adsabs/AstroCLIMB huggingface dataset:
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Chandrayaan M3 pyroxene spectral map and Kaguya MI overlaid on the LROC WAC mosaic showing the central mare province region in the Apollo basin. No distinct lava flows can be identified. (a) Chandrayaan M3 pyroxene spectral map showing the overview of the central mare province in the Apollo basin. (b) M3 spectra from seven key locations (indicated in panel (a)) compared with PDS spectral library data. Red: mature mare material; yellow: “fresh,” immature mare deposit; blue: feldspathic material. The ejecta of the large, unnamed Copernican-aged crater overlaying Resnik crater is a prominent feature even on spectral data. This ejecta deposit superposes “Crater 1” (marked with a white arrow in Figure 11) in the northeast–southwest direction (blue; number 4). Crater 1 is 4491 m in diameter with a calculated excavation depth of 377 m (Huang et al. 2018). Crater 1 might indicate exhumation of fresh mare material (yellow; number 5) similar to the small, fresh craters (numbers 2 and 7). (c) Kaguya MI spectral ratio map exhibiting the central mare province (light blue) and basin material (yellow) in the Apollo basin. The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S. M3 image numbers: M3G20090718T054612, M3G20090718T014252, M3G20090717T211502, M3G20090717T171142, M3G20090717T124352, M3G20090717T084032, M3G20090717T041548, M3G20090717T000932.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Geologic maps of ROIs overlaid on the Kaguya TC image, with exploration zones of 2.5, 5, and 10 km from the proposed sites (yellow star). (a) ROI 1 has access to study Im; Copernican-aged ejecta (Cc), which might excavate SPA and Apollo impact melt from the subsurface; and remnants of NpNbh with putative impact melt origin. (b) ROI 2 could sample different Copernican-aged ejecta rays (Cc), potential SPA and Apollo impact melt materials, and Imbrian mare deposit. (c) ROI 3 could investigate Imbrian mare deposits, as well as NpNbm. (d) Geologic correlation chart of geologic units. The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Maps of regolith thickness estimations for each ROI ((a), (b), and (c)) using Quaide & Oberbeck (1968). The data were derived by measuring the diameter of the inner and outer rim of CCs (d) using LROC NAC 1 m pixel−1 data and applying the kriging technique to interpolate the results to the larger area. Points mark the measured values. The circles indicate exploration zones of 2.5, 5, and 10 km from the proposed landing site (yellow star). LROC NAC coverage as of 2018 February is overlaid over Kaguya TC data. The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Geologic map of the central mare province of the Apollo basin overlaid on Kaguya TC and LROC WAC at 1:50,000 mapping scale. ROI 1 (upper) and ROI 2 (lower) are indicated with circular exploration zones of 2.5, 5, and 10 km from the proposed landing sites (yellow star). The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Geologic map of the southern mare province of the Apollo basin overlaid on Kaguya TC and LROC WAC at 1:50,000 mapping scale. ROI 3 is indicated with circular exploration zones of 2.5, 5, and 10 km from the proposed landing site (yellow star). Same legend as in Figure 7. The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Rock abundance derived from LRO Diviner 236 m pixel−1 data overlaid on the Kaguya TC mosaic ((a), (b), and (c)) for ROIs 1, 2, and 3, respectively. (d) Example of a “rocky” young crater. The circles indicate exploration zones of 2.5, 5, and 10 km from the proposed landing sites (yellow star). The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Maps of crater densities overlaid on the Kaguya TC 7 m pixel−1 mosaic on which craters >70 m in diameter were measured. (a) ROI 1, (b) ROI 2, and (c) ROI 3. The circles indicate exploration zones of 2.5, 5, and 10 km from the proposed landing sites (yellow star). The maps are in Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: Based on this study, a proposed theoretical subsurface stratigraphy in the central (a) and southern (b) mare provinces.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: FeO and TiO2 contents derived from Clementine 400 m pixel−1 data overlaid on the Kaguya TC image. (a)–(b), (c)–(d), (e)–(f) FeO and TiO2 contents of ROIs 1, 2, and 3, respectively. Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: National Research Council (2007) science concepts and goals assessed for a robotic exploration mission with rover and lander assets in the Apollo basin. The highest-ranked National Research Council (2007) science concepts and goals cannot be fully addressed without sample return capability.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: National Research Council (2007) science concepts and goals in the case of a robotic exploration mission to the lunar surface with a rover and lander with sample return capability. The highest-ranked science concepts and goals can be achieved with sample return capability.
