adsabs/AstroCLIMB huggingface dataset:
Paper: Temperature-related Variations of 1064 nm Surface Reflectance on Mercury: Implications for Space Weathering
Authors: Ariel N. Deutsch, Gregory A. Neumann, Mikhail A. Kreslavsky, Petr Pokorný, Jose M. Martinez Camacho, David Trang, Noam R. Izenberg, Brett W. Denevi, Anna Galiano, Gianrico Filacchione
Figure caption: Northern hemisphere cylindrical maps of (left) 1064 nm surface reflectance from our newly empirically corrected MLA data and (right) I/F reflectance from the LOI MDIS map, resampled to the 1° × 1° resolution of our MLA map using a nearest-neighbor interpolation. Maps are shown for (A) and (B) all northern surfaces (areas in white correspond to areas with no data), (C) and (D) SP surfaces (Denevi et al. 2013), and (E) and (F) surfaces outside of the SPs. Note: a nearest-neighbor interpolation was used to average nearby MLA tracks and make them more visible in this figure.
Paper: Temperature-related Variations of 1064 nm Surface Reflectance on Mercury: Implications for Space Weathering
Authors: Ariel N. Deutsch, Gregory A. Neumann, Mikhail A. Kreslavsky, Petr Pokorný, Jose M. Martinez Camacho, David Trang, Noam R. Izenberg, Brett W. Denevi, Anna Galiano, Gianrico Filacchione
Figure caption: Map of modeled MST over the course of a full Mercury solar day at 1° × 1° resolution. The 50 K contours are shown in white lines.
Paper: Temperature-related Variations of 1064 nm Surface Reflectance on Mercury: Implications for Space Weathering
Authors: Ariel N. Deutsch, Gregory A. Neumann, Mikhail A. Kreslavsky, Petr Pokorný, Jose M. Martinez Camacho, David Trang, Noam R. Izenberg, Brett W. Denevi, Anna Galiano, Gianrico Filacchione
Figure caption: The 1064 nm median surface reflectance (R  s ) during the first 3 months of MESSENGER operations in 20 km × 1° bins, (A) before and (B) after our empirical corrections. Corrections included exclusions of (1) R  s  > 0.6; (2) anomalous time interval unit readings, where the low-threshold (PULSE_WIDTH_LO) and high-threshold (PULSE_WIDTH_HI) values are separated by <1 ns; (3) data obtained from above a given range (R max) or emission angle (θ; areas to the right of or above the vertical dotted–dashed lines, respectively); and (4) data lying above the pulse parameter P = R max * tan(θ), shown by the dashed line, where range > R min.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: This figure depicts the processing steps as a tutorial example for the corresponding steps in the text above. Step 1 begins with the Voyager frame (vg-iss-2-u-c2683649) used in Figure 4(A) to produce Figure 4(B) in the main text.
Paper: Temperature-related Variations of 1064 nm Surface Reflectance on Mercury: Implications for Space Weathering
Authors: Ariel N. Deutsch, Gregory A. Neumann, Mikhail A. Kreslavsky, Petr Pokorný, Jose M. Martinez Camacho, David Trang, Noam R. Izenberg, Brett W. Denevi, Anna Galiano, Gianrico Filacchione
Figure caption: Median surface reflectance trends for SPs (black) and non-SPs (purple) plotted in 1° latitudinal bins, derived from (A) MLA R  s  and (B) MDIS I/F values.
Paper: Temperature-related Variations of 1064 nm Surface Reflectance on Mercury: Implications for Space Weathering
Authors: Ariel N. Deutsch, Gregory A. Neumann, Mikhail A. Kreslavsky, Petr Pokorný, Jose M. Martinez Camacho, David Trang, Noam R. Izenberg, Brett W. Denevi, Anna Galiano, Gianrico Filacchione
Figure caption: Modified from Gleiter (1989). Experimental measurements of the mean grain diameter (nm) of nanophase Fe0 after annealing for 10 hr under various heating temperatures. The shaded areas show the extent of the MST for the Moon and Mercury.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: (A) Voyager frame (vg-iss-2-n-c1139617) of Triton. The black dots are control points. (B) The same as (A), but reprocessed using a nonuniform blind deconvolution to reduce camera motion blur.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: (A) Voyager frame (vg-iss-1-j-c1639100) of Sengen Patera and the surrounding area on Io. The black dots are control points. (B) The same as (A), but reprocessed using a nonuniform blind deconvolution to reduce camera motion blur.
