adsabs/AstroCLIMB huggingface dataset:
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: Photographs and a drawing of the earlier prototypes of LISTER.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: Left: an overview drawing of the pneumatic subsystem. Right: a drawing of the pneumatic manifold.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: Drawings of the two major hardware components (the avionics box and the deployment mechanism). The subsystems of the deployment mechanism are color-coded (the middle diagram). The lander interface structure is in magenta. The pneumatic subsystem is in green. The deployment subsystem is in blue. The sensor subsystem is shown in a separate diagram (right).
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: Top: a drawing of the exterior of the sensor subsystem. Bottom: a drawing of the internal construction of the needle sensor and the gas nozzle. The dimensions are in millimeters.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: Drawings of the mechanism for spooling and straightening the S.S. tube of the deployment subsystem.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: A graph of LISTER’s sensor depth vs. time for operation 8. The zigzags indicate occurrences of the dithering maneuver.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: Conceptual drawings describing the dithering maneuver of LISTER.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: A series of snapshots obtained by Argus 8 during operations 4 (A–E) and 5 (F). The depth of the needle sensor is indicated by the red dot in the graph in the upper left corner of each photo. Photo A shows the very beginning of the excavation. Photo B captured the eruption plume of fine-grained reflective particles that preceded the first explosion captured in photo C. Photo D captured the eruption plume that preceded the second, larger explosion. Photo E captured the projectiles ejected by the second explosion. Photo F was taken during operation 5.
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: A photograph of the lunar surface below the lander obtained by camera SFL1 of the SCALPSS payload toward the end of the surface mission. See Figure 14 for the camera position and the field of view. The green arrows point to lithified materials exposed on the surface. They are likely regolith breccia. Courtesy of the SCALPSS team (O. K. Tyrrell et al. 2022).
Paper: The Lunar Instrumentation for Subsurface Thermal Exploration with Rapidity (LISTER) on Blue Ghost Mission 1 to Mare Crisium. I. Pneumatic Excavation of Regolith
Authors: S. Nagihara, K. Zacny, P. Ngo, L. Sanasarian, R. Misra, M. Zasadzien, V. Sanigepalli, M. Schmitt, A. Wang, C. Ladd, A. Shmavonian, P. Ng, Y. Hwang, W. Garcia, J. Knorr, R. Tuanuma, T. Thomas, H. Jung, X. Estey, T. Colenbrander, X. Fries, J. Emery, N. Jeevanjee, C. Castle, N. Sadagopan, T. Heiman, E. Killian, N. Steele, Y. Matsuyama, G. Paulsen, M. Grott, J. Knollenberg, T. L. Hudson, S. E. Smrekar, M. A. Siegler
Figure caption: A top-down view drawing of the positions of the below-deck cameras used to monitor LISTER’s operations. Argus 8 and 9 are video cameras operated by Firefly Aerospace. SFL1 is a wide-angle, short-focus black-and-white camera of the SCALPSS payload. The blue dashed lines indicate its field of view.
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: A portion of the 1:7,000,000 scale geological map of Pluto (O. L. White et al. 2022), centered on Kiladze at 212﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9E, 28﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4N. North is up. The rim of the crater is mapped with a depressed margin. Black lineations indicate fault lines. The dotted area indicates high-albedo terrain of East Tombaugh Regio. The yellow dashed line indicates the approximate crest of the broad annular ridge that contains the Sputnik impact basin. Unit labels are as follows: hur = rough, undulating highland material; ra = ridged arcuate material; rb = bladed arcuate material; rs = subdued ridged material; lp = lowland plains material; c = crater material; pi = pit material.
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: (a) Transects to extract the elevation profiles of the Kiladze area are shown in the upper panel. The transects intersect at the peak of the central rise in the smooth terrain. (b) Elevation profiles for the four transects are in the lower panel, with arrows indicating the rise in the smooth-textured material presumed to have slumped into the crater from a collapse of the southwestern wall. The vertical scale is in meters. AA′, BB′, CC′, and DD′ are the four transects.