Paper: Characterization of High-priority Landing Sites for Robotic Exploration Missions in the Apollo Basin, Moon
Authors: Csilla Orgel, Ines Torres, Sebastien Besse, Carolyn H. van der Bogert, Rickbir Bahia, René Prissang, Mikhail A. Ivanov, Harald Hiesinger, Gregory Michael, Jan Hendrik Pasckert, Mayssa El Yazidi, Balazs Bradak, Sebastian H. G. Walter
Figure caption: FeO abundances of mare deposits derived from Kaguya MI 60 m pixel−1 data. Continuous stripes indicate no data. Lambert azimuthal equal-area projection, centered at −152.0°W, −35.8°S.
Paper: Understanding the Dust Environment at Mercury: From Surface to Exosphere
Authors: Harald Krüger, Michelle S. Thompson, Masanori Kobayashi, Valeria Mangano, Martina Moroni, Anna Milillo, Lindsay P. Keller, Sho Sasaki, Joe Zender, Deborah Domingue, Johannes Benkhoff, André Galli, François LeBlanc, Go Murakami, Menelaos Sarantos, Daniel W. Savin
Figure caption: Top left: impact products including visible-light image of a lunar agglutinate from Apollo 11 soil sample with shiny glass coating and vesicles on the surface. Top right: secondary electron (SE) image of the surface of a lunar rock showing evidence of micrometeoroid impacts including microcraters, melt spherules, melt splashes, etc. Bottom left and right: cross-section images of regolith grains from Ryugu in high-angle annular dark field (HAADF) imaging and Apollo 17, respectively, in a transmission electron microscope. Bright spherules of nanophase Fe-bearing particles, ranging in size from a few nanometers to hundreds of nanometers in diameter, can be seen in the images.
Paper: Understanding the Dust Environment at Mercury: From Surface to Exosphere
Authors: Harald Krüger, Michelle S. Thompson, Masanori Kobayashi, Valeria Mangano, Martina Moroni, Anna Milillo, Lindsay P. Keller, Sho Sasaki, Joe Zender, Deborah Domingue, Johannes Benkhoff, André Galli, François LeBlanc, Go Murakami, Menelaos Sarantos, Daniel W. Savin
Figure caption: Simulated images of calcium emission in Mercury's dayside equatorial plane at three different true anomaly angles (TAAs) in Mercury's orbit. The image was produced by interpolating between UVVS observations where the line of sight crosses the equatorial plane approximately perpendicular (white points; Burger et al. 2014). The color scale indicates the interpolated radiance. Mercury's sunlit hemisphere is shown. The dawn terminator is to the left and the subsolar point is at the bottom. The white points represent positions where the UVVS line of sight crosses the equatorial plane. The images reflect large-scale local-time variations (small-scale variations in the images are not real). Although the magnitude of the emission varies with Mercury TAA, calcium is always brightest in the dawn hemisphere, usually, but not always, peaking at dawn. From Burger et al. (2014, their Figure 3).