Paper: Categorization of Spatial and Temporal Ejecta Outcomes in Binary Systems Based on Variations of the Didymos System
Authors: Jennifer N. Larson, Yanga Fernandez, Gal Sarid
Figure caption: Examples of each provenance map category showing ejecta on the target object (the red star signifies the impact location): (a) evenly spread, (b) local, (c) equator, (d) hole opposite impact site, and (e) cluster opposite impact site. The circles in (d) and (e) respectively highlight the absence of particles and the cluster of particles that distinguish these categories.
Paper: Categorization of Spatial and Temporal Ejecta Outcomes in Binary Systems Based on Variations of the Didymos System
Authors: Jennifer N. Larson, Yanga Fernandez, Gal Sarid
Figure caption: A comprehensive view of the system configuration. General parameters that are consistent in all simulations are represented by blue labels, while the red underlined labels represent parameters that we vary throughout this study. While this is only displaying the configuration for the ellipsoidal case, the setup and orientation of the secondary with respect to the impact sites still applies in the cases of the shape model and the spherical targets.
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: Crater size–frequency distribution for Titania's cratered terrain as mapped by Plescia (1987), Strom (1987), and Kirchoff et al. (2022). Figure modified from Kirchoff et al. (2022).
Paper: Cratering and Tectonic History of the Largest Uranian Satellite, Titania: New Insights Enabled by Image Reprocessing
Authors: Erica Nathan, James Head, Christian Huber
Figure caption: (A) Voyager frame (vg-iss-1-j-c1640354) taken in 1979 of Shu Crater (the largest bright crater in the image) and the surrounding area on Ganymede, cropped and contrast-adjusted. The black dots are control points. (B) The same as (A), but reprocessed to reduce camera motion blur. Note that even small-scale features (small bright craters, grooves, and crater rays) are now recovered. (C) Juno image (NASA/SwRI/MSSS: JNCE_2021158_34C00002_V01; ∼1–2 km pixel−1) from 2021 June 7 of a similar region.
Paper: Titan’s Atmospheric Albedo Asymmetry and Seasonal Variability Observed through the Cassini Imaging Science Subsystem
Authors: C. Snell, D. Banfield
Figure caption: The location and orientation of the NSA boundary changes over time and shows a seasonal dependence. Results are shown for both the initial major NSA boundary where brightness increases in the northward direction (blue) and for the new reversed boundary that arises near the end of the Cassini mission (red). The top panel shows the amplitude of the tilt with respect to the solid body north pole, the middle panel shows the mean latitude of the NSA boundary, and the bottom panel shows the offset of the azimuth from the subsolar longitude. The dashed line in the bottom panel represents a best fit to the azimuth offset if it was fixed in inertial space. Deviations from this line in the data may indicate that seasonal or other atmospheric phenomena affect the tilt azimuth.
Paper: Titan’s Atmospheric Albedo Asymmetry and Seasonal Variability Observed through the Cassini Imaging Science Subsystem
Authors: C. Snell, D. Banfield
Figure caption: Top: image W1536388236_1 after reduction of noise and banding artifacts in units of I/F. Only the pixels considered useful to the analysis are shown, i.e., parts of the disk with emission angle <85° and incidence angle <87°. Middle: the surface brightness model (in I/F) produced when the empirical photometric model is interpolated for the incidence and emission angles of each pixel in the image. Bottom: the resulting flattened image after the calibrated image is divided by the brightness model.
Paper: Titan’s Atmospheric Albedo Asymmetry and Seasonal Variability Observed through the Cassini Imaging Science Subsystem
Authors: C. Snell, D. Banfield
Figure caption: Top: image N1496574260_1 after limb-brightening reduction. Middle: the brightness gradient in the northward direction (north is to the lower right in this image). The locations of gradient extrema, as determined from polynomial fits, are indicated on the images, where black points indicate extrema determined to belong to a strong edge (used for subsequent analysis) and white points indicate extrema belonging to weaker edges (not used). Bottom: a few slices from the above image gradient, demonstrating the degree-10 polynomial fitting.
Paper: Titan’s Atmospheric Albedo Asymmetry and Seasonal Variability Observed through the Cassini Imaging Science Subsystem
Authors: C. Snell, D. Banfield
Figure caption: The relative brightness by latitude after limb-brightening reduction is shown throughout the Cassini mission. Brightness data were interpolated through the time gaps between images. This figure shows the NSA boundary move south and eventually fade, while a new reversed boundary arises slightly to the north. Due to the image geometries used in this study, the data near the poles were often low quality or unavailable throughout the mission.