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: Comparison of Kiladze and the similar-sized Giclas crater on Pluto. A 3D visualization of the base map (a) and the TIN map (b) at the Kiladze area and the base map (c) and a DEM (d) at Giclas crater and its surroundings. The 3D visualization of the monochromatic base map at 300 m pixel−1 spatial resolution (P. M. Schenk et al. 2018) was rendered vertically to elevation model data and the TIN.
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: Giclas crater with a diameter of ∼46 km. (a) The highest-resolution base map image of the region around the crater. Yellow transects to extract the elevation profiles of the crater, shown in (c). The transects intersect at the peak of the central rise. (b) Two-dimensional visualization of the DEM of Giclas crater. (c) Elevation profiles for the four transects on (a), with arrows indicating the central peak of the crater. Vertical scale in meters. AA′, BB′, CC′, and DD′ are the four transects.
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: Geologic resemblance of calderas on Pluto and Mars. (a) The panchromatic base map (P. M. Schenk et al. 2018) of the Kiladze structure on Pluto, as observed by the New Horizons flyby in 2015 July, and (b) a panchromatic image of Siloe Patera within the Arabia Terra region on Mars, as observed by an instrument on board the Mars Reconnaissance Orbiter.
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: (a) The 0 km contour (black line) overlaid on the elevation model used for calculation of the caldera volume. (b) The proposed outline (with much stronger ammoniated water ice) of deposit (black line) overlaid on the compositional map modified from A. Emran et al. (2023a). The differences in the orientation of the outline and compositional units in this figure vs. Figure 1(d) are due to the image projections used (simple cylindrical vs orthographic, respectively).
Paper: Kiladze Caldera: A Possible Cryovolcano on Pluto
Authors: A. Emran, D. P. Cruikshank, C. J. Ahrens, J. M. Moore, O. L. White
Figure caption: (a) Two-dimensional visualization of the DEM and (b) a TIN contour map at the Kiladze area and its surroundings. The DEM (P. M. Schenk et al. 2018) was derived from combined observational data from the New Horizons MVIC and LORRI instruments. The DEM was produced at 100–300 m vertical and 300–800 m spatial resolution, and with a stereo height accuracy from 100 to 1500 m. The data product is peer reviewed and certified for further scientific use for mission data analysis. Note that a 3D visualization of the base map and the TIN can be found in Figure 6.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Offset reflectance spectra converted to emissivity of Allende with increasing regolith porosity (top to bottom). The vertical offset is labeled to the right for each spectrum. Standard deviations between multiple measurements are shaded in gray. Each panel shows the spectra for each particle size: (a) 0–20 μm (S), (b) 20–45 μm (M), and (c) 45–63 μm (L). The 10 μm region is shown within the gray box in (a). Panel (b) includes peaks labeled with P and dips labeled with D. Some features are marked with a black vertical bar for clarity. Note the different scales on the y-axes.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Comparison of reflectance (R) spectra (converted to emissivity via Kirchhoff's law) of two enstatite samples from A. C. Martin et al. (2023) with different scattering regimes to the emissivity spectrum of an airless body. The top spectrum (green) is of an enstatite (Mg89.7) sample with 0 wt% KBr with a particle size range of 45–63 μm, and is primarily in the surface-scattering regime. The middle spectrum (red) is of the same 45–63 μm enstatite sample as above, but with 90 wt% KBr mixed in to simulate regolith porosity, and represents a spectrum dominated by volume-scattering. Both enstatite spectra are scaled by 0.72 and are offset for clarity. The bottom spectrum (black) is asteroid (4035) Thestor from A. C. Martin & J. P. Emery (2023) observed with the Spitzer Space Telescope. The enstatite spectrum with 90% KBr better resembles the spectrum of Thestor than the enstatite spectrum with no KBr, indicating that Thestor's MIR spectrum may be dominated by volume-scattering.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Comparison of Allende MIR spectra with different particle sizes. Solid lines represent 0–20 μm (S) spectra, dashed lines represent 20–45 μm (M) spectra, and dotted lines represent 45–63 μm (L) spectra.