adsabs/AstroCLIMB huggingface dataset:
Paper: SOHO SWAN Lyα Models Supporting LRO LAMP: 2008–2023
Authors: Wayne R. Pryor, W. Kent Tobiska, Kurt D. Retherford, Cesare Grava, Anthony Egan, Thomas K. Greathouse, G. Randall Gladstone, Eric Quémerais
Figure caption: Top: solar Lyα line-integrated flux used as a model input at 1 au from the Sun for 2008–2023. Bottom: the value of the asymmetry parameter A of the best-fitting model for the SWAN data is shown as a function of time. Each dot is the daily best-fitting model; each diamond is the annually averaged best-fitting model. The annually averaged best-fitting models for points in the northern and in the southern hemispheres are shown with red triangles and green X symbols, respectively. A 43 R constant Galactic background was added to the scaled heliospheric model before fitting.
Paper: Artificial Impacts on the Moon: Modeling 3D Seismic Propagation Effects with AxiSEM3D
Authors: Ceri Nunn, Benjamin A. Fernando, Mark P. Panning
Figure caption: Observations of artificial impacts on the Moon, showing seismograms (blue) and smoothed seismic envelopes (purple). The impacts comprised lunar module impacts (purple circles) and Saturn IV impacts (pink circles). The events were recorded at Apollo stations S12, S14, S15, and S16. Seismograms are arranged with epicentral distance in degrees from impact to station. We removed seismograms that do not have a clear signal. Seismograms are from the vertical component (blue), with the exception of Apollo 16's Saturn IV recorded at S14, which is only available on the horizontal components (MH1, gray). We removed the instrument response and filtered seismograms and envelopes between 0.3 and 0.5 Hz. The envelopes are smoothed over 25 s. The traces are displayed in displacement and normalized to the maximum value of each trace. The x-axis is in seconds (the impact time is at 0 s) and the y-axis in degrees (1° on the Moon is ∼30 km). The left inset shows a close-up of 500 s. Theoretical arrival times for the P waves (blue dashed line), PS waves (magenta dashed line), and S waves (purple dashed line) are calculated using Model M1 (R. F. Garcia et al. 2019). The PS and S phases overlap. Additionally, we estimate a range for the onset of the P wave (pink box).
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: (a) Modeled H-parameter for the one-parameter model, showing the mask boundary (yellow) defined by H 1param = 0.025 m. (b) RGB composite map of the two-parameter model results only (no masking applied), with a 2%–98% stretch on each channel. (c) East–west slope, calculated from the 128 ppd SLDEM2015. For reference, the mask boundary defined by panel (a) is shown in gray in panel (b) and in black in panel (c). Arrows in panels (b) and (c) indicate west-sloping regions that correspond to anomalously high values of H/I  d,273K  in the two-parameter model. The pink star indicates the location of temperature data plotted in Figure 19.
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: (a) Bolometric surface temperatures from the location marked in Figure 18, showing nighttime data used in the model fit (red points) and daytime data (gray points), along with three modeled surface temperature curves: the best-fit one-parameter model (purple), the best-fit two-parameter model (dotted–dashed cyan), and the best-fit one-parameter model with the east–west component of local slope removed (dashed black). Arrows indicate local times where the third model shows a significantly better fit to the daytime data, demonstrating the sensitivity to topographic inputs. Note the break and change in scale of the y-axis to allow both daytime and nighttime data, as well as differences in the predicted surface temperature between the three models, to be sufficiently legible. (b) Subsurface variation in I 273K for the three models, with (c) a zoom-in on the upper 8 cm to show subtle differences within the thermal skin depth. (d) A grid search of the parameter space for the two-parameter model at this location, showing ﹩{\chi }_{r}^{2}﹩ for each pair of values. The red crosshairs and point indicate the best-fit values used for the model plotted in cyan in panels (a)–(c).