Paper: Titan’s Atmospheric Albedo Asymmetry and Seasonal Variability Observed through the Cassini Imaging Science Subsystem
Authors: C. Snell, D. Banfield
Figure caption: The empirically determined photometric model for Titan in the 889 nm methane band filter, with I/F shown as a function of incidence and emission angles.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: L’LORRI photometry of the DART impact event. The image inset in the upper right corner shows the placement of the synthetic photometry apertures on a L’LORRI image of the Didymos system shortly after the impact: the green circle is used to determine the “target” signal (3-pixel radius, projecting to 1113 km at Didymos), after subtraction of a background signal derived from the measured level in the annular regions defined by the cyan (inner radius is 10 pixels) and magenta (outer radius is 15 pixels) circles. The large dip in the photometry near 1 hr post-impact is caused by the fast ejecta moving into the background annulus, but by ∼6 hr after impact all the fast ejecta had exited the background region and the signal settled down to a steady-state value. The mean count rates and V-mag values of pre-impact Didymos (dashed blue line), the fast+slow ejecta (dashed orange line), and the slow ejecta (dashed red line) are also indicated. A dashed pink vertical line indicates the impact time of the DART spacecraft into Dimorphos, as viewed from Lucy. See the text for further discussion.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: Composite of five L’LORRI images of the Didymos system, each with an exposure time of 9.9 s, after subtraction of the pre-impact image of Didymos to better reveal the ejecta morphology. The image is displayed using an ASINH intensity stretch (ranging from −1 to 1000 DN) and a cubehelix color scheme. The mid-exposure time was 897 s (14 minutes 57 s) after the DART impact. The frame is centered on Didymos; each pixel subtends 371 km at Didymos. Projected directions to the Sun (yellow), Didymos’s heliocentric velocity (cyan), and the DART spacecraft velocity (red) are shown; the compass shows celestial north (N) and east (E). Slower-moving dust is concentrated near the location of Didymos, but there is also a shell of early-released, fast-moving (up to ∼3.6 km s−1 projected speed) ejecta that is more concentrated to the east. Other objects in the field are stars.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: The solar spectrum is plotted near the location of the sodium D lines: D2 has λ = 5889.95095 Å, and D1 has λ  =  5895.92424 Å. The solar scattering efficiencies, or g-factors, of any sodium atoms in the DART ejecta depend strongly on the heliocentric radial velocities (﹩\dot{r}﹩) of those atoms. Sodium atoms ejected toward the Sun (i.e., with negative values of ﹩\dot{r}﹩) absorb sunlight at wavelengths longward of the corresponding solar lines, while atoms ejected away from the Sun (i.e., with positive values of ﹩\dot{r}﹩) absorb sunlight at wavelengths shortward of the corresponding solar lines. ﹩\dot{r}﹩ for Didymos itself is −4.487 km s−1, and this would be the effective ﹩\dot{r}﹩ for sodium atoms ejected perpendicular to the Sun−Didymos line. For sodium atoms ejected from Didymos toward the Sun at a speed of 1.8 km s−1, the effective ﹩\dot{r}﹩ is  −6.287 km s−1; the dashed vertical lines show where the absorptions for the D lines would be for this case. Sodium atoms ejected from Didymos away from the Sun at a speed of −4.487 km s−1  have an effective ﹩\dot{r}﹩ of 0 km s−1.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: L’LORRI photometry spanning from 180 s before to 400 s after the time of the DART impact event. Points from the first 7 minutes (3 minutes before to 4 minutes after the impact) were derived from 0.9 s exposures taken at 1 Hz cadence. The other points were derived from 4.9 s exposures taken every 13 s. The fastest-moving ejecta start to leave the target aperture (3-pixel radius) at ∼305 s after the impact, as indicated by the green arrow. The mean count rates and V-mag values of pre-impact Didymos (dashed blue line), the fast+slow ejecta (dashed orange line), and the slow ejecta (dashed red line) are also indicated. A dashed pink vertical line indicates the impact time of the DART spacecraft into Dimorphos, as viewed from Lucy. See the text for further discussion.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: Model spectra for the DART ejecta only (i.e., not including light from Didymos or Dimorphos), including both continuum and sodium line emissions. The black line is the spectrum (at a resolving power of ∼250) assuming that all of the emission associated with the fast ejecta is produced by the sodium D lines. In that case, the line-integrated emission totals to an observed flux of 1.9 × 10−11 erg cm−2 s−1, and the V-mag would be 14.274. The red line is the spectrum (again at a resolving power of ∼250) assuming that there is no atomic line emission (i.e., all the emission is scattered sunlight from dust grains in the ejecta), in which case V = 13.671. The magenta curve shows the relative QE of L’LORRI, whose peak is 0.675 at a wavelength of 5660 Å.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: L’LORRI photometry of the ejecta only (i.e., pre-Didymos signal has been subtracted) starting 50 s before the time of the DART impact event and ending 100 s after the impact. The mean count rates for the pre-impact period (dashed blue line), for the fast+slow ejecta peak (dashed orange line), and for the post-impact mean signal of the slow ejecta (dashed red line) are also indicated. A dashed pink vertical line indicates the impact time of the DART spacecraft into Dimorphos, as viewed from Lucy. See the text for further discussion.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: A composite pre-impact Didymos image produced by averaging 280 of the 9.9 s pre-impact images, cropped to 128 × 128 pixels centered on Didymos, and using an ASINH intensity stretch ranging from −0.3 to 180 DN. The compass shows the directions of celestial north (N) and east (E), and the scale bar is 30″ across.
