adsabs/AstroCLIMB huggingface dataset:
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: Nonproteinogenic amino acid and other organic abundances measured in the four organic haze particle samples in this study. Biomolecule order is from lowest to highest molar mass. Units are μg biomolecule/g haze particles, or ppm.
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: Proteinogenic amino acid abundances measured in the four organic haze particle samples in this study. Amino acid order is from lowest to highest molar mass. Units are μg biomolecule/g haze particles, or ppm.
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: Blank-subtracted GC/MS/MS chromatograms for extracted samples of the high-methane organic haze particles, the low-methane organic haze particles, and the 1- and 7-day heated high-methane organic haze particles.
Paper: An Updated Shape Model of Dimorphos from DART Data
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Hari Nair, Harrison Agrusa, Nancy L. Chabot, Andrew F. Cheng, Elisabetta Dotto, Elena Mazzotta Epifani, Raymond C. Espiritu, Tony L. Farnham, Eric E. Palmer, Petr Pravec, Andrew S. Rivkin, Dany C. Waller, Angelo Zinzi
Figure caption: Terminator position as a function of asteroid elongation. (a) The last DRACO image to contain all of Dimorphos (dart_0401930039_14119_01_iof.fits), with overlays as described in Figure 5. (b)–(j) Simulated images of triaxial ellipsoids with different a/b ratios. The tips of the blue arrows show the positions of terminator markers. Panel (h) shows the starting ellipsoid for the updated model. Panel (i) shows the starting ellipsoid for the preliminary model.
Paper: An Updated Shape Model of Dimorphos from DART Data
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Hari Nair, Harrison Agrusa, Nancy L. Chabot, Andrew F. Cheng, Elisabetta Dotto, Elena Mazzotta Epifani, Raymond C. Espiritu, Tony L. Farnham, Eric E. Palmer, Petr Pravec, Andrew S. Rivkin, Dany C. Waller, Angelo Zinzi
Figure caption: The highest-resolution DRACO image to contain all of Dimorphos (dart_0401930039_14119_01_iof.fits), with markings related to terminator identification. (a) Shadows (outlined in yellow) cast by large boulders prematurely create darkness. (b) Disconnected knobs of terrain (green) lie beyond the terminator of the background shape. (c) The farthest pieces of contiguous lit terrain in areas not affected by shadows from large boulders are reliable markers (blue arrows) of the terminator position. (d) Boulder shadows, terrain knobs, and terminator markers overlaid on the same image.
Paper: An Updated Shape Model of Dimorphos from DART Data
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Hari Nair, Harrison Agrusa, Nancy L. Chabot, Andrew F. Cheng, Elisabetta Dotto, Elena Mazzotta Epifani, Raymond C. Espiritu, Tony L. Farnham, Eric E. Palmer, Petr Pravec, Andrew S. Rivkin, Dany C. Waller, Angelo Zinzi
Figure caption: SPC maplets relative to the size of Dimorphos. (a) Extent of a single maplet with the labeled GSD. Many overlapping maplets of a given GSD are tiled across the body wherever DRACO images cover sunlit terrain. (b) Extent of the location of the finest-scale standard maplet to cover a given part of the body. The diamond-shaped patterns follow the outlines of DRACO images whose pixel scales are twice the maplet GSD. The figure shows only the finest-scale maplets in a given area. Each area is also covered by maplets with a coarser GSD than the color shown. For example, the area covered by 2.8 cm maplets is also densely tiled with 4.2-, 7.2-, 8.6-, 10-, 25-, and 60-cm maplets. The example maplets are shown in the updated model described in this paper.
Paper: An Updated Shape Model of Dimorphos from DART Data
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Hari Nair, Harrison Agrusa, Nancy L. Chabot, Andrew F. Cheng, Elisabetta Dotto, Elena Mazzotta Epifani, Raymond C. Espiritu, Tony L. Farnham, Eric E. Palmer, Petr Pravec, Andrew S. Rivkin, Dany C. Waller, Angelo Zinzi
Figure caption: An analysis of the quality of the DRACO images compared to the ideal image set for SPC. The figure shows the number of cardinal look directions met by DRACO images. DRACO images satisfy only one of the imaging conditions that lead to optimal SPC results. The color bar shows the number of cardinal directions that are satisfied, not the number of images that match a particular cardinal direction.