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: (a) Arecibo S-band CPR (color) modulated by same-sense polarized return (lightness) for the impact melt flow to the northwest of the highlands crater Glushko (8.°1 north, 77.°7 west, D = 43.1 km). (b) Mini-RF S-band monostatic and (c) X-band bistatic CPR (color) modulated by total backscattered power (lightness) for the same area. Note that CPR ranges in panels (a)–(c) have been adjusted to emphasize similar features, due to known discrepancies in absolute CPR values between Mini-RF and Arecibo data (L. M. Carter et al. 2017). (d) Diviner two-parameter model RGB composite of the same area, overlaid on a mosaic of Kaguya TC images (see Table 3 in Appendix A for the list of frames used). (e) I  d,273K values from the two-parameter model fit. In all panels, the main impact melt flow is outlined in pink.
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: Reduced chi-squared values at each 128 ppd spatial bin for the one-parameter (left column) and two-parameter (middle column) models, along with their ratio (right column), for (a–c) Giordano Bruno, (d–f) Tharp, (g–i) Wargo, and (j–l) Korolev Z. In all plots, the mask boundary based on the one-parameter model is shown in black. Note the higher range of values in panel (c) than in panels (f), (i), and (l).
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: (a–c) Diviner-derived RA from T. M. Powell et al. (2023) and (d–f) Diviner best-fit two-parameter model RGB composite overlaid on a base of NAC frame mosaics over the LROC WAC Global Morphology mosaic (E. J. Speyerer et al. 2011) for the craters Giordano Bruno (panels (a) and (d)), Wargo (panels (b) and (e)), and Korolev Z (panels (c) and (f)). See Table 3 in Appendix A for the list of NAC frames used for Giordano Bruno and Korolev Z. For Wargo, the base map is the LROC NAC controlled mosaic NAC_ROI_JOULE__TLOA_E275N2119 (S. M. Klem et al. 2014). Note the different range for RA in panel (a) compared to panels (b) and (c).
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: Close-up of the melt pool west of Messier (pink outline) with (a) the Diviner two-parameter model RGB composite and (b) Mini-RF monostatic S-band CPR (color) modulated by total backscattered power (lightness), overlaid on a combination of the same 12 m pixel−1 low-Sun Kaguya TC mosaic as in Figure 11 and a 1.8 m pixel–1 low-Sun LROC NAC controlled mosaic (NAC_ROI_MESSIER_LOA_E020S0469; S. M. Klem et al. 2014).
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: Best-fit I  d,273K vs. H, RA vs. H, and RA vs. I  d,273K for the craters (a) Giordano Bruno, (b) Tharp, (c) Wargo, and (d) Korolev Z. Note that the range of values for I  d,273K and RA is greater in panel (a) than in panels (b), (c), and (d).
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: Multiple data sets for the small highlands crater Donner M (32.°2 south, 98.°0 east, D = 8.0 km). (a) Mini-RF S-band CPR (color) modulated by total backscattered power (lightness). (b) Diviner two-parameter model RGB composite, overlaid on an NAC mosaic (see Table 3 in Appendix A for the list of frames used). (c) NAC close-up of the region marked with a white box in panels (a) and (b), showing the ponded areas of melt at the distal end of the flow. (d) Diviner two-parameter model RGB composite overlaid on Mini-RF S-band total backscatter. (e) Diviner two-parameter model best-fit I  d,273K.
Paper: Thermophysical Diversity of Young Lunar Crater Ejecta Revealed with LRO Diviner Observations
Authors: Cailin L. Gallinger, Jean-Pierre Williams, Catherine D. Neish, Tyler M. Powell, Catherine M. Elder, Rebecca R. Ghent, Paul O. Hayne, David A. Paige
Figure caption: Calculated sunset horizon angles around Mirzakhani, using (a) the standard algorithm of J. Dozier (2021) and (b) our updated version that incorporates the effects of surface curvature, as well as (c) their difference. The floor of Gibbs has horizon angles a maximum of 1.°5 lower and the upper northeast wall a maximum of ∼3° lower than they would if curvature was not accounted for. This translates to an onset of lunar night ∼12 LST minutes earlier in the corresponding thermal model during the critical twilight period.