Paper: Lucy Observations of the DART Impact Event
Authors: H. A. Weaver, J. M. Sunshine, C. M. Ernst, T. L. Farnham, S. Mottola, J. R. Spencer, S. Marchi, N. Dello Russo, O. Barnouin, H. F. Levison, K. S. Noll, C. B. Olkin, T. S. Statler, A. F. Cheng, E. G. Fahnestock, A. Fitzsimmons, M. M. Knight, J.-Y. Li, N. A. Moskovitz, C. A. Thomas, N. L. Chabot, A. S. Rivkin
Figure caption: L’LORRI photometry is compared to the ATLAS photometry, zoomed in near the time of the DART impact event. Although the signal rise times are similar for the L’LORRI and ATLAS data, the amplitude of the increase is significantly larger for ATLAS. See the text for further discussion.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Left panels: ACB cloud opacities for MYs 32–36 as a function of LTST, averaged across bins of 30 minute lengths. Individual observations are indicated by the colored markers. There does not appear to be any meaningful variability, either across the whole day or comparing AM and PM values. The apparent drop-off in opacities near sunrise and sunset is an illumination effect caused by the limitations of our simplified radiative transfer model rather than an actual change in opacity. Right panels: ACB cloud opacities for MYs 32–36, averaged across 5° solar longitude bins. Individual observations are indicated by the colored markers. There is no clear intraseasonal variability, though MYs 35 and 36 do have slightly higher opacities near L s = 140°.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Derived opacities for all movies with visible clouds, combining data from this paper, Moores et al. (2015), and Kloos et al. (2016, 2018). The cyan circles are ZMs, and the black triangles are SHMs. The yellow shaded regions indicate the solar longitude ranges of the ACB, and the red shaded region is the MY 34 GDS event. We can see that ZMs generally have higher opacities than SHMs, particularly outside of the ACB season, consistent with their greater sensitivity to clouds. The notable exception is MY 33, where the SHMs consistently recorded opacities that were much higher than those seen by Curiosity in other years.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: A comparison between the surface reflectances observed at Gale by the MRO Context Camera (left; Dickson et al. 2023) and water-ice optical depths observed by MARCI (right). The highest MARCI optical depths clearly correspond to the dark sand patches seen by CTX. These sand patches are bright in the UV (where both the MARCI and EXI retrievals operate), which will result in anomalously high optical depths if the surface reflectance maps used by the retrievals are of insufficient resolution. Low-altitude fogs have never been observed in Gale, so it would be surprising if the values measured by MARCI/EXI were real and not an artifact of the low-resolution surface reflectance maps.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: ACB cloud opacities for MYs 34–36, averaged across bins of 30 minutes (left) and 5° solar longitude (right). Individual observations are indicated by the colored markers. Here, we have removed the phase function correction, as well as all points taken at scattering angles <70°. The smaller number of data points in each bin compared to Figure 13 makes a robust analysis more difficult, but there is no obvious diurnal or seasonal variability. This suggests that the observed low variability in Figure 13 is real and not an effect of the assumptions we made when applying the phase function correction.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Comparisons between EXI and MSL water-ice retrievals for MY 36 as a function of solar longitude (top) and LTST (bottom). As with the MARCI data, the MSL retrievals are flatter (in solar longitude) and lower magnitude than the EXI retrievals, though the EXI data are subject to the same surface reflectance problem as the MARCI data, as the ZM averages are higher than the SHM averages. However, we do see that EXI does not appear to observe any meaningful diurnal variability during the ACB season, other than a potential slight enhancement in the very early morning and late evening. This low diurnal variability is consistent with what we observe with MSL.
Paper: Five Mars Years of Cloud Observations at Gale Crater: Opacities, Variability, and Ice Crystal Habits
Authors: Conor W. Hayes, Jacob L. Kloos, Alex C. Innanen, Charissa L. Campbell, Haley M. Sapers, John E. Moores
Figure caption: Examining interannual variability in the scattering phase function by comparing the AM and PM phase functions across MYs 34–36. We see relatively close agreement between the three MYs for which a phase function was derived, leading us to conclude that there is no meaningful interannual variability in the shape of the phase function.