Paper: An Updated Shape Model of Dimorphos from DART Data
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Hari Nair, Harrison Agrusa, Nancy L. Chabot, Andrew F. Cheng, Elisabetta Dotto, Elena Mazzotta Epifani, Raymond C. Espiritu, Tony L. Farnham, Eric E. Palmer, Petr Pravec, Andrew S. Rivkin, Dany C. Waller, Angelo Zinzi
Figure caption: The final DRACO image to contain all of Dimorphos (dart_0401930039_14119_01_iof.fits). (a) When stretched normally, the sunlit limb on the left side of the body is clearly revealed. Didymos is out of the scene and to the right, and scattered light from Didymos illuminates the dark side of Dimorphos. (b) Strongly stretching the image brings out the dark Didymos-lit limb (white arrows). (c) Combining the limbs from the sunlit and Didymos-lit terrain reveals the complete outline of Dimorphos.
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: Calibration curves calculated for 22 amino acids and other organics. Equations of the lines of best fit and χ 2 values are added to the legend. Uncertainties are the shaded regions calculated as the variance from a model linearly connecting each data point. Peak areas for the 7-day, 200°C heated 5% CH4 haze particles are added to the plots to demonstrate our quantification calculations.
Paper: An Updated Shape Model of Dimorphos from DART Data
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Hari Nair, Harrison Agrusa, Nancy L. Chabot, Andrew F. Cheng, Elisabetta Dotto, Elena Mazzotta Epifani, Raymond C. Espiritu, Tony L. Farnham, Eric E. Palmer, Petr Pravec, Andrew S. Rivkin, Dany C. Waller, Angelo Zinzi
Figure caption: Process used to build the updated shape model of Dimorphos. Green text denotes places where the steps used to build the updated shape model differed from those used to build the preliminary model.
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: Calibration curves calculated for 22 amino acids and other organics. Equations of the lines of best fit and χ 2 values are added to the legend. Uncertainties are the shaded regions calculated as the variance from a model linearly connecting each data point. Peak areas for the 1-day, 200°C heated 5% CH4 haze particles are added to the plots to demonstrate our quantification calculations.
Paper: Depth-to-diameter Ratios of Fresh Craters on the Moon and Implications for Surface Age Estimates
Authors: Rachael H. Hoover, Stuart J. Robbins, Brian M. Hynek, Paul O. Hayne
Figure caption: Summary of d/D results reported in Stopar et al. (2017). Panel (a) shows data for all “fresh” craters, panel (b) displays only the freshest craters (A craters), and panels (c) and (d) show fresh craters with increasing evidence of degradation (AB and B craters, respectively). Note that their publicly available data are quantized to two decimal points.
Paper: Current Events at Saturn: Ring–Planet Electromagnetic Coupling
Authors: Omakshi Agiwal, Hao Cao, Hsiang-Wen Hsu, Luke Moore, Ali H. Sulaiman, James O'Donoghue, Michele K. Dougherty
Figure caption: In situ B  ϕ  measurements taken by Cassini MAG on ring-connected magnetic field lines are shown for 21 out of 22 Grand Finale orbits (Revs 271-292) in panels (a) and (b). Rev 277 is omitted due to missing data in the region of interest. The data are shown at 1 s resolution and organized by magnetic L-shell. The data from individual orbits are shown by different colored solid lines, and the median B  ϕ  from the (a) inbound (z > 0 R S) and (b) outbound (z < 0 R S) segments of all the orbits is shown by a thick solid black line. The L-shell mapping of Saturn’s rings is indicated by shaded gray regions. Panels (c) and (d) show the field-aligned currents j ∣∣ derived from the gradients in B  ϕ  for the (c) inbound and (d) outbound segment of each orbit as a function of the L-shell. The j ∣∣ are positive (pink) when flowing in the same direction as the background magnetic field. Black dashed, dotted, and solid lines indicate the Kronosynchronous Orbit (KSO ∼ 1.85 R S; dashed), the X06 emission source (∼1.76 R S), and the cold plasma critical radius (r  C  ∼ 1.62 R S; solid) on all panels. Black box-and-whisker plots outside the main axes in panels (c) and (d) show the median (solid horizontal line), interquartile range (box), and interdecile range (whiskers) of the L-shell mapping of the j ∣∣ signatures. The L-shell mapping of the CDA CAT impact rates, the ﹩{{\rm{H}}}_{3}^{+}﹩ emissions, and the RPWS constraints on the whistler wave emission source are also indicated on panels (c) and (d). The B  ϕ  measurements and j ∣∣ distributions presented in this figure can be found on Zenodo: doi:10.5281/zenodo.10823289 (Agiwal 2024).
