adsabs/AstroCLIMB huggingface dataset:
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: Reduced infrared χ2 values vs. thermal inertia for various combinations of surface roughness (symbol coded) and optimized diameters of the equivalent surface sphere (color coded). Solutions for pole 1 (left) and for pole 2 (right). Due to the multitude of parameters, for surface roughness only the surface element coverage is shown (f), while the opening angle of spherical-section craters ranged from 10° to 90°. Higher opening angles provided better fit to thermal data.
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: The model fit to normalized phase curve of (269) Justitia resulting from the CITPM: solution for pole 1 (left) and pole 2 (right). Calibrated brightness measurements have to be normalized in the modeling process in order not to overweight other types of data.
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: Shape models of asteroid (269) Justitia from the CITPM: solution for pole 1 (top) and pole 2 (bottom). Shapes are displayed in three views, left to right: two equatorial views, 90° apart, and a pole-on view.
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: On-sky views of Justitia shape models from the CITPM phased for the 2023 August 31 occultation moment at 10:56 UT. North is up and east is left. Left plot: shape model for pole 1; right plot: same for pole 2 (see Table 1).
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Interquartile range of standardized roughness at a baseline of 50 m for the north (left) and south (right) pole as a function of average regolith temperature. Blue and red lines represent regions where thermal models predict subsurface (SS) ice is stable or unstable, respectively (N. Schorghofer & J.-P. Williams 2020; N. Schorghofer et al. 2024). Dashed and solid lines denote areas with a 1600 m baseline topographic slope of 0°–5° and 15°–20°, respectively.
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Slope (left column) and roughness (right column) for 100, 400, and 800 m baselines. The roughness color scale ranges from the 2nd to the 98th percentile.
Paper: Long-term Spectral Monitoring of Active Asteroid (6478) Gault: Implications for the H Chondrite Parent Body
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Neil Pearson, Benjamin N. L. Sharkey, Theodore Kareta
Figure caption: Molar content of fayalite (Fa) vs. olivine-to-pyroxene ratio, ol/(ol+px), with boundaries for the ordinary chondrite subgroups displayed. The plot is adapted from T. L. Dunn et al. (2010). However, outside the boxes defining the meteorite types, Gault shows mineralogy most consistent with H chondrites. X-ray diffraction measurements for several meteorites presented in T. L. Dunn et al. (2010) are shown with their petrologic type indicated. For the H chondrites, the ol/(ol+px) ratio increases with increased thermal metamorphism. Gault’s ol/(ol+px) values are lower than the H4 types, suggesting similar or lower levels of thermal alteration. Gault’s marker size increases with time and shows no clear trend in mineralogy. Data for only five nights are shown because no Band II parameters could be measured for 2020 September 19.
Paper: Long-term Spectral Monitoring of Active Asteroid (6478) Gault: Implications for the H Chondrite Parent Body
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Neil Pearson, Benjamin N. L. Sharkey, Theodore Kareta
Figure caption: NIR (0.7–2.5 μm) spectra of Main Belt active asteroid (6478) Gault used in this study plotted with reflectance normalized at 1.5 μm. Plotted error bars for each night’s spectrum are from the standard deviation of bins used to improve spectrum signal-to-noise ratio. The gray band for the average spectrum represents the standard deviations across all six nights of observations. Observational circumstances for each night can be found in Table 1.
Paper: Long-term Spectral Monitoring of Active Asteroid (6478) Gault: Implications for the H Chondrite Parent Body
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Neil Pearson, Benjamin N. L. Sharkey, Theodore Kareta
Figure caption: Molar content of fayalite (Fa) vs. ferrosilite (Fs) derived for Gault, showing a mineralogy consistent with H chondrites. The typical uncertainty for this type of measurement is represented by the error bars in the upper left corner, corresponding to 2.0 mol% uncertainty for Fa and 1.4 mol% for Fs as derived by J. A. Sanchez et al. (2020). Marker size increases with time, showing that Gault’s derived mineralogy fluctuates within uncertainty values, but with no distinct pattern in time. Measured values are displayed for LL (squares), L (triangles), and H (circles) ordinary chondrites from T. Nakamura et al. (2011).
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: Temporal and hemispheric means of the vertical distribution of air temperature, liquid and ice cloud abundances, and mole fractions χi of chemical species i related to ozone formation in both simulations. Each plot has a title corresponding to the variable or chemical species shown. Solid lines indicate the mean over the 0∘ hemisphere and dashed lines the mean over the 180∘ hemisphere, representing the dayside and nightside in a 1:1 SOR. The vertical distributions illustrate important differences between a 1:1 and 3:2 SOR for Proxima Centauri b (PCb).
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: Temporal and hemispheric means of the vertical distribution of selected reaction rates for both simulations of Proxima Centauri b (PCb). Each plot title corresponds to the chemical reaction shown. Solid lines indicate the mean over the 0∘ hemisphere and dashed lines the mean over the 180∘ hemisphere, representing the dayside and nightside in a 1:1 SOR. The reactions were selected to include the Chapman mechanism of ozone formation (panel a and b), the rate-limiting steps for HOx catalytic cycles (panel (c)–(g)), and NOx catalytic cycles (panel (h) and (i)).
