adsabs/AstroCLIMB huggingface dataset:
Paper: The State of CO and CO2 Ices in the Kuiper Belt as Seen by JWST
Authors: Michael E. Brown, Wesley C. Fraser
Figure caption: The geometric albedo from a collection of Mie scattering particles from 0.1 to 10 μm in diameter. The colors of the lines correspond to the scattering behavior at the different wavelengths of the same colors of the dashed lines in Figure 2. The strong changes in both the real and imaginary index of refraction across this spectral region make the spectral behavior an extremely complicated and sensitive function of particle size.
Paper: The State of CO and CO2 Ices in the Kuiper Belt as Seen by JWST
Authors: Michael E. Brown, Wesley C. Fraser
Figure caption: Full spectral models of a collection of Mie scattering CO2 particles of four particle sizes. The prominent peaks at both 4.19 and 4.34 μm are only seen for particle diameters of 1–2 μm.
Paper: The State of CO and CO2 Ices in the Kuiper Belt as Seen by JWST
Authors: Michael E. Brown, Wesley C. Fraser
Figure caption: The spectra of two representative KBOs from the sample. Each shows subtle 1.5 and 2.0 μ absorption features indicative of a modest exposure of water ice, deep 3 μm absorption consistent with a tholin-like processed organic surface, a broad 3.4–3.6 μm absorption owing to organic materials, a narrow 4.6 μm absorption from CO, and numerous and variable features from 4.0 to 4.4 μm all attributable to CO2.
Paper: MIR Spectra and Analysis of Jovian Trojan Asteroids
Authors: Audrey C. Martin, Joshua P. Emery
Figure caption: Measured SEDs (black points) of the Trojans with the calculated best-fit NEATM (red lines) for each object. The radius, p  v , and η for each Trojan is listed in its respective panel and Table 2.
Paper: MIR Spectra and Analysis of Jovian Trojan Asteroids
Authors: Audrey C. Martin, Joshua P. Emery
Figure caption: The SST/IRS emissivity spectra of Achilles, Patroclus, Nestor, Diomedes, Deiphobus, Teucer, Eurybates, Thestor, Deipylos, Ennomos, and Iphinous. The spectra of Hektor, Aneas, and Agamemnon from Emery et al. (2006) have been rereduced using version S18.18 of the Spitzer calibration pipeline.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Hybrid mapping reveals the complex overlap of ejecta compositions from Marcia, Calpurnia, and Minucia craters. (A) LAMO mosaic, showing albedo. (B) Digital Terrain Model acquired from Survey orbit data, where low areas are in blue shades and higher areas are in red and brown. (C) HAMO color-ratio mosaic. (D) Portion of hybrid map associated with (A)–(C).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Ages of the five cratered terrain units derived from crater statistics: (A) Cratered highlands; (B) Cratered terrain, greenish-yellow; (C) Cratered terrain, purple–blue–orange; (D) Cratered terrain, purple–orange; (E) Cratered terrain, light blue–orange. Counts using the lunar-derived method (LDM; left) and asteroid-derived method (ADM; right) are shown. Crater plots for all other units where crater statistics could be taken are included in the Appendix for this manuscript.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Ejecta patterns from Numisia, Cornelia, and Drusilla craters on Vestallia Terra show the complexity of mixing materials (sharp crater rays) and enigmatic ejecta materials (orange spots around Teia). (A) FC HAMO mosaic. (B) FC color-ratio mosaic. (C) Hybrid map.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Generalized correlation of map units (COMU). On the y-axis are unit ages as calculated using the LDM; periods based on the LDM and ADM are listed to the right of unit ages. The Rheasilvia impact served to reset ages across Vesta.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for crater material, undivided (c1). The μ symbol indicates that age is based on a numerical model, in this figure and others. (b). Crater size–frequency distribution and randomness plots calculated from ADM for crater material, undivided (c1).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for crater material, greenish-yellow (c2). (b). Crater size–frequency distribution and randomness plots calculated from ADM for crater material, greenish-yellow (c2).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for crater material, light blue (c4). (b). Crater size–frequency distribution and randomness plots calculated from ADM for crater material, light blue (c4).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for crater material, orange (c5). (b). Crater size–frequency distribution and randomness plots calculated from ADM for crater material, orange (c5).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots from LDM for crater material, purple (c3). (b). Crater size–frequency distribution and randomness plots calculated from ADM for crater material, purple (c3).