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: Spectra and XRD results obtained by the Zoë rover contact instruments during the Yellow Cat, Utah 2022 October field campaign. XRD results were not obtained in real time for the rover to use. The blue spectrum is from an ASD spectrometer, and the red spectrum is from an FTIR spectrometer, both contact instruments. Flagged features (arrows) are Tetracorder identifications. The Fe2+ wollastonite is an identification of an Fe2+ absorption and not necessarily diagnostic of wollastonite, only that wollastonite was the reference spectrum. Features with no arrows were not evaluated by Tetracorder. Note that the carbonate features near 3.4 μm could be misidentified as organics if there are no carbonate reference spectra for this wavelength region in the Tetracorder expert system.
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: Tetracorder standard product showing the 1.9 μm water band position for Mars Reconnaissance Orbiter, Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) image cube FRT0000B385_07_IF164J_MTR3. Red and magenta indicate a very long 1.9 μm band position typical of sulfates. Examinations of absorptions indicate that the sulfate kieserite is present. Green and yellow indicate that absorptions in the 1.93 μm region are less diagnostic, consistent with phyllosilicates or other sulfates. Some montmorillonite is mapped in the green area near the upper right corner based on detection of a 2.2 μm feature. This image is a Tetracorder 5.27e1 standard product. Earlier expert system versions showed results with fewer wavelength bins.
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 simplified version of the data flow and how Tetracorder is integrated into the Zoë rover system. Data from the ASD spectrometer are collected and pushed to the ROS message bus. Tetracorder is started using an ROS wrapper program, and spectra are fed by updating a specpr file. Tetracorder is run using the “single-spectrum” mode for this operation, following the growing specpr file. After processing the spectra, Tetracorder writes the results to a results file, which is then read by the Science Planner, which analyzes the detections and generates guidance plans. The Vehicle Controller picks up the plans generated by the Science Planner and gives instructions to the drive mechanism to visit the next location.
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: Zoë rover in the field. For scale, the height of the communication antenna is about 3 m. Tetracorder runs on a Ubuntu Linux computer in the body of the rover, analyzing data in real time from an ASD spectrometer covering 0.35–2.5 μm. The spectrometer is located in the body under the solar panels and receives light via a fiber optic feed from a telescope mounted at the top of the mast. Here the telescope and mast camera are pointing down in front of the rover to analyze data as the rover autonomously drives forward. The view is to the southeast toward the La Sal Mountains near Moab Utah.
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: Image of the lunar surface with rover tracks showing that the disturbed soil is darker and different in color than the surface, indicating changes in grain size and/or composition with depth. Contrast has been increased from the original to show the tracks better. AS17-145-22206 Apollo 17, 1972 Hasselblad image taken post Extravehicular Activity EVA 3. The original film magazine was labeled D.
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) The nonscattering slab model used the derived MOPL from optical constants and is used in Model 2. (b) The random walk model uses the derived MOPL from optical constants and is used in Models 3 and 4.
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: Water absorption positions and widths derived from the USGS Library 06 (R. N. Clark et al. 2007) for materials measured in a dry environment. From R. N. Clark et al. (2016).
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: Reflectance and estimated absorption coefficients for kaolinite in the USGS Library 06 (R. N. Clark et al. 2007). The delta absorption coefficient Δk = kb –kc  = 234–57.3 = 176.7 cm−1. From the observed band depth in the reflectance spectrum, the MOPL = 24 μm.
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: Band depth of the hematite 0.9 μm band as a function of abundance and continuum reflectance (lightness of the gray rectangles). The relationship can be considered piecewise linear as long as one stays within the bounds where linearity is valid. The trend lines are derived from models.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Albedo snapshots at model time (a) 0001-10-03-00:00:00 and (b) 0001-110-25-00:00:00. Maps are zoomed in.