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: Instantaneous surface temperature for Proxima Centauri b in a 3:2 SOR for (a) the substellar point at 0∘ longitude and (b) the substellar point at 180∘ longitude. The horizontal wind vectors are again shown at P ≈ 250 hPa.
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: Mean over 600 days of the vertically integrated ozone column density for Proxima Centauri b in a 1:1 SOR.
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: Temporal mean surface temperature over 600 days for Proxima Centauri b in a 1:1 SOR. The substellar point is located at (ϕ, λ) = (0°,0°). Overplotted are the horizontal wind vectors at P ≈ 250 hPa, showing the equatorial jet. The white contour lines indicate surface temperatures of 273.15 K, and therefore the regions that can sustain liquid water.
Paper: Earth-like Exoplanets in Spin–Orbit Resonances: Climate Dynamics, 3D Atmospheric Chemistry, and Observational Signatures
Authors: Marrick Braam, Paul I. Palmer, Leen Decin, Nathan J. Mayne, James Manners, Sarah Rugheimer
Figure caption: Instantaneous vertically integrated ozone column density for Proxima Centauri b in a 3:2 SOR for (a) daytime on the 0∘ hemisphere and (b) daytime on the 180∘ hemisphere.
Paper: Implications of Differentiated Late Accretion for the Volatile Inventory of the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Varun Manilal
Figure caption: C–N–H and S–Se–Te show siderophile character across a reasonable range of temperatures relevant for metal–silicate equilibration in a lunar-sized impactor.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Four simulations of Phobos encountering the 2:1 tesseral resonance with the Martian rotation. Gold and light blue lines show simulations with zero initial inclination of Phobos, and these simulations show captures into different inclination-type T3BRs involving Phobos, the Martian figure, and the Sun. The green line shows a simulation with a nonzero inclination and low eccentricity that experiences a temporary capture into the principal eccentricity-type T3BR. The purple line shows a simulation with Phobos starting both inclined and eccentric in which Phobos crosses the 2:1 tesseral resonance without any captures into T3BRs. Under our assumptions, this crossing happened 300 Myr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Left-hand panel: two 100× accelerated simulations of Phobos encountering the 3:2 tesseral resonance. The simulation with low initial eccentricity (gold) results in capture into the eccentricity-type T3BRs involving Phobos, the Martian figure, and the Sun, while the simulation with initial eP = 0.002 (green) crosses the resonance without capture. Right-hand side: three simulations of Phobos crossing the 3:2 tesseral resonance without a resonance capture. The purple points show the simulation with the realistic migration rate, while the blue and green points show runs with Phobos’s migration accelerated 10 and 100 times, respectively. The inclination is plotted relative to the Martian equator and includes a forced inclination of 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩12. Assuming a constant Martian Q, this resonance happened about 1.1 Gyr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: The evolution of Phobos’s eccentricity and inclination under the APH (left) and RPH (right). The middle panels indicate the resonance locations. Between resonances, we used the relation eP ∝ a6.46, based on the work of P. Goldreich & R. Sari (2009) on tidal dissipation in rubble piles. In the right-hand panel, the teal line plots an alternative evolution path in which Phobos experiences temporary capture (Figure 5) rather than a “kick” (Figure 4) at the Touma resonance at 2.94 RM.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Left-hand panel: five simulations of Phobos encountering the 2:1 tesseral resonance with Martian rotation resulting in temporary capture into an eccentricity-type T3BR involving Phobos, the Martian figure, and the Sun. Right-hand panel: six simulations of Phobos encountering the 2:1 tesseral resonance with Martian rotation that experienced no resonant capture.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Dependence of the eccentricity change of Deimos over 1 Myr on the obliquity of Mars. Each of the 10 simulations in Figure 11 has been divided into 100 1 Myr segments, and the averaged eD and obliquity of Mars (with respect to its heliocentric orbit) θ were calculated for each segment. Individual points plot the magnitude of the difference between the average eD of each segment and its predecessor as a function of the average θ for the segment. There appear to be secular resonances affecting the orbit of Deimos when the obliquity of Mars is in the 33°–38° range.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Two simulations of Phobos encountering the 4:3 tesseral resonance with Martian rotation. The simulation with very low initial eccentricity (green) results in capture into the eccentricity-type T3BRs involving Phobos, the Martian figure, and the Sun, while the simulation with an initial eP = 0.001 (purple) crosses the resonance without capture. The inclination is plotted relative to the Martian equator and includes a forced inclination of 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩18. Assuming a constant Martian Q, this resonance happened 1.8 Gyr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Seven simulations of Phobos encountering the 2:1 tesseral resonance with Martian rotation resulting in capture into the inclination-type T3BRs involving Phobos, the Martian figure, and the Sun. The gold line (same simulation as the gold line in Figure 14) plots a rare capture into a higher-order inclination-type T3BR. While in all other runs, capture into the lowest-order inclination-type T3BR persists to the end of the simulation, the higher-order capture is temporary.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Eccentricity (purple) and inclination in radians (green) in a simulation of Phobos encountering the 5:4 tesseral resonance with Martian rotation. The inclination is plotted relative to the Martian equator and includes a forced inclination of 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩22 (0.0038 rad). Assuming a constant Martian Q, this resonance happened 2.5 Gyr ago.