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Methane clathrate stability as a function of NaCl wt%. Increasing the salt content raises the equilibrium pressure required to keep methane clathrate stable. Other clathrate types exhibit a similar increase in dissociation pressure with increasing salt concentration.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Alternate phase assemblage assuming that Pluto accretes from cometary dust with a 1:1:1 ratio of C:O:H. In this case, Pluto’s mantle contains anhydrous silicates after differentiation and therefore does not go through a dehydration event that releases water. Therefore, in this scenario the only significant volatile release would be CO2.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Wt% of extracted volatiles from mineral phase changes during Pluto’s thermal evolution as a function of temperature and pressure. Only H2O and CO2 release is significant. The remaining species are released as solutes within water.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Left: roughness spectra of the six k-means classes. Error bars represent the standard deviation of 1 km pixels for each class and baseline. Middle: box plots of the roughness spectral slope of the classes. Each box shows the median (horizontal line), mean (plus sign), interquartile range (box edges), and 9th/91st percentiles (whiskers). Right: box plots of the mean roughness over all baselines.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: LOLA roughness (meters) on 50 m baselines (left panel), LOLA 1064 nm normal albedo (middle panel), and LROC WAC 321 nm reflectance (right panel; Lunar QuickMap; https://quickmap.lroc.asu.edu/). The black square outlines the 80°–90° S region covered by the color-composite image (Figure 12), which is overlaid on the right panel where the WAC mosaic has no data. Candidate ejecta rays are labeled with arrows and, in the right panel, overlaid with great circles.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Box plots of LOLA 1064 nm normal albedo (left) and FeO wt.% (right) for the k-means classes. Each box shows the median (horizontal line), mean (plus sign), interquartile range (box edges), and 9th/91st percentiles (whiskers).
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: PSR CSFD (left) and CAFD (right) for 80°–90° S. In each panel, the total distribution (thick black line) is compared to that in nine equal-area annuli moving out from the pole (dark blue to red thin lines) with outer radii of 101.33, 143.31, 175.51, 202.67, 226.59, 248.21, 268.10, 286.61, and 304.00 km.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Left: Hurst exponent over 100–800 m baselines (1 km pixel−1). The color scale ranges from the 2nd to the 98th percentile. Right: same as Figure 16, but for the Hurst exponent of the k-means classes.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: 2D histogram showing the relative frequency of the k-means classes as a function of 1600 m baseline slope. Each column is normalized to the total number of points in that column, with the color indicating the fraction of each column’s total within each bin. The white lines show the mean and standard deviation.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Comparison between slope, Hurst exponent, and roughness on 200 m (top row) and 1600 m (bottom row) baselines at 50 m pixel−1. The Hurst exponent is generally smaller at 800–1600 m baselines (panel (e)) compared to 100–200 m baselines (panel (b)), and the Hurst exponent inside individual craters decreases as their size relative to the baseline decreases.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: 1 km pixel−1 map of the k-means classes, with cold to hot colors representing low to high roughness spectral slope, respectively.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: New 20 m pixel−1 map of PSRs within 80°–90° S.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: Distribution of NavCam cloud observations at various times of sol as a function of solar longitude, LS, and mission sol number. Red dots are cloud movies, blue stars are cloud surveys, and black circles are observations in which we have seen clouds. The gray box highlights the ACB season from LS ∼45° to ∼140°.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: The top four images depict the raw FDR frames 1, 3, 6, and 8 from the NavCam cloud movie captured on sol 292 at LMST 16:23. By observing the prominent cloud features, for example, features enclosed within the black circles, it is noticeable that these clouds exhibit a general diagonally downward motion.
