adsabs/AstroCLIMB huggingface dataset:
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Shear stress curves (scale bar: 50 kPa) vs. displacement (scale: 1 mm for runs at 5 × 10−7 m s−1 to 1 × 10−5 m s−1; 3 mm for 1 × 10−4 m s−1 and 2 × 10−2 m s−1) of HS STFOC tethers for temperature–velocity combinations tested under an applied normal stress of 100 kPa. The before and after labels indicate the condition of the central ice block: before is intact, while after is composed of gauge (due to cracking during high-velocity events).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Shear stress curves (scale bar: 50 kPa) vs. displacement (scale bar: 1 mm for runs at 5 × 10−7 m s−1 to 1 × 10−5 m s−1; 3 mm for 1 × 10−4 m s−1 and 2 × 10−2 m s−1) of STFOC tethers for temperature–velocity combinations tested under an applied normal stress of 100 kPa. The before and after labels indicate the condition of the central ice block: before is intact, while after is composed of gouge (due to cracking during high-velocity events).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: (a) Fracture network formed inside ice sample after shear testing at 199 K; STFOC fiber (175 K) imaged with an SEM, using secondary electrons. (b) The failure of the outer LCP layer (bottom right panel) and impact on bare fiber (bottom left panel).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: The behavior of the (a) central ice sample during shear testing depends on the temperature of the ice: (b) it behaves viscously at warmer conditions (left), and the tether cuts a groove (see inset); (c) at colder temperatures, the ice is pulverized.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: ICE #1 (panel (a)) and ICE #2 (panel (b)) velocity driving programs used during double-direct shear tests. Velocities, durations, and displacements for each driving program are provided in Table 1.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Shear stress curves (scale bar: 25 or 50 kPa) vs. displacement (scale: 1 mm for runs at 5 × 10−7 m s−1 to 1 × 10−5 m s−1; 3 mm for 1 × 10−4 m s−1 and 2 × 10−2 m s−1) of control samples of ice for temperature–velocity combinations tested under an applied normal stress of 100 kPa.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Damage to the outer layer of STFOC (panels (a)−(c)) and HS STFOC (panels (d)–(e)) during testing to accommodate shearing, with kinks observed at lower temperatures (T = 250 K) and low-velocity runs (panel (d)).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Example of (a) a single velocity step used to determine rate-state friction parameters (a, b) and (b) a slide-hold-slide that consists of relaxation of friction on the onset of hold and a peak when sliding is resumed. Here, D  C  is the critical slip distance needed for the system to evolve from one steady-state friction to another; parameters μ, a, and b are experimentally determined coefficients; and V 1, V 2 are sliding velocities. The examples are from polycrystalline ice sliding between two granite blocks (McCarthy et al. 2017).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: RIL recorded for HS STFOC tether at (a) ∼250 K, (b) 237 K, (c) 220 K, (d) 199 K, (e) 150 K, and (f) 120 K, highlighting variations in signal (±0.5 to ∼ ±7.0 dB) during velocity ramps.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: RIL recorded for STFOC tether at (a) 195 K and (b) 255 K.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: (a) Pencil wrap tests for the HS STFOC tether with OP735 optical power meter: (b) before and (c) after recalibration by manufacturer to address a −30 dB tare; relative dB loss is accurately replicated, indicating that prior measurements are accurate.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: (a) RIL recorded for STFOC and HS STFOC cables at 253, 220, and 77 K over 3 days, and (b) insertion loss over the temperature range of 100–273 K, highlighting the negligible drop in signal (<1.75 dB) with temperature and time.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Temporal response of Io’s atmospheric oxygen (red) and sodium (orange) following ingress. Diamonds were measured using LBT/PEPSI following the 2019 April 24 ingress. Circles show APO/ARCES measurements on 2018 March 20. The concurrent SO and SO2 molecular response reported in millimeter-wavelength ALMA data by de Pater et al. (2020) is shown in blue associated flux density in janskys on the right axis (see their Figure 5). Squares show the only spectrum obtained from APO on 2021 June 9. Data points show summed Na doublet emission, while the [O I] 6364 Å counterpart to 6300 Å is not included, since it falls out of the PEPSI bandpass in one LBT eye. Horizontal error bars show the integration time, and the data points are located mid-exposure.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Io’s [O I] 6300 Å line emission amidst Jupiter scattered light on 2018 March 20 with APO/ARCES (left) and 2019 April 24 with LBT/PEPSI (right). The red-to-blue color scheme shows the elapsed time in shadow. Scattered-light levels increase as Io approaches the Jovian limb, and dotted lines show the fitting of a background spectrum to this component. The lower panels show the residual after scattered-light subtraction. Gaussians are fit to Io’s emission line, which Doppler shifts slightly in time. The observing geometry for each date appears in Figures 1 and 2.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Io–Jupiter geometry during the LBT/PEPSI measurement on 2019 April 24. The circle around Io indicates PEPSI’s field of view.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Diagram and guider frame images showing the ARCES aperture (red box) during ingress on 2018 March 20.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Same as Figure 3 but showing the Na D line region with spectra in the top panels consecutively offset by 12 kR Å–1 for clarity. No offset is applied to the blue spectrum, which is the last observation taken shortly before Io was occulted by Jupiter’s limb.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Electron impact excitation frequencies on an atomic gas for all observed electronic transitions. Alkali impact cross sections are taken from Stone & Kim (2004). Oxygen impact cross sections are taken from Barklem (2007).
