in the near-infrared region. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene over Chile. This is a Tetracorder standard product with expert system 5.27e1. (c). EMIT scene emit20220831t171631_o24311_s000_l2a_rfl_b0106_v01 Tetracorder color map for the eight EMIT minerals (excluding hematite and goethite): calcite, chlorite/serpentine, dolomite, gypsum, illite/muscovite, kaolinite-dioctahedral group, montmorillonite group, and vermiculite. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene over Chile. This is a Tetracorder standard product with expert system 5.27e1. (d). EMIT scene emit20220831t171631_o24311_s000_l2a_rfl_b0106_v01 Tetracorder color map for aluminum content in the octahedral layer in muscovite/illite. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene over Chile. This is a Tetracorder standard product with expert system 5.27e1.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: (a). EMIT scene emit20220814t223444_o22615_s000_l2a_rfl_b0106_v01 Tetracorder color map showing vegetation, snow and melting snow, and water sediments and another contaminants. Each of these is a combination of images showing finer detail. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene on the US California–Nevada border. North is to the upper right. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce this image and others in panels (b)–(d). (b). EMIT scene emit20220814t223444_o22615_s000_l2a_rfl_b0106_v01 Tetracorder color map showing vegetation spectral type. The spectral type was determined using the shape of the chlorophyll absorption like that shown in Figure 9(b). The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene on the US California–Nevada border. North is to the upper right. This is a Tetracorder standard product with expert system 5.27e1. (c). EMIT scene emit20220814t223444_o22615_s000_l2a_rfl_b0106_v01 Tetracorder color map showing the chlorophyll absorption edge position near 0.7 μm relative to the position of a green lawn grass. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene on the US California–Nevada border. North is to the upper right. This is a Tetracorder standard product with expert system 5.27e1. (d). EMIT scene emit20220814t223444_o22615_s000_l2a_rfl_b0106_v01 Tetracorder color map showing relative strengths of the water absorptions in vegetation in the RGB composite image. Blue areas have relatively weak 0.9 and 1.2 μm water absorptions and thus less water. White areas have three absorptions strong and thus higher water content. The EMIT swath width is approximately 77 km, in this non-ortho-corrected scene on the US California–Nevada border. North is to the upper right. This is a Tetracorder standard product with expert system 5.27e1.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: EMIT scene emit20220912t154138_o25510_s001_l2a_rfl_b0106_v01 Tetracorder color map showing a mountain snow scene in the Chile–Argentina border. The snow shows no detectable melting at higher elevations (magenta), but melting at lower elevations (cyan, light blue). Also shown are sediments in water from the snow melt. The EMIT swath width is approximately 77 km. This is a Tetracorder 5.27 standard product with expert system 5.27c1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce this image.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Eccentricity vs. semimajor axis of the 20:1 resonance with Neptune. In gray are resonance widths with only Neptune and the Sun acting as perturbers. In blue are resonance widths with all four giant planets included as perturbers. Notice how resonance width decreases with higher eccentricity in the four-planet case relative to the simplified case.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Example evolution of a test particle that scatters and sticks to Neptune's resonances. We show the evolution in barycentric a vs. time (upper left), ψ vs. time (upper right), q vs. time (lower left), and a–ψ space (lower right). We highlight sticking events in the 35:2 (ψ alternates between ∼90° and ∼270° at each perihelion passage) and the 17:1 (ψ first librates in the leading asymmetric island then the trailing island).