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: (a) The VNIR reflectance spectra of an Allende sample with a particle size of 0–75 μm from RELAB (MS-CMP-040-A; dashed gray line), and 1999 JD6 (purple points) measured by MITHNEOS (R. P. Binzel et al. 2019). The spectrum of 1999 JD6 is scaled by 0.15 based on the geometric albedo (J. de León et al. 2010). (b) The VNIR spectra of a 0–75 μm Allende sample with melted/fused grains from RELAB (MS-CMP-040-C; dashed gray line), and the asteroid 114 Kassandra (dark cyan points) measured by SpeX (J. T. Rayner et al. 2003; F. E. DeMeo et al. 2009). Kassandra is scaled by 0.0884 based on the albedo measurement from E. Dotto et al. (2002). All VNIR spectra are normalized to a reflectance of 0.10 at 0.55 μm. (c) The MIR emissivity spectrum of 1999 JD6 measured by the SST (dark purple solid line with points), and ALDS,30 (light purple solid line) scaled by 0.18 and offset for comparison. (d) The MIR spectra of Kassandra (dark cyan solid line with points) and ALDS,90 (cyan solid line), which is scaled by 0.19 and offset. The full 5.12–14.11 μm spectrum of Kassandra is in Figure A1. For (c) and (d), several Allende peaks are located using dashed vertical lines and are compared to possible corresponding peaks in their respective asteroid spectrum (marked by triangles). The area between each peak and its continuum is shaded.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: (a) MIR emissivity spectrum of Eureka measured by the SST (dark red solid line with points), and ALDL,20 (red solid line) scaled by 0.79 and offset for comparison. (b) MIR spectra of Barbara (dark cyan solid line with points) and ALDS,90 (cyan solid line), which is scaled by 0.28 and offset. In the spectrum of Barbara, the 13.65–14.15 μm region is removed because the SST has an artifact at those wavelengths, which is documented in Section 7.3.8 in the Infrared Spectrograph Instrument Handbook (https://irsa.ipac.caltech.edu/data/SPITZER/docs/irs/irsinstrumenthandbook/). For both (a) and (b), several Allende peaks and dips are located using dashed and dotted vertical lines, respectively, and are compared to possible corresponding features in their respective asteroid spectrum (marked by triangles). The area between each feature and its continuum is shaded. Figure A1 shows the full 5.2–38 μm spectra of both Eureka and Barbara.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Each panel shows the spectrum of an Allende sample from this study and an olivine sample (OLV2) from A. C. Martin et al. (2022). Panel (a) shows 45–63 μm (L) spectra with a regolith porosity of 10%, panel (b) shows 20–45 μm (M) spectra with a regolith porosity of 50%, and panel (c) shows 0–20 μm (S) spectra with a regolith porosity of 90%. Select features identified from both studies are labeled, with peaks labeled on top of each spectrum, and dips labeled on the bottom. Positions of Allende peaks and dips are marked with dashed and dotted lines, respectively, and positions of the corresponding OLV2 features are marked with triangles. The area between each peak and its continuum is shaded. For the Allende spectra, we used the location of P2 for the CF1.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: SEDs of the asteroids from this study observed by the SST. (a) The flux of each asteroid (black solid line with points) and its best-fit NEATM (red solid line). (b) Emissivity (i.e., εbolSED/NEATM) of each asteroid.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Positions and spectral contrasts of several Allende spectral features (pink crosses) and corresponding olivine features (purple diamonds). The top, middle, and bottom rows show examples of tier 1, 2, and 3 matches, respectively. The left column shows the change in position with increasing regolith porosity (regolith porosity vs. wavelength), and the right column shows the change in spectral contrast with increasing regolith porosity (spectral contrast vs. regolith porosity). A best-fit curve is shown to highlight the differences between how each feature changes with increasing regolith porosity, where the best-fit curve is dashed for the olivine features, and dotted for the Allende features.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Spectral contrasts of defined Allende spectral features, calculated from Equation (3). Subplot (a) shows peaks (emissivity maxima), and subplot (b) shows dips (emissivity minima). In each subplot, green triangles denote spectral contrast values from the 0–20 μm spectra, yellow diamonds denote 20–45 μm spectra, and red squares denote 45–63 μm spectra.