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: Asteroid Justitia infrared model fluxes (red circles) compared to measured fluxes in various bands indicated in each plot (black circles). Infrared measurements spaced by more than 100 days are shown in separate plots.
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: Composite lightcurves of (269) Justitia from the verge of the years 2019 and 2020 (left) and from the year 2021 (right).
Paper: Thermophysical Model of (269) Justitia—Main Belt Asteroid Possibly Implanted from Trans-Neptunian Region
Authors: Anna Marciniak, Antoine Choukroun, Julia Perła, Waldemar Ogłoza, Robert Szakáts, Pierre Antonini, Raoul Behrend, Géza Csörnyei, Marek Dróżdż, Marcel Fauvaud, Stéphane Fauvaud, Adrian Jones, Dong-Heun Kim, Myung-Jin Kim, Viktor Kudak, Iga Mieczkowska, Erika Pakštienė, Vasyl Perig, Eda Sonbas
Figure caption: Composite lightcurve of (269) Justitia from the year 2022.
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: (a) Activity averaged over all maps in Figure 5. At each point, the intensity represents the number of times the point was determined to be active divided by the number of times it was observed (i.e., determined to be either active or inactive). Indeterminate and degenerate points are not counted, except in cases where two fractures are so close to one another as to be effectively indistinguishable (e.g., Baghdad vs. B8; see text). (b) Number of observations used for each average in (a). (c) Standard deviation at each point in (a). Blue points have zero standard deviation.
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Final activity maps. The same as in Figure 4, except segments showing no activity have been removed and the degenerate colors have been consolidated.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Raw activity maps at 15 epochs superimposed on stereographic projections of Enceladus’s SPT down to 60°S. Dates are in YYYY-DOY format and refer to observation midtimes. Mean anomaly (MA) ranges are listed for each observation. REV indicates the Cassini orbit number. Points in green are active. Points in red are inactive. Points in blue are indeterminate. Other colors are degenerate.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Mean-anomaly coverage for each data set used in this study.
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Inactivity correlation vs. mean anomaly overlap. Symbol shading represents the mutual fracture coverage, from black = 100% to white (invisible) = 0%. The diagonal line gives the approximate minimum expected correlation for a given overlap if the eruptions are tidally controlled. Most points fall on the y-axis (and are not plotted) because most observations have no overlap in mean anomaly.
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Illustration of the difficulty in measuring eruptive activity as only discrete jet-like features. The left panel shows a Cassini image with no overlays. The right panel shows the same image with discrete jets identified with numbered line segments (red). Other more subtle linear jet-like features may be identified in the image, but it is clear that most of the activity seen in the image cannot be represented in that way. The curtain representation, shown in green, is able to represent all of the eruptive activity seen in the image. The abrupt lower edge seen in the curtains corresponds to the shadow of Enceladus and can often be used to uniquely identify the source fracture.
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Stereographic projection of Cassini ISS images (T. Roatsch et al. 2018) showing names assigned to each candidate fracture considered in this work. Colors are used to distinguish adjoining fractures.
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Comparisons of inactivity patterns and mean anomaly overlaps for every pair of maps in Figure 5. Lower-right regions (red) compare the fraction of common points that are inactive. Upper-left regions (green) give the mean anomaly overlap criterion (see text).
Paper: Curtain-based Maps of Eruptive Activity in Enceladus’s South-polar Terrain at 15 Cassini Epochs
Authors: Joseph N. Spitale, Mattie D. Tigges, Alexander Berne, Alyssa Rhoden, Terry A. Hurford, Kevin D. Webster
Figure caption: Short-term variability identified in passing during this mapping project. In the top row, a jet is seen to turn on between the two images. In the bottom row, a jet is seen to turn off, and a curtain dims noticeably. Analysis of these observations is outside the scope of this paper. Other instances of possible short-term variability were noted but would require further analysis to confirm.
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Left: map of north polar effective resolution (in meters, binned at 80 m pix−1) defined as the largest crater diameter that would not be sampled by a LOLA spot. The minimum map latitude is 80° at X/Y = 0 km and 75﹩\mathop{.}\limits^{\unicode{x000B0}}﹩89 at the corners. For this and all map-projected figures, the map projection is polar stereographic centered at the pole. Scale is true at the pole, with a projection radius of 1737.4 km. Figure 1 of M. K. Barker et al. (2023) shows a similar map for the south pole. Right: effective resolution variation with latitude. The effective resolution improves toward both poles, but, due to LRO’s evolving polar orbit, some longitudes have received greater coverage than others even at the same latitude, and the north pole generally has lower (i.e., worse) effective resolution than the south pole.
Paper: Large-scale Roughness Properties of the Lunar North and South Polar Regions as Measured by the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: North polar color-composite image of LOLA roughness with each baseline assigned to a different color.