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Resonance strengths as a function of the N:U period ratio averaged across Neptune’s 2:1 through 14:1 resonances (left panel) and 15:1 through 28:1 resonances (right panel). The blue points and dashed lines show the averaged strengths in simulations with the Sun and all four giant planets, with Neptune’s semimajor axis increased or decreased to change its period ratio with Uranus. The black points and dashed lines show the averaged strengths in simulations with the same values of Neptune’s semimajor axes but with Uranus removed (i.e., simulations with the Sun, Jupiter, Saturn, and Neptune as perturbers). The red stars highlight the present-day N:U period ratio (1.96) in the simulations with Uranus removed; the average resonance strengths measured in each simulation are normalized relative to these two values (both red stars are at y = 100). The purple triangles represent the averaged strength from a set of simulations where Uranus perturbs the orbits of Neptune and the other giant planets but is not included in the force calculations on the test particles. Note that these values are similar to those of the 1.96 N:U period ratio simulations with the full effects of Uranus included. Neptune’s more distant resonances (right panel) are much more dramatically weakened by the presence of Uranus across all tested N:U period ratios. All of Neptune’s resonances show the most dramatic weakening at period ratios close to the N:U 2:1 and less weakening at higher N:U period ratios.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Relative sticking strengths of Neptune’s N:1 resonances for different N:U period ratios (see the Appendix for the definition of our strength parameter). The black triangles and dashed line show the strengths in the current solar system (Sun plus all four giant planets on their present-day orbits); the gray circles and dashed line show the strengths with Uranus removed. The four sets of colored points and lines show strengths from simulations with Jupiter, Saturn, and Uranus on their current orbits and Neptune’s semimajor axis adjusted to the labeled period ratio with Uranus (these are the same simulations shown in Figure 7). The purple colored points and lines show strengths from simulations where Uranus is included as a perturber for the other massive bodies but not for the test particles. In all simulations, the strengths have been normalized such that Neptune’s external 2:1 resonance has a strength of 100. There is a very rapid drop-off in N:1 resonance strengths with increasing N at the exact N:U 2:1 resonance. The resonance strengths plateau past the ∼5:1 in the simulation with Uranus removed. In the simulations with Uranus, the destabilization of Neptune’s distant N:1 resonances is more pronounced when the N:U period ratio is closer to 2:1. The simulations with limited gravitational effects from Uranus on the test particles show similar destabilization.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Barycentric semimajor axis (a) vs. ψ for particles in Neptune's distant resonances, with perihelia of 33 au; each resonant particle is plotted in a different color, while the background scattering population is plotted in gray. On the left, only the Sun and Neptune are included as perturbers. On the right, the Sun and all four giant planets are included as perturbers. Note how the N:1 resonances in the four-planet problem get weaker as the semimajor axis increases and begin to drop out entirely at the 20:1 position, with a brief resurgence around the 26:1 position. This contrasts the more gradual shrinking of distant resonances in the three-body problem.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Barycentric semimajor axis (a) vs. ψ for particles near Neptune's 20:1 resonance (a ≈ 221 au) with perihelion distance q = 33 au. In all panels, we plot particles that remain within 10 au of their initial semimajor axis in colored points, with each particle plotted in a different color (these are the particles that tend to interact with the resonances); less stable particles that quickly scatter away from their starting a are plotted as gray background points. In the top panel, only the Sun and Neptune act as perturbers on the test particles. In the middle left panel, the Sun and all major planets except for Uranus act as perturbers. In the middle right panel, the Sun and all four major planets act as perturbers. In the bottom left panel, all giant planets except Uranus act as perturbers, with the addition of a J2 parameter to simulate Uranus’s secular effects. In the bottom right panel, the Sun and all four giant planets are included as perturbers in the integration of the massive bodies, but the test particles are only perturbed by the Sun, Jupiter, Saturn, and Neptune. Note the similarity between the simplified (Sun + Neptune) model at the top and the middle left panel with Uranus excluded from the simulation. The destabilization of the 20:1 resonance only occurs when Uranus is included in the simulation; the destabilization remains when Uranus perturbs Neptune’s orbit but is not included as a perturber for the test particles themselves.
Paper: The Trojan-like Colors of Low-perihelion Kuiper Belt Objects
Authors: Matthew Belyakov, Michael E. Brown, Alya Al-Kibbi
Figure caption: Statistical comparison of Centaur (black; a < 30 au, q < 30 au), and low-perihelion Kuiper Belt (orange, a > 30 au, q < 30 au) colors, with Jupiter Trojan colors as dashed lines. The bottom panel shows the results of two tests of the difference in color of the Centaurs and low-perihelion KBOs: a one-sided Fisher exact test (black) and a bootstrap method (blue). In both tests, objects are sequentially added to the analysis starting with the lowest-perihelion objects. For any perihelion 15 au < q < 25 au, the probability that the proportion of red objects in the low-q KBOs is greater than that of the Centaurs is more than 3σ for the Fisher test and nearly 4σ for the bootstrap method, indicating that the low-perihelion Kuiper Belt is potentially a Trojan-like population in the outer solar system.
