adsabs/AstroCLIMB huggingface dataset:
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The solar phase coefficients for Iapetus between 1° and 8° and <0.2°, along with the ground-based visible data of Noland et al. (1974).
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Principle of dust suspension by impact splash of saltating grains. The underlying image is from Kruss et al. (2020) and shows a superposition of images of saltating grains under Martian gravity with a time interval of about 2 ms. The “suspended dust grains” inset is only a sketch but refers to the dust fraction sampled in the experiments.
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Volume size distributions of the MGS sample; the sample is a mix of two populations of equal total volumes.
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Scanning electron microscope image of the MGS sample. Dust of the fine fraction is sticking to the surface of a particle of the coarse fraction.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: The pressure and temperature signals for several vortices. The blue dots show the pressure signals that were used to find the vortices, while the blue curves show the best-fit pressure models (assuming a white noise model). The orange dots show the contemporaneous temperature data. The dashed black lines show the best-fit temperature models without including any noise, while the orange curves show samples from the modeling that include noise. The sol and central occurrence time t 0  P  for each vortex is shown at the top of each panel.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: Comparison of the vortex heights estimated from this work (blue solid curve) to those from Stanzel et al. (2008) (orange dashed curve) and Reiss et al. (2014) (green dashed–dotted curve). To guide the eye, a curve showing an ∝h −1 dependence (gray, solid) is included. The y-axis shows the fraction of that data set that falls within that bin. For instance, about 46% of the vortices reported in “This work” fall into the smallest bin, centered on 100 m.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: Estimated temperature signal amplitudes ΔT 0 vs. the pressure signal amplitudes ΔP 0 (b) and vs. time of day LMST (c) for the 112 vortices with credible temperature signals. Histograms of ΔP 0 and ΔT 0 for the vortex encounters with credible temperature excursions are shown in (a) and (d), respectively.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: (a) The best-fit ΔP 0 and Γ P  values (blue dots) with error bars for sols 90 through 179. (b) Cumulative histogram of Γ values, along with the median value (﹩{\rm{\Gamma }}=\left(19.7\pm 1.6\right){\rm{s}}﹩) shown by the dashed orange line. (c) Cumulative histogram of ΔP 0 values, along with the median value (﹩{\rm{\Delta }}{P}_{0}=\left(0.45\pm 0.01\right)\mathrm{Pa}﹩) shown by the dashed orange line. The dashed green line shows a power-law fit to the histogram for ΔP 0 > 0.45 Pa with ﹩N\propto {\rm{\Delta }}{P}_{0}^{-1.90\pm 0.01}﹩.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: Estimates for the heights h of the encountered convective vortices, scaled by the atmospheric scale height H as a function of time of day LMST. Error bars derive from the uncertainties on the vortex ΔP 0 and ΔT 0 values.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: MCMC chains for the fit parameters for the temperature signal in Figure 1 (d). The autocorrelation times τ are shown in red. (We fit −ΔT 0 and the difference between the central encounter times for the pressure and temperature signals ﹩{\rm{\Delta }}{t}_{0}^{T}﹩.)
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: (Top) When pressure data were collected during each sol. The orange dots also show when vortex signals were detected. (Bottom) The blue bars show the number of vortex encounters during each sol, while the orange bars show the number of encounters each sol divided by the total number of hours during which the pressure sensor collected data. The gray dashed–dotted lines show sols when data were unavailable. Solid black lines indicate the L s values.
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: The marginalized posterior distributions for the fit parameters from Figure 2 and for the temperature model in Figure 1(d).
Paper: Estimating the Heights of Martian Vortices from Mars 2020 MEDA Data
Authors: Brian Jackson
Figure caption: The blue bars show the total number of vortex encounters that took place during that hour over the whole 90 sol period, while the orange bars show that number divided by the total number of hours that hour of the day was observed.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Examples of impact craters that have been modified. In some cases, combinations of processes affect an impact crater, so amalgamations of features detailed in Table 1 may be present. However, in this figure the craters are labeled by the most prominent modification process for simplicity. Panel (a) shows examples of “mostly mantled” and “partially mantled” craters in the Tisia Valles region of Mars, identified by Beddingfield et al. (2018). These craters are mantled by regolith deposited from a regional-scale deposition event and have also undergone some degree of degradation, forming irregular rims in locations where regolith cover is lower (Beddingfield et al. 2018). This figure shows a portion of Context Camera (CTX) image D20_035182_1681_XN_11S315W, and the small crater in the top right corner is located at −10.°0 latitude and 44.°3 longitude. Panel (b) shows examples of impact craters that appear to have experienced viscous relaxation in the