adsabs/AstroCLIMB huggingface dataset:
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 FOV captured by a north-facing SHM (in red) assuming a cloud altitude of 22.5 km overlaid on top of a MARCI water-ice optical depth map. The black circle marks the rim of Gale, while the black line within Gale is the MSL traverse. The Navcam FOV captures clouds in a large area with a range of optical depths.
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: Comparing the calculated cloud opacities before (red) and after (black) applying the phase function correction as a function of scattering angle (top panel), solar longitude (middle panel), and LTST (bottom panel). In the top panel, we can see that the near-Sun increase (also shown in Figure 8) goes away after applying the correction.
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 MARCI and MSL water-ice retrievals for MYs 34–36. The MSL retrievals generally track those from orbit, with deviations occasionally seen near both the beginning and end of the ACB season, possibly indicating the presence of more dust in the atmosphere at these times than at the peak of the ACB season.
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: Vertical profiles of eddy diffusion coefficient (K  zz ) for the Nominal Case (black solid line), Case 1 (red dotted line), Case 2 (blue double-dotted–dashed line), and Case 3 (green dashed–dotted line), with estimated values by von Zahn et al. (1980), Woo et al. (1982), Mahieux et al. (2021), and Woo & Ishimaru (1981) labeled as vZ1980, W1982, M2021, and WI1981, respectively. The arrow of WI1981 indicates that the value is the upper limit.
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: Vertical profiles of the simulated H2O VMR in the Nominal Case and Cases 1, 2, and 3 compared with observations by SPICAV/SOIR (Fedorova et al. 2008), VIRTIS-H (Cottini et al. 2012), NASA Infrared Telescope Facility (Krasnopolsky et al. 2013), SPICAV/IR (Fedorova et al. 2016), and SPICAV/SOIR (Chamberlain et al. 2020), labeled as F2008, C2012, K2013, F2016, and C2020, respectively.
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: (a) Vertical profiles of the simulated mass loading (mg m−3) in the Nominal Case, Case 1 (red dotted line), Case 2 (blue double-dotted–dashed line), and Case 3 (green dashed–dotted line). The mass loading obtained by the LCPS (Knollenberg & Hunten 1980) is plotted for comparison as KH1980. (b) Vertical profiles of the simulated extinction coefficient (km−1) at 3 μm wavelength in the Nominal Case (black solid line), Case 1 (red dotted line), Case 2 (blue double-dotted–dashed line), and Case 3 (green dashed–dotted line) in comparison with the extinction coefficient at 3 μm wavelength measured by the VEx/SOIR (Wilquet et al. 2012) labeled as W2012 (season 10: S10; season 11: S11; season 12: S12).
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: The simulated particle size distribution as a function of radius at (a) 48 km, (b) 54 km, (c) 63 km, (d) 70 km, (e) 80 km, and (f) 90 km in the Nominal Case (black solid line) and Case 1 (red dotted line) in comparison with the previous work by Imamura & Hashimoto (2001; labeled as IH2001). The size distribution measured by the LCPS on board PV (Knollenberg & Hunten 1980) is plotted as KH1980.
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: (a) Vertical profiles of temperature used in the model. The black solid line represents the temperature profile adapted from Seiff et al. (1985) and is used for the Nominal Case, as well as for Cases 1, 2, and 3. The magenta dashed line represents the temperature profile above 85 km adapted from Mahieux et al. (2015) and is used for Cases 4 and 5. (b) Vertical profile of pressure (Seiff et al. 1985) used in the model.
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: (a) Vertical profiles of the simulated H2SO4 VMR in the Nominal Case and Cases 1, 2, and 3 compared with the observations by Magellan radio occultation measurements (Kolodner & Steffes 1998; labeled as KS1998), VEx/VeRa measurements (Oschlisniok et al. 2021; labeled as O2021), and the upper limit suggested by Sandor et al. (2012; labeled as S2012). The saturation level of H2SO4 VMR (SVMR) is also indicated by a brown dashed line for the Nominal Case. (b) Vertical profiles of the simulated H2SO4 relative humidity in the Nominal Case and Cases 1, 2, and 3.
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: Vertical profiles of H2SO4 vapor (red solid line) and CN (green dashed–dotted line) production rates used in the model. The H2SO4 vapor production rate is adapted from Krasnopolsky (2012).