Paper: Understanding the Dust Environment at Mercury: From Surface to Exosphere
Authors: Harald Krüger, Michelle S. Thompson, Masanori Kobayashi, Valeria Mangano, Martina Moroni, Anna Milillo, Lindsay P. Keller, Sho Sasaki, Joe Zender, Deborah Domingue, Johannes Benkhoff, André Galli, François LeBlanc, Go Murakami, Menelaos Sarantos, Daniel W. Savin
Figure caption: Lunar dust density distribution in a reference frame where the Sun is in the -x direction and the apex motion of the Moon about the Sun is in the +y direction. Left: top-down view of the dust density for particles with s > 0.3 μm. LDEX did not make measurements between 12 and 18 hr local time, while it was pointed near the direction of the motion of the spacecraft. The white coloring indicates regions where LADEE did not visit or was not set up for normal operations. From Horanyi et al. (2015, their Figure 3). Right: modeled annually averaged lunar dust density distribution for particles with s > 0.3 μm. From Szalay & Horanyi (2016a, their Figure 3).
Paper: Understanding the Dust Environment at Mercury: From Surface to Exosphere
Authors: Harald Krüger, Michelle S. Thompson, Masanori Kobayashi, Valeria Mangano, Martina Moroni, Anna Milillo, Lindsay P. Keller, Sho Sasaki, Joe Zender, Deborah Domingue, Johannes Benkhoff, André Galli, François LeBlanc, Go Murakami, Menelaos Sarantos, Daniel W. Savin
Figure caption: Left: vertical density profiles of the CaO and the calcium components at perihelion (TAA = 0°) assuming a vapor cloud quenching temperature of ≤3750 K. Right: comparison between the simulation results obtained in the approximation of the quenching temperature of the vapor cloud ≤3750 K (red line) and =4000 K (purple line) with the MASCS observations (blue line; Burger et al. 2014) along the Mercury orbit (from Moroni et al. 2023, their Figures 7 and 8).
Paper: Understanding the Dust Environment at Mercury: From Surface to Exosphere
Authors: Harald Krüger, Michelle S. Thompson, Masanori Kobayashi, Valeria Mangano, Martina Moroni, Anna Milillo, Lindsay P. Keller, Sho Sasaki, Joe Zender, Deborah Domingue, Johannes Benkhoff, André Galli, François LeBlanc, Go Murakami, Menelaos Sarantos, Daniel W. Savin
Figure caption: Simulated fluxes of particles larger than 100 μm for crossings of comet 2P/Encke's dust trail by the BepiColombo spacecraft. The simulations were performed with the Interplanetary Meteoroid Environment for eXploration Dust Streams in Space model (IMEX; Soja et al. 2015a, 2015b) with a 1 day time step. The solid line shows the simulated flux of interplanetary dust particles larger than 100 μm, as derived from the Interplanetary Meteoroid Engineering Model (IMEM; Dikarev et al. 2005), for an assumed spherical sensor with a 4π sensor field of view. Vertical dashed lines indicate the Mercury flybys (M3–M6) and Mercury orbit insertion (MOI).
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Top row: mass, density, and ice mass fraction evolution of protoplanets with pebble accretion of the power-law density distribution (model 1, Equations (21) and (22)). Actual KBO data are overplotted with green stars. The best accreted pebbles at each mass are still too icy to lead to significant density increase through silicate accretion. The most massive planets formed within 5 Myr are of Pluto mass, but their composition is almost pure water ice. Middle row: same as the top row, but for the bimodal density distribution (model 2, Equations (23) and (24)). As the intermediate-mass objects (10−2 M Pluto to 10−1 M Pluto) accrete silicate pebbles, the mass–density trend is reproduced. The flattening at higher mass is also reproduced, matching Haumea, Pluto, and Triton. The model does not reproduce the density of Eris. Bottom row: same as the other rows, but for constant (silicate) pebble density (model 3). The intermediate-mass objects (10−2 M Pluto to 10−1 M Pluto) are similar to those in model 2, but the model overshoots the density of the higher-mass objects Haumea, Pluto, and Triton. Eris, however, is reproduced.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: The results from applying the polydisperse pebble accretion model with the bimodal distribution of pebbles across various heliocentric distances. At 10 au (top left), not only do we underestimate the densities of the KBOs, but the masses produced are also much larger than those seen in the Kuiper Belt. At just 500,000 yr, planetesimals are already an order of magnitude larger than Pluto. From 15 to 22 au, we fit the density trend well and reach Pluto mass in 1.8, 5.7, and 8.5 million years, respectively. Beyond 22 au, accretion rates are so low that we cannot reach Pluto’s mass within the assumed lifetime of the disk (10 million years).