Paper: Current Events at Saturn: Ring–Planet Electromagnetic Coupling
Authors: Omakshi Agiwal, Hao Cao, Hsiang-Wen Hsu, Luke Moore, Ali H. Sulaiman, James O'Donoghue, Michele K. Dougherty
Figure caption: A meridional view of Saturn is shown in cylindrical (ρ, z) coordinates. The planetary magnetic field is shown using gray contours, and the planetary rings are shown by gray slabs at z = 0 R S. Solid black lines indicate a representative spacecraft trajectory near orbit periapsis from the Cassini Grand Finale. Projected along the trajectory are in situ Cassini measurements of the median B  ϕ  from MAG (blue–red color bar), dust impact rates from CDA (yellow histogram), and whistler mode wave emissions from RPWS (downward and upward green triangles indicate the start and stop locations of individual whistler mode emission intervals) from the Grand Finale. The current system proposed by Xin et al. (2006) is indicated by the shaded pink region. The direction of current flow is indicated by pink solid lines and arrows. The ring plane position of the Kronosynchronous orbital boundary (KSO) at ρ ∼ 1.85 R S and the RPWS whistler mode wave emission source constrained by Xin et al. (2006) are indicated. The “critical radius” r  C  boundary is shown by a solid yellow line, which scales with latitude λ as ﹩{r}^{3}={r}_{C}^{3}{\;\mathrm{cosec}}^{2}\,(\lambda )﹩. The shaded yellow region within is where models predict ionospheric siphoning of ring plasma, or “ring rain.” Modeled trajectories of charged dust grains flowing from the rings to the ionosphere along B are shown in brown. Finally, ﹩{{\rm{H}}}_{3}^{+}﹩ ion emissions (white–red–black color bar) from remote observations of Saturn’s upper atmosphere in ∼2011 are projected at their observed latitudes on Saturn’s surface.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) image of Gruithuisen region displaying the near side of the Moon. PKT represents Procellarum KREEP Terrane and GR represents Gruithuisen Region. (b) Close-up view of the Gruithuisen region using WAC. G denotes Gamma dome, D represents Delta dome, NW indicates the Northwestern dome, GE denotes the Gamma Extension, and Hummocky denotes the highlands region nearby.
Paper: Current Events at Saturn: Ring–Planet Electromagnetic Coupling
Authors: Omakshi Agiwal, Hao Cao, Hsiang-Wen Hsu, Luke Moore, Ali H. Sulaiman, James O'Donoghue, Michele K. Dougherty
Figure caption: This figure has the same format as Figures 2(a) and (b), except it shows n = 2 polynomial subtracted ΔB  ϕ  measurements that serve as a proxy for removing the effects of the PPO and auroral field-aligned current perturbation fields. The red arrows indicate the region mapping to the L-shell between ∼1.95 and 2.6 R S (B-ring outer edge to A-ring inner edge, respectively). The n = 2 polynomial was fit only to the data in this region and then subtracted from the MAG data connected to the A–C rings.