Paper: The Trojan-like Colors of Low-perihelion Kuiper Belt Objects
Authors: Matthew Belyakov, Michael E. Brown, Alya Al-Kibbi
Figure caption: Gaussian mixture models for the spectral slopes of the Jupiter Trojans (top panel), Centaurs (middle panel), and low-perihelion KBOs (bottom panel). Only objects with spectral slope <15% or those objects with Trojan-like slopes are included. For the Centaurs, a single-Gaussian model is preferred to describe the data, with a double-Gaussian fit shown with dotted lines for reference. By contrast, the spectral slopes of the low-q KBOs are best described by a bimodal model, with a ΔAIC = 14 between the unimodal and bimodal models.
Paper: The Trojan-like Colors of Low-perihelion Kuiper Belt Objects
Authors: Matthew Belyakov, Michael E. Brown, Alya Al-Kibbi
Figure caption: Left panel: the median total years spent within 20 au of realizations of simulated objects with orbital elements similar to the observed low-q KBOs (orange circles) and Centaurs (black circles). The Centaurs spend a similar amount of time within 20 au to the low-q KBOs. Right panel: simulation of the proportion of red objects in the two populations (starting from around the KBO red proportion), assuming that heating is responsible for changing very red objects into red ones. The difference between Centaurs and low-q objects in their red/total ratio never approaches that of the photometric data. Heating is therefore not sufficient to create the observed difference between the two populations.
Paper: The Trojan-like Colors of Low-perihelion Kuiper Belt Objects
Authors: Matthew Belyakov, Michael E. Brown, Alya Al-Kibbi
Figure caption: Schematic of the method used in Section 3 for tracking the source and dynamical evolution of low-q KBOs and Centaurs. We begin with the CFEPS L7 simulated Kuiper Belt reference population (Petit et al. 2011), integrating it forward for 4 Gyr with the four giant planets. These integrations produce around 150,000 realizations of the q < 25 au component of the Kuiper Belt. Simultaneously, we find the color distribution for each CFEPS object based on the known colors of nearby KBOs, using a K-nearest neighbor algorithm. During the integration, we also track the heating history (time spent within 20 au) of all of the synthetic objects. Using all of these snapshots of synthetically generated low-q KBO and Centaur populations, we then compute statistics on real objects that we have colors for by drawing the closest objects from our simulations. As a result, we obtain distributions on both the possible heating histories and color as a function of original Kuiper Belt source for the Centaurs and low-q KBOs from Section 2.
Paper: The Trojan-like Colors of Low-perihelion Kuiper Belt Objects
Authors: Matthew Belyakov, Michael E. Brown, Alya Al-Kibbi
Figure caption: Colors and perihelia of the KBOs (blue; a > 30 au) and Centaurs (black; a < 30 au) taken from MBOSS and Col-OSSOS (Hainaut et al. 2012; Schwamb et al. 2019). The colors of the two Jupiter Trojan subpopulations are shown as dashed lines. While KBO and Centaur colors are statistically indistinguishable and significantly different from Jupiter Trojan colors, the colors of KBOs at low perihelia appear Trojan-like below q < 25 au.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as Xk-types. Plotted are (55) Pandora (DeMeo et al. 2009; black open squares), CM2 chondrite EET 83389 (<125 μm; red line), pallasite Y-8451 (slab; blue line), and EH4 chondrite Abee (<125 μm, heated at 800°C for 1 week in 10–5 atm of H2; green line). The Pandora spectrum was normalized to unity at 0.55 μm and then multiplied by 0.3013 (IRAS albedo; Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as R-types. Plotted are (349) Dembowska (DeMeo et al. 2009), lodranite Lodran (chip; red line), howardite EET 87503 (<25 μm; blue line), and eucrite PCA 82501 (bulk; green line). The Dembowska spectrum was normalized to unity at 0.55 μm and then multiplied by 0.3840 (IRAS albedo; Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as U-types. Plotted are ungrouped C2 chondrite Tagish Lake (<45 μm, heated at 200°C for 1 week with oxygen eater; red line), Martian meteorite (chassignite) NWA 2737 (<45 μm; blue line), and R chondrite Rumuruti (<150 μm; green line).