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Left: planetesimal formation rate (number of planetesimals N formed per time interval ﹩{{\rm{\Omega }}}_{0}^{-1}﹩), as a function of time, in the box. There is a rapid burst of planetesimal formation between two and four orbits, and planetesimal formation comes to a halt after about five orbits. Right: time evolution of maximum dust density in a mesh cell. The blue line corresponds to the Roche density. If this threshold is exceeded, particles in that mesh cell are removed. The initial rise in density from zero to one orbit marks the sedimentation of solids and concentration by the instability, after which the Roche density is achieved for several orbits but then drops after roughly five orbits.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Ice mass fraction of the planetesimals formed at the end of the streaming instability simulations. The composition is not uniform; a trend emerges where the higher-mass planetesimals are formed with higher ice mass fraction.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: The vertically integrated (top) and azimuthally integrated (bottom) dust density after six orbits, when planetesimal formation has saturated. The left panels correspond to the sum of ice and silicate densities, while the middle and right panels are the ice and silicate densities, respectively. Circles indicate formed planetesimals, and circles in the top panels show the Hill radii of these planetesimals. The Hill radii appear close to ice overdensities, consistent with our detailed measurements of high ice mass fractions.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Comparison of accretion rates for the bimodal distribution at different radii. The window at which silicate accretion is most effective shifts to higher masses as we move outward in the disk. This provides further evidence for 20 au being a favorable location, as silicate accretion is most effective around 10−2 M Pluto, right when the densities of KBOs begin to increase.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Evolution of the ice-to-silicate ratio in the vertical plane. The bright yellow is saturated. The ices settle in about 0.5 orbits, reaching an ice-to-silicate ratio of about 10 in the midplane. The filamentary structure of the streaming instability is seen after roughly one orbit.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Left: ice-to-silicate ratio in the midplane at t = 0.5 orbits, approximately the time when the ices settle. Right: ice-to-silicate ratio in the midplane at t = 2.0 orbits, approximately the time of formation of the first planetesimals. The increase in ice-to-silicate ratio due to settling leads to a factor 10 enhancement. Further enhancement is due to the streaming instability.
Paper: A Solution for the Density Dichotomy Problem of Kuiper Belt Objects with Multispecies Streaming Instability and Pebble Accretion
Authors: Manuel H. Cañas, Wladimir Lyra, Daniel Carrera, Leonardo Krapp, Debanjan Sengupta, Jacob B. Simon, Orkan M. Umurhan, Chao-Chin Yang, 朝欽 楊, Andrew N. Youdin
Figure caption: Body temperature T 1 resulting from heating from decay of 26Al, as a function of mass fraction of silicates, F  s .
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: The difference in MARCI water-ice optical depths between the north- and south-facing SHM FOVs over MYs 32–36. Outside of the ACB, the south-facing average is almost always greater than the north-facing average, possibly suggesting that the dune fields filling the southern half of Gale are artificially driving up the orbital retrievals. During the ACB, we see higher optical depths to both the north and south, though the south-facing retrievals are, on average, higher than those to the north.
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 our three phase functions and those previously derived for six cloud types observed on Mars. We can see reasonable agreement between the reference phase functions and those that we have derived, though the limited scattering angle coverage (particularly in the forward-scattering direction) and lack of distinctive features in any of the phase functions make direct comparisons challenging. The different appearance of our phase function in the panels is a consequence of the normalization procedure performed for each comparison phase function.
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: The six PFSS phase functions compared to our derived phase functions (in black with associated 95% confidence intervals) for MYs 34–36. MSL-derived PFSS phase functions agree reasonably well with ours, with the MCS-derived PFSS phase functions agreeing less well with the forward-scattering peak starting approximately 20° earlier. A robust comparison between the phase functions is limited due to the overlap being constrained to the lowest-information portion of the curves.