adsabs/AstroCLIMB huggingface dataset:
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) ShadowCam image M15308992S (Figure 4) colorized with model temperatures for the date the image was acquired (2023 January 29) and (b) the temperature profile across the floor. Location of image shown in Figure 1(b). The line in panel (a) shows the location of the temperature profile, and white arrow shows the location of an LRC in Figure 16. Black arrows in panel (b) denote the wall/floor contact locations.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) Shaded relief of Faustini crater and colorized with model temperatures during (b) the period of peak average temperatures of the crater floor near summer solstice (2024 February 2) and (c) winter solstice (2024 July 27), highlighting differences in the diurnal peak in illumination occurring on the equator-facing wall between the two seasonal extremes. Black temperature contours in panels (b) and (c) are 110 K (thick) and 50 K (thin), representing temperatures at which H2O and CO2 sublimation rates become negligible (e.g., N. Schörghofer & J.-P. Williams 2024).
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: Shaded relief maps of the Faustini floor colorized with (a) maximum and (b) average Diviner bolometric temperatures derived from 240 m pixel−1 polar stereographic gridded data from J.-P. Williams et al. (2019) and (c) time-averaged sublimation rate of water ice from N. Schörghofer & J.-P. Williams (2020). Elevation contours are −2710 and −2740 m from Figure 3.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) PSR area as a function of solar decl. (N. Schörghofer & R. Rufu 2023). The axial tilt of the Moon has dampened to smaller values over time. Therefore, the map can be interpreted as the relative age of PSR area. (b) Using a model of the Earth−Moon evolution (e.g., R. H. Tyler 2021), the map in panel (a) is converted to a map of maximum PSR age. Here, following N. Schörghofer & R. Rufu (2023), we use the integration of M. Farhat et al. (2022). The red outlines indicate PSRs with areas greater than 1 km2.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) Shaded relief colorized by elevation of a portion of the Faustini floor centered on the Upper unit area. (b) Elevation with the local slope removed. White arrows highlight broad, arcuate ridges that are smoother (lower VRM values), and have fewer craters, than their surroundings and circumscribe shallow depressions highlighted with dashed circles in panel (c), which may be the remnants of ∼2 km diameter impact craters.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: Modeled mean of the Faustini floor surface temperature during the primary KPLO mission (year 2023), where southern summer solstice is L  s  = 270° and southern winter solstice is L  s  = 90°.
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: Sample SWAN all-sky Lyα map for 2008 January 1 (bottom) and a corresponding scaled heliospheric model, with an added 43 R of isotropic Galactic background with charge-exchange lifetime asymmetry parameter A = 0.5 in both N and S hemispheres, indicated as A  N  = 0.5 and A  S  = 0.5 (top). Contour lines are 50 R apart. The small figure at the lower left illustrates the position of the Earth (E) in its orbit around the Sun with respect to the interstellar wind flow, indicated by an arrow, and upwind (u) and downwind (d) indicators.
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: Examples of various albedo (panels (a) and (b)) and land reflection/emission (panels (c) and (d)) models compared to bolometric temperatures for two regions near Wargo: 27.°355 north, 148.°730 west (panels (a) and (c)); and 27.°871 north, 148.°074 west (panels (b) and (d)) (see Figure 21 for locations). Panels (a) and (c) show data and models for a point on the west interior wall of Joule T, while panels (b) and (d) show data and models for a point on Joule T’s floor. Data points used in model fitting are shown in red, while daytime data are shown in gray and are included to evaluate the performance of the different upper boundary condition models. In panels (a) and (b) all models use the same land emission model (T. M. Powell et al. 2023), and in panels (c) and (d) all models use the same albedo model (E. J. Foote et al. 2020). Insets in panels (c) and (d) show nighttime surface temperatures with a smaller y-axis range to emphasize model differences.
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 (a) sunrise and (b) sunset horizon angles, as well as (c) the landview factor around the 14.3 km diameter crater Wargo (148.°6 west, 27.°7 north), which formed on the rim of the larger crater Joule T. Yellow markers indicate the location of corresponding diurnal temperature data shown in Figure 22.
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: F275W brightness scans (left) and Lomb–Scargle periodogram (right).
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: Images used for latitudinal scans in the FQ889N filter. All images are scaled over the same brightness range; the 2023 January image shows a saturated satellite transiting.