Paper: Current Events at Saturn: Ring–Planet Electromagnetic Coupling
Authors: Omakshi Agiwal, Hao Cao, Hsiang-Wen Hsu, Luke Moore, Ali H. Sulaiman, James O'Donoghue, Michele K. Dougherty
Figure caption: This figure follows the same general format as Figure 1. The interhemispheric, intra D-ring field-aligned current system is shown using solid pink lines. Meanwhile, the proposed flow and closure of the B-ring field-aligned current system is shown using dashed pink lines. Pink arrows indicate the direction of current flow for both current systems. Large gray arrows and corresponding labels indicate the bifurcation of ring plasma properties inferred from our analysis that would control the pathways of current closure.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) WAC image of Gruithuisen domes region. (b) Reflectance spectra of the locations marked in 2a. The vertical lines represent 1000 and 2000 nm. (c) Continuum-removed reflectance spectra displayed in 2b. (d) M3 map of estimated band center near 1000 nm (EBC1). (e) M3 map of estimated band center near 2000 nm (EBC2). (f) Histogram displaying distribution of EBC1 and EBC2 over the region.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) 24 hr temperature variation of the Gamma dome. The beginning and end of the blue box represent the 25th and 75th percentiles of the values, and the pink line in the middle represents the 50th percentile (median). The black lines (or black dots) at the top and bottom are the maximum and minimum. The green dots are outliers with more than 1.5 times the value of the 25th or 75th percentiles. (b) 24 hr temperature variation of the Gamma extension. (c) 24 hr temperature variation of the Delta dome. (d) 24 hr temperature variation of the mare and highlands area surrounding the domes. (e) Histogram displaying variation in the maximum temperature. (f) Histogram displaying variation in the minimum temperature. The data displayed for all the units in this figure are for flat surfaces. See Table A1 for more details.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Kaguya 750 nm image displaying the albedo of the region; NC and NA refer to the locations of the newly identified crater and mound. (b) Histogram displaying the variation in albedo of the three domes. (c) FeO image of the region. (d) Histogram displaying the variation in FeO wt.% of the three domes. (e) CF image of the region. (f) Histogram displaying the variation in CF of the three domes.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Image displaying difference between the maximum and minimum temperatures in the region. (b) Normalized maximum temperature vs. nighttime anisothermality, with markers colored by temperature amplitude for pixels with slope less than 15°. (c) H-parameter map of the region. (d) Histogram displaying distribution of H-parameter across the domes for pixels with slope less than 15°.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Rocks mapped on top of the Gamma dome. (b) Map displaying the sizes of the mapped boulders atop the Gamma dome. (c) Histogram displaying boulder size on top of the Gamma dome. (d) Power-law fit between cumulative size frequency distribution and boulder lengths binned at 0.5 m intervals.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Water abundance map of the region. (c) Histogram displaying the variation in water abundance over the three domes and surrounding region (includes both mare and highland shown in the figures).
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Rock abundance map from Bandfield et al. (2017) of the region. (b) Rock abundance vs. nighttime anisothermality of the region (c) Nighttime anisothermality map of the region. (d) High-resolution NAC image of the two young craters atop the Gamma dome.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Maximum temperature image of the region. (b) Cosine fit of the mean of the maximum temperatures by latitude. (c) Normalized maximum temperature of the region using the cosine fit from (b). (d) Minimum temperature image of the region. (e) Cosine fit of the mean of the minimum temperatures by latitude. (f) Normalized minimum temperature of the region using the cosine fit from (e).
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) NAC image of the hummocky region with the newly identified mound and the crater. (b) Kaguya 750 nm albedo image of region. (c) FeO image of the region. (d) CF image of the region. (e) Elevation of the domes and newly identified silicic regions overlaid onto the WAC image.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) Vent structure to the south of the Gamma extension. (b) High-resolution NAC view of the vent.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) NAC image of the newly identified crater. (b) FeO image of the crater. (c) CF image of the crater. (d) NAC image of the newly identified dome. (e) FeO image of the dome. (f) CF image of the dome.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: (a) H-parameter on top of the Gamma dome. (b) Rock abundance on top of the Gamma dome. (c) H-parameter on top of the Gamma dome. (d) Rock abundance on top of the Gamma dome.
Paper: Extended Silicic Volcanism in the Gruithuisen Region—Revisiting the Composition and Thermophysical Properties of Gruithuisen Domes on the Moon
Authors: Nandita Kumari, Timothy D. Glotch, Jean-Pierre Williams, Mark T. Sullivan, Shuai Li, Benjamin T. Greenhagen, Dany Waller, Tyler Powell, Catherine M. Elder, Benjamin D. Byron, Katherine A. Shirley
Figure caption: Magnetic field strength image of the region.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: The average plume spectra and residual of 249 spectral cubes from Cassini-VIMS observed from 2005 to 2015. The top panel shows the background-subtracted average spectra along with a quadratic fit to the regions between 2.484–2.598 μm and 2.748–2.850 μm. The middle panel shows the residual brightness after subtracting the quadratic polynomial. The bottom panel shows the same plume residual compared to the PSG models for 2005 (gray), 2010 (black), and 2015 (red). The wavelength shift in the PSG models was applied using values from Clark et al. (2018). The models assume a column density of 3.63 × 1019 molecules m−2, consistent with the best-fit column density based on the feature’s band area (see Section 3.3).