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Comparison between [O I] 557.7 nm and Hα 656.3 nm disk-integrated brightness observations and predicted brightnesses from modeled column densities. Black circles with vertical error bars show observations and their associated uncertainties. Red squares show predicted brightnesses from column densities averaged over 57 minutes (2°) of Ganymede’s orbit (the horizontal bars show the extent of the averaging window). The dashed gray horizontal line in each plot shows the detection threshold (the typical standard deviation of the observations). The [O I] 557.7 nm modeled brightness from the O2 atmosphere does not substantially change over the course of the eclipse, so we have shown its value as a solid horizontal dark gray line. The shaded gray regions in the background are the same eclipse boundaries shown in Figure 8. For both the [O I] 557.7 nm and Hα 656.3 nm observed brightnesses, the H2O contribution quickly drops below the detection threshold. Because the first two observations should exhibit some contribution from H2O above the detection threshold but do not appear significantly brighter than the rest of the eclipse observations, we concluded that there was no emission from a localized H2O atmosphere present in this data set. The model simulations in this figure are available in machine-readable format.(The data used to create this figure are available.)
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Simulation of Ganymede's [O I] 630.0 nm auroral emission from electron impact on O2 incorporating an updated electron energy distribution and emitting region. We used a Maxwell–Boltzmann electron energy distribution centered at 200 eV with a number density of 950 cm−3 (Saur et al. 2022), a typical O2 column density during eclipse, and we restricted the aurora emission to a Gaussian shape along the open/closed field line boundaries with an FWHM of 5° (Greathouse et al. 2022). The top high-resolution image shows the spatially confined emission from discrete elements 0.″01 wide, with brightnesses peaking above 10 kR at the limb. The bottom image shows this same image scaled down to the detector resolution and binning used in the Ganymede eclipse observations on 2021 June 8 UTC. We convolved this image with a two-dimensional Gaussian kernel with a FWHM of 0.″5, approximating typical seeing conditions on the summit of Maunakea. The white circle shows the size of the apparent disk of Ganymede. This simulation has equal electron flux for the northern and southern hemispheres and is therefore representative of the plasma conditions encountered by Ganymede at the plasma sheet midplane. The data in this figure are available in FITS format.(The data used to create this figure are available.)
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Time series of the ratio of the [O I] aurora brightness at 630.0 nm to the brightness at 557.7 nm. We have selected only data points for which the ratio signal-to-noise was greater than 2, which eliminated the observation at 14:15:28. Dashed horizontal lines show the modeled ratios for atmospheres of pure O, O2, H2O, and CO2. The ratios remain relatively constant over the duration of the observed eclipse and do not show evidence for the presence of significant H2O or CO2. The dark gray background region spanning most of the time range shows the 3 hr and 47 minute duration of the umbral eclipse. The light gray regions on either side are the approximately 8 minute duration of the partial umbral eclipse. The top axis shows the altitude of the Sun as observed from the summit of Maunakea. Sunrise on Maunakea occurred at 15:46 UTC, preventing observations of the end of the eclipse.
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Simulation of Ganymede’s O2 (top row) and H2O (bottom row) atmospheric column densities before, during, and after eclipse by Jupiter as observed from Earth. Each time step was averaged over 2° (57 minutes) of Ganymede’s orbit. The coordinate system is right-handed, measured counterclockwise along Ganymede’s orbit, with 0° pointing toward the Sun and 180° at the midpoint of the eclipse. Small-scale structures prominent in the H2O column densities are artifacts from the Monte Carlo simulation method. These simulations suggest that the H2O atmosphere, if present, collapses rapidly after the onset of the eclipse and recovers quickly after Ganymede emerges back into sunlight.(The data used to create this figure are available.)
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Simulated subsolar surface temperature (Leblanc et al. 2017) and number of simulated H2O molecules before, during, and after eclipse. Ganymede’s surface temperature dropped rapidly at the onset of eclipse, decreasing by 30 K in the first half hour and a further 5 K by the end of the first hour. The number of simulated H2O molecules in the simulation (proportional to the H2O number density) decreased by an order of magnitude within the first hour and remained relatively constant for the rest of the eclipse even though the temperature continued to decrease by an additional 7 K before the end of the eclipse. The data in this figure are available in FITS format.(The data used to create this figure are available.)