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Sodium D emission (top) and line ratios (bottom) as a function of duration in sunlight postegress. Symbols indicate different observing dates following the Figure 6 legend. The top panel shows the summed D1 + D2 emission. Io’s heliocentric Doppler shift causes increased sunlight to resonantly scatter in the atoms, so a static column, shown in blue, will brighten in time. A constant column density cannot reproduce the data points, however, suggesting that Io’s Na density is rebuilding after the eclipse phase. The optically thin line ratio of 1.75 is shown in the bottom panel, where 15 minute binned data (black) become optically thick after 45 minutes, confirming growth in the Na abundance.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Curve-of-growth models for sodium D1 and D2 emission (top) and their line ratio (bottom) as a function of time on 29 October 2021. Color coding indicates the time past egress. Measured emissions and line ratios are plotted vs. their column density inferred from each metric. The opacity treatment here derives from Brown & Yung (1976) and is interpolated to an assumed gas temperature of 1600 K. Incident sunlight at the D1 and D2 wavelengths is changing in time due to Io’s heliocentric Doppler shift. Hence, there is a vertical spread in the top panel curve-of-growth lines; i.e., emission changes with time, even if the column density is fixed.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Potassium D line emissions seen just preceding egress with Keck/HIRES on 2018 August 7. The top panel shows nine raw spectra that have the Jovian scattered light subtracted off in the middle panel. The bottom panel shows the median of these frames after coaligning for Io’s changing Doppler shift. The stronger D2 line at 7665 Å is partially absorbed by telluric O2, making the D2/D1 line ratio lower than the statistical value of 2.0.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Effects of the changing torus latitude on Io’s disk-averaged emission from the [O I] red line doublet. Filled symbols represent observations following ingress, and open symbols represent observations preceding egress. The blue curve shows the approximate plasma density of the ribbon and warm torus regions based on Juno radio occultations.
Paper: Io’s Optical Aurorae in Jupiter’s Shadow
Authors: Carl Schmidt, Mikhail Sharov, Katherine de Kleer, Nick Schneider, Imke de Pater, Phillip H. Phipps, Albert Conrad, Luke Moore, Paul Withers, John Spencer, Jeff Morgenthaler, Ilya Ilyin, Klaus Strassmeier, Christian Veillet, John Hill, Mike Brown
Figure caption: Sodium D line ratios following ingress. A ratio of 2.0 is expected for optically thin emission, and only the ratio nearest ingress on 2019 April 24 deviates from this value with appreciable significance (σ = 2.5; cf. Figure 4).
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: X-ray diffraction patterns showing temperature-quenched samples at high pressure after their final heating event (first row), and materials after decompression to 1 bar (second row). Patterns shown along columns and their respective heating temperatures are from experiments Mg50-2 (2450 K) and Mg90-1 (<1000 K) respectively (Table 1). Phases marked “Fp” represent any phase of composition (Mg1−x Fe x )O, as in many cases after heating the exact composition is unknown since the sample has reacted with hydrogen and lost some amount of Fe through reduction. The starred peaks in pattern (d) are unassigned. These peaks did not exist after heating at high pressure but appear when the sample was pressure quenched to 1 bar. Therefore, they are not related to the high-temperature reactions we focus on in this paper. They are likely from possible conversions of the sample during pressure unloading.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: Cartoon demonstrating possible implications of the chemical reactions explored in this work. Of particular importance is the link between the atmosphere and interior showing that in large exoplanets the oxidation of the atmosphere may stem from the reduction of the interior. It also demonstrates how super-Earths formed through atmospheric loss from a sub-Neptune may retain significant amounts of their primordial hydrogen stored in the metal part of the core as an alloy component or the silicate part of the core as H2O.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: Comparison of the volumes per Fe atom (V/Z) of Fe and Fe-H phases observed in our experiments and the volume previously reported at 300 K. Both the fcc and dhcp FeH x  phases observed in this study (red and green circles, respectively) show V/Z consistent with 1:1 stoichiometric FeH (colored curves). Equations of state for hcp Fe, fcc FeH, dhcp FeH, and FeH2 are from Dewaele et al. (2006), Narygina et al. (2011), Pepin et al. (2014), and Pepin et al. (2014), respectively.