Paper: Measuring the Effects of Regolith Porosity on Mid-IR Spectra of the Allende Meteorite
Authors: Lonnie D. Dausend, Audrey C. Martin, Joshua P. Emery
Figure caption: Positions of Allende features as a function of regolith porosity. Subplot (a) shows peaks (emissivity maxima), and subplot (b) shows dips (emissivity minima). Within each subplot, each panel from top to bottom shows the positions of the 0–20, 20–45, and 45–63 μm particle sizes. Points marked with stars represent shallow and sloped features.
Paper: Photometry of Lunar Swirls in Comparison to Fresh Crater Ejecta
Authors: Mallory J. Kinczyk, Brett W. Denevi, Hiroyuki Sato, Aaron K. Boyd, Anna C. Martin, Emerson J. Speyerer, Bruce W. Hapke
Figure caption: Reiner Gamma swirl site phase curves. Left panels in blue are regolith, and right panels in red are fresh crater ejecta. Lighter colors signify on-swirl locations, and darker colors signify off-swirl locations for both with intermediate colors in transitional areas. (a), (b) The average reflectance for individual NAC observations at each ROI across the phase range superposed by the empirical photometric model fit (A. K. Boyd & M. S. Robinson 2019) with normalized model residuals below. (c), (d) The same empirical model fit to the data as in (a) and (b) using uniform incidence and emission (i = e = 60°) as well as the photometric models for high-TiO2 mare and immature mare in purple. (e), (f) The empirical model fits to the data normalized to the high-TiO2 mare photometric model.
Paper: Photometry of Lunar Swirls in Comparison to Fresh Crater Ejecta
Authors: Mallory J. Kinczyk, Brett W. Denevi, Hiroyuki Sato, Aaron K. Boyd, Anna C. Martin, Emerson J. Speyerer, Bruce W. Hapke
Figure caption: Distribution of viewing geometries for LROC NAC images collected at each swirl site.
Paper: Photometry of Lunar Swirls in Comparison to Fresh Crater Ejecta
Authors: Mallory J. Kinczyk, Brett W. Denevi, Hiroyuki Sato, Aaron K. Boyd, Anna C. Martin, Emerson J. Speyerer, Bruce W. Hapke
Figure caption: Oblique LROC image of the Reiner Gamma albedo anomaly. Located in the western portion of Oceanus Procellarum, the view is pointing to the northeast, and the crater indicated by the white arrow is ∼1.75 km in diameter. Image M1127569280L (7.35°N, 300.1°E, i: 73﹩\mathop{.}\limits^{\unicode{x000B0}}﹩8, e: 68﹩\mathop{.}\limits^{\unicode{x000B0}}﹩7, g: 5﹩\mathop{.}\limits^{\unicode{x000B0}}﹩5) and M1127569280R (7.39°N, 301.4°E, i: 75﹩\mathop{.}\limits^{\unicode{x000B0}}﹩1, e: 72﹩\mathop{.}\limits^{\unicode{x000B0}}﹩7, g: 3﹩\mathop{.}\limits^{\unicode{x000B0}}﹩1).
Paper: Photometry of Lunar Swirls in Comparison to Fresh Crater Ejecta
Authors: Mallory J. Kinczyk, Brett W. Denevi, Hiroyuki Sato, Aaron K. Boyd, Anna C. Martin, Emerson J. Speyerer, Bruce W. Hapke
Figure caption: Firsov swirl site phase curves. Left panels in blue are regolith, and right panels in red are fresh crater ejecta. Lighter colors signify on-swirl locations, and darker colors signify off-swirl locations for both with intermediate colors in transitional areas. (a), (b) The average reflectance for individual NAC observations at each ROI across the phase range superposed by the empirical photometric model fit (A. K. Boyd & M. S. Robinson 2019) with normalized model residuals below. (c), (d) The same empirical model fit to the data as in (a) and (b) using uniform incidence and emission (i = e = 60°) as well as the photometric models for highlands and immature highlands in purple. (e), (f) The empirical model fits to the data normalized to the mature highlands photometric model.