Paper: VLT/MUSE Characterization of Dimorphos Ejecta from the DART Impact
Authors: Brian P. Murphy, Cyrielle Opitom, Colin Snodgrass, Matthew M. Knight, Jian-Yang Li, Nancy L. Chabot, Andrew S. Rivkin, Simon F. Green, Paloma Guetzoyan, Daniel Gardener, Julia de León
Figure caption: Primary tail relative flux profiles as measured from the integrated area under the Lorentzian fits. Cooler colors represent earlier dates in the campaign, while warmer colors represent later dates. Uncertainties have been removed from the measurements, since we have artificially offset the profiles to compare their relative slopes. Black lines depict the regions where we applied power-law fits.
Paper: VLT/MUSE Characterization of Dimorphos Ejecta from the DART Impact
Authors: Brian P. Murphy, Cyrielle Opitom, Colin Snodgrass, Matthew M. Knight, Jian-Yang Li, Nancy L. Chabot, Andrew S. Rivkin, Simon F. Green, Paloma Guetzoyan, Daniel Gardener, Julia de León
Figure caption: Primary tail widths as measured from the FWHM of the Lorentzian fits. Cooler colors represent earlier dates in the campaign, while warmer colors represent later dates. Width measurements on October 19 cannot be commented on, as atmospheric seeing for that night is on the order of 3–5× higher than all other observations, and have positively biased our measurements.
Paper: VLT/MUSE Characterization of Dimorphos Ejecta from the DART Impact
Authors: Brian P. Murphy, Cyrielle Opitom, Colin Snodgrass, Matthew M. Knight, Jian-Yang Li, Nancy L. Chabot, Andrew S. Rivkin, Simon F. Green, Paloma Guetzoyan, Daniel Gardener, Julia de León
Figure caption: Secondary tail relative flux profiles as measured from the integrated area under the Lorentzian fits. Cooler colors represent earlier dates in the campaign, while warmer colors represent later dates. Uncertainties have been removed from the measurements, since we have artificially offset the profiles to compare their relative slopes. Black lines depict the regions where we applied power-law fits.
Paper: VLT/MUSE Characterization of Dimorphos Ejecta from the DART Impact
Authors: Brian P. Murphy, Cyrielle Opitom, Colin Snodgrass, Matthew M. Knight, Jian-Yang Li, Nancy L. Chabot, Andrew S. Rivkin, Simon F. Green, Paloma Guetzoyan, Daniel Gardener, Julia de León
Figure caption: Secondary tail position angles (top panel) and widths (bottom panel), from October 3 to 14. Cooler colors represent earlier dates in the campaign, while warmer colors represent later dates.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Elemental abundance ratios for the Hypatia catalog stars in dex. Throughout, the white star shows solar values. (a) [Mg/H] vs. [Fe/H], showing growth of an α nuclide compared with Fe. [Fe/H] is broadly taken as an indicator of time. The influence of Type Ia supernovae on GCE is indicated by the two arrows. (b) Same data as [Mg/Fe] vs. [Fe/H]. The solid negatively sloping line shows the effect of induced ratio correlation due to Fe appearing on both axes. (c) Same as panel (b), but with contours showing 50%, 80%, and 95% levels for the chondritic (solid contours) and nonchondritic (dashed contours) populations of stars based on ﹩{\chi }_{\nu }^{2}﹩ tests. The larger points indicate stars that pass as chondritic, and the smaller points do not pass. The nonchondritic population generally extends to lower metallicities than the chondritic stars. (d) Ratios of lithophile elements only, showing no clear trend.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Comparison of Hypatia catalog metal abundances to chondritic composition, for the 35 randomly chosen Hypatia catalog stars. The ﹩{\chi }_{\nu }^{2}﹩ parameter is listed for each star. The order of elements in each plot, from left to right, is Cr, Ni, Ca, Al, Fe, Si, all ratioed to Mg. Stars with dark-gray backgrounds are not considered a good fit to chondrite, using an α parameter of 0.05 for goodness of fit. Stars with light-gray backgrounds are not a good fit for chondrite when all elements are used to calculate ﹩{\chi }_{\nu }^{2}﹩, but they do pass as chondritic when an outlier element is ignored (outliers highlighted in orange).