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: 2D X-ray diffraction map of the (Mg0.5Fe0.5)O sample heated in a pure H medium at 23 GPa and 2450 K. The mapping was conducted after the recovery of the sample at 1 bar and 300 K inside a diamond-anvil cell. The green dashed circle indicates the hot spot center. (a) Fe content in (Mg,Fe)O was calculated from the unit-cell volume using a linear relationship between the volume and the Fe content (Jackson & Rigden 1996). (b) Intensity ratio between Fe metal (bcc converted from FeH x ) and (Mg,Fe)O. (c) Intensity ratio between brucite and (Mg,Fe)O.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: X-ray diffraction patterns from run Hem-4 (Table 1) taken at 38 GPa (a) before heating, (b) during heating (∼1850 K), and (c) after heating. The upper pattern in panel (b) is during the first heating event, and the lower pattern is during the final heating event. The vertical tick marks below each integrated diffraction pattern represent the diffraction peak positions of the various observed mineral phases. Expected peak positions are calculated by combining the experimentally determined crystal structure and equation of state for a given material. Initially both FeO and FeH x  were formed, but after four heating events only FeH x  was observed in diffraction patterns.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: Schematic diagram of the sample loading in this study. Note that the sample spacers allow for hydrogen layers to form during gas loading. The hydrogen layers then insulate the sample foil from the diamond anvils. Particles of gold and ruby were placed to the side of the sample chamber to avoid sample contamination by potential chemical reaction.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: The unit-cell volume of ferropericlase before (stars) and after (circles) heating and subsequent decompression to 1 bar for heating runs Mg50-2 (black) and Mg90-1 (yellow). Also shown are compositional curves for the pressure–volume relationship of (Mg,Fe)O with various Fe contents: 1FeO from Fischer et al. (2011), 2(Mg,Fe)O from Fei et al. (2007), and 3MgO from Speziale et al. (2001).
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: Pressure–volume data for brucite formed in run Mg90-3, along with the 1 bar measurement from run Mg50-2 (Table 1). The data points were measured at 300 K. We also show the equation of state from Xia et al. (2015) at 300 K for comparison.
Paper: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths
Authors: H. W. Horn, V. Prakapenka, S. Chariton, S. Speziale, S.-H. Shim
Figure caption: Pressure−temperature (P − T) conditions of the LHDAC experiments in this study (data points) shown with the melting curves of relevant materials: MgO (Kimura et al. 2017), (Mg0.72Fe0.28)O (Fu et al. 2018), FeO (Boehler 1992), FeH x  (Sakamaki et al. 2009), and H (Gregoryanz et al. 2003). No experiment in this study exceeded the melting temperature of MgO, while most were near or above the melting temperature of FeO and FeH x . All experiments were conducted above the melting temperature of hydrogen.
Paper: The Distribution of Molecular Water in the Lunar South Polar Region Based upon 6 μm Spectroscopic Imaging
Authors: William T. Reach, Paul G. Lucey, Casey I. Honniball, Anicia Arredondo, Erick R. Malaret
Figure caption: Water profile through Moretus. The top panel, aligned with the lower panel along the horizontal axis, shows a two-dimensional spectrum from a single pointing of the spectrometer. The shades of blue indicate the emissivity, relative to the continuum fit, from 0.997 (no color) to 1.019 (dark blue). The thick, horizontal dark band is the 6.1 μm water feature. The lower panel shows spatial profiles of the 6.1 μm feature summed brightness W (blue) and the continuum (black). The profiles extend from the northernmost edge of Figure 2, just right of the left-hand edge, traversing several labeled features including the “wet ridge” of high H2O content, and the central peak of the Moretus crater. The spatial structures are significant local enhancements in H2O content, and they are superposed on a gradual trend that decreases from north to zero (immeasurably low) at the limb beyond the permanently shadowed crater Cabeus. In the top panel, the horizontal stripes are electronic artifacts on the detector triggered by saturated pixels, and the small white patch near 101″ offset and 6.08 μm wavelength is due to a defect on the detector surface (mentioned in the Figure 2 caption).
Paper: The Distribution of Molecular Water in the Lunar South Polar Region Based upon 6 μm Spectroscopic Imaging
Authors: William T. Reach, Paul G. Lucey, Casey I. Honniball, Anicia Arredondo, Erick R. Malaret
Figure caption: (a) LRO Wide Angle Camera image of the southern limb of the Moon, oriented with celestial pole at the top as appropriate for 2022 February 17, with a lunar coordinate grid overlaid and an outline of the region observed with SOFIA (blue lines). (b) Color rendition of SOFIA water and continuum emission. The color image combines the 6 μm continuum surface brightness (green) and the 6.1 μm water feature strength W (blue). The diagonal empty regions on the water image mask a defect on the surface of the detector that leads to significantly higher noise. (c) The 6 μm continuum surface brightness, together with a color bar in Jy pixel−1, for a pixel size of 0.″768. (d) The 6.1 μm integrated water band strength, W, defined in Equation (1).