Paper: One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure
Authors: Hiroki Karyu, Takeshi Kuroda, Takeshi Imamura, Naoki Terada, Ann Carine Vandaele, Arnaud Mahieux, Sébastien Viscardy
Figure caption: The simulated particle size distribution as a function of radius and altitude in (a) the Nominal Case and (b) Case 1.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: The moment of inertia factor of the postimpact largest remnant (y-axis) as a function of its mass, with accretion efficiency of the largest remnant (ξ L) in color. The moment of inertia factor is the moment of inertia divided by that of a hydrostatic body with the same mass and core mass fraction, as outlined in Appendix A. Both axes use logarithmic scales. To avoid catastrophic events, only collisions where ξ L > − 1 are shown. The simulation number is shown when the moment of inertia factor is larger than 1.5. A black label is used for runs in the 1000 simulation set, and red for those in the 250 simulation set.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Debris velocity at infinity given in terms of the relative velocity between the initial bodies (target and impactor) at initial contact for all the simulations of this study. Left panel shows the values as function of the mass fraction of debris at the end and color coded by the initial v coll/v esc. Right panel shows the same data with the horizontal axis and color code inverted. The step-wise line shows the median of the values in the given range.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Mass ratio of the satellite-to-primary pairs (γ P) as function of the primary mass (computed as ﹩{m}_{\mathrm{tar}}\left(1+\gamma {\xi }_{{\rm{P}}}\right)﹩), for all simulations ending in coorbiting secondary remnants. The number in the plots refers to the corresponding run numbers: black for those in the 1000 simulation set, and red for those in the 250 simulation one. The color scale represents the ratio between the orbital frequency of the satellite and the spin rate of the primary (n P/ΩL), which is 1 for synchronous orbit and must be <1 for stable, outward tidal migration.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Scatter plots of the number of resolved (>10 SPH particle) fragments, excluding the largest and second remnants, found in our simulation database as function of target mass and relative velocity v coll/v esc. The color represents number of fragments in a single simulation. Collisions not producing any fragment are shown by smaller black circles. Although these points include simulations with various impactor-to-target mass ratios, we show absolute impact velocities for the target mass alone, assuming a core mass fraction of 30%. It can be seen that the number of resolved clumps decreases with increasing target mass.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Density ratio with respect to the reference value from the EOS (left) and moment of inertia factor I/I ref (such that 1 is a uniform density sphere; right) as function of body mass and core mass fraction.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Comparison of the accretion efficiency of debris ξ D and the rms of the debris velocity for collision 561 of the 1000 simulation set for two different SPH resolutions, as indicated in the legends. The dashed horizontal line in the right panel shows the impact velocity.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Comparison of the size–frequency distribution of the remnants for collision 566 of the 1000 simulation set for two different SPH resolutions, as indicated in the legends. The two texts “LR” and “SR” denote the largest and second remnants, respectively.
Paper: A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes
Authors: Alexandre Emsenhuber, Erik Asphaug, Saverio Cambioni, Travis S. J. Gabriel, Stephen R. Schwartz, Robert E. Melikyan, C. Adeene Denton
Figure caption: Final state of simulation #0058 with different values for parameters of the solid model. The left panel shows the nominal case and is the same as the right panel of Figure 4. The right panel shows the same initial conditions, but with μ d = 0.63, and μ i = 1.58.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: NIRSpec IFU images for Callisto's leading (left column) and trailing (right column) hemisphere. The globes show the simulated observing geometries (inset plot shows the orbit of Callisto around Jupiter), the mean reflected emission at 2.9 μm, the estimated surface temperatures, and the retrieved CO2 column densities, from the top row to bottom row, respectively. Notable asymmetries in the distribution of CO2 gas are indicated with white arrows (discussed in Section 4.2).
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: 4.25 μm 12CO2 band depth (top) and band center (middle) maps. Example continuum-divided 4.25 μm bands and model fits (bottom) are shown for spaxels near the center of Callisto's trailing side (left) and in the Asgard impact basin (right). These maps highlight the substantially stronger 12CO2 feature on Callisto's trailing side and the shifted central wavelength of the 12CO2 band on Callisto's leading side.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: 4.38 μm 13CO2 band depth map, including both the “base” and “peak” components of this feature (top) and 4.38 μm band center map for the base component only (middle; the peak component does not exhibit wavelength shifts, and so is excluded). Example continuum-divided 4.38 μm bands and model fits (bottom) are shown for spaxels near the center of Callisto's trailing side (left) and in the Asgard impact basin (right). These maps highlight the modestly stronger 13CO2 feature on Callisto's trailing side, in part resulting from the narrow peak component overprinting the wide and shallow base component. This narrow peak feature is fit by a second Gaussian model (shown in bottom, left plot).
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: 4.57 μm band depth (top) and band center (middle) maps. Example continuum-divided 4.57 μm bands and model fits (bottom) are shown for spaxels near the center of Callisto's trailing side (left) and in the Asgard impact basin (right). These maps highlight the notably stronger 4.57 μm feature on Callisto's leading side, and the shift of its band center to shorter wavelengths on Callisto's trailing side.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption:  12CO2/4.57 μm band depth ratios highlighting the apparent spatial antiassociation between these two spectral features. White and light blue colors indicate regions where 12CO2 is strongest, i.e., trailing hemisphere, and dark blue colors indicate regions where the 4.57 μm band is stronger, i.e., leading hemisphere, away from Asgard and Valhalla (extents approximated with gold circles).
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption:  13CO2/12CO2 band area (filled circles) and depth (filled triangles) ratios and 1σ errors for the binned NIRSpec spectra of Callisto and VIMS spectra of Phoebe and Iapetus (spectra shown in Figure 9; ratios reported in Table 3). The hollow circles and triangles respectively show the band area and depth ratios for Callisto measured using Io-subtracted data.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: Comparison between 12CO2 and 13CO2 features in VIMS spectra of Iapetus (blue) and Phoebe (green; Clark et al. 2019) and NIRSpec integrated spectra of Callisto's leading (purple) and trailing (orange) hemisphere, which have been binned to simulate the spectral resolution of VIMS data. All spectra are normalized to 1 at 4.35 μm. Approximate band centers are indicated (dashed lines). Error bars represent the 1σ uncertainties for each spectrum.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: 4.25 μm 12CO2 band depth (top) and band center (middle) error maps for data shown in Figure 6.
Paper: Revealing Callisto’s Carbon-rich Surface and CO2 Atmosphere with JWST
Authors: Richard J. Cartwright, Geronimo L. Villanueva, Bryan J. Holler, Maria Camarca, Sara Faggi, Marc Neveu, Lorenz Roth, Ujjwal Raut, Christopher R. Glein, Julie C. Castillo-Rogez, Michael J. Malaska, Dominique Bockelée-Morvan, Tom A. Nordheim, Kevin P. Hand, Giovanni Strazzulla, Yvonne J. Pendleton, Katherine de Kleer, Chloe B. Beddingfield, Imke de Pater, Dale P. Cruikshank, Silvia Protopapa
Figure caption: Integrated NIRSpec spectra of Callisto's leading (purple) and trailing (orange), Ganymede's leading (blue) and trailing (green), and Europa's leading (black) hemisphere highlighting the 12CO2 band, normalized to 1 at 4.305 μm. Central wavelengths for each 12CO2 band are listed on the plot using the same color scheme. Error bars have been suppressed for clarity.
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 the Apollo basin overlaid on LROC WAC mosaic. (a) LROC WAC mosaic of 100 m pixel−1, with three ROIs with a proposed central landing site (yellow star) and 2.5 (yellow), 5 (white), and 10 (red) km exploration zones. (b) Kaguya TC DEM (7 m pixel−1). (c) Slope map derived from the Kaguya TC DEM. (d) Diviner Lunar Radiometer Experiment rock abundance map (236 m pixel−1). (e) 1:5M scale unified geologic map of Fortezzo et al. (2020). (f) and (g) Clementine TiO2 and FeO maps (400 m pixel−1; Lucey et al. 2000). ROIs overlap the highest FeO and TiO2 concentrations. (h) Kaguya MI FeO map (∼60 m pixel−1; Lemelin et al. 2016). All figures 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: Oblique view of Apollo basin derived from a merged LRO LOLA and Kaguya TC 60 m pixel−1 DEM (Barker et al. 2016) and 100 m pixel−1 LROC WAC mosaic. Vertical exaggeration is 2×.
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: DEMs ((a), (c), and (e)) and slopes ((b), (d), and (f)) derived from the Kaguya TC 7 m pixel−1 stereo image mosaic for ROIs 1, 2, and 3, respectively. 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: SPA (2400 × 2050 km) and Apollo (492 km) basins shown on the LOLA DEM 100 m pixel−1 data (Smith et al. 2010) overlaid on LROC WAC (Robinson et al. 2010).