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Comparison of WD pollution compositions to the CI chondrite composition, for the raw data (top) and steady-state-adjusted abundances (bottom). The order of elements in each plot, from left to right, is Cr, Ni, Ca, Al, Fe, Si, all ratioed to Mg. The ﹩{\chi }_{\nu }^{2}﹩ parameter appears in the upper left corner of each panel. WDs with white backgrounds are consistent with having accreted a chondritic rock composition. WDs with dark-gray backgrounds are not considered a good fit to chondrite, using an α parameter of 0.05 for goodness of fit. WDs with light-gray backgrounds have an outlier element that allows the WDs to pass as chondritic when the outlier is removed (outliers highlighted in orange).
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption:                    ﹩{\chi }_{\nu }^{2}﹩ for each WD, relative to CI chondrite, for the raw abundances (circles) and steady-state-adjusted values (triangles). The points are colored and grouped by n, the number of elements used to calculate ﹩{\chi }_{\nu }^{2}﹩. The horizontal line shows a typical critical ﹩{\chi }_{\nu }^{2}﹩ value (﹩{\chi }_{\nu }^{2}\sim 3﹩–4, based on the number of observed elements). In most cases, the steady-state values provide a better fit.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Ternary diagram for all of the WD samples, for raw abundances. The white points indicate the OLV, OPX, and CPX quantities derived from the median values of Mg, Ca, and Si for each WD. We also demonstrate the spread in OLV, OPX, and CPX that is due to the uncertainties in the WD abundances by showing the spread from 100 random draws of Mg, Si, and Ca for WD Ton345. The total spread in points is truncated for visibility.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Ternary diagram for 100 randomly selected Hypatia stars, and the spread in OLV, OPX, and CPX for one of the best Hypatia fits to chondrite, HIP 26834 (﹩{\chi }_{\nu }^{2}\sim 0.02﹩). Despite being statistically indistinguishable from chondritic composition, the uncertainties in the measured abundances lead to huge spread in OLV and OPX quantities. Similar OLX, OPX, and CPX ranges resulting from propagation of uncertainties are found for all of the Hypatia stars.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: The fractional difference between the measured abundances in the Hypatia catalog stars relative to chondrite, for the stars that do not pass as chondritic. For the nonchondritic stars, siderophiles (Fe, Cr, Ni) tend to be the worst-fitting elements rather than lithophiles.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Distribution of elemental abundances in Hypatia catalog stars relative to solar abundances, grouped by stellar type. All element distributions are well centered at solar abundances, with the exception of Ca in M stars and Al in F stars.
Paper: A Chondritic Solar Neighborhood
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young
Figure caption: Distribution of the distances of Hypatia catalog stars from the Sun (classified by stellar type). M dwarfs in the sample tend to be much closer to the Sun than other stars in the catalog. K stars also appear to have a bimodal distribution in distance.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Scans along the tails of the SPACEOBS images. The panels are labeled (a)–(i), corresponding to the dates shown in Table 2 (“Code” column). The black lines correspond to the observations and the red line to the model. The horizontal axes are labeled in kilometers projected on the sky plane, and the vertical axes are expressed in mag arcsec−2. These scans were obtained using a broken power-law differential size distribution function with κ = −2.5 between 1 μm and 3 mm and κ = −3.7 between 3 mm and 5 cm. The total dust mass sent to interplanetary space is 4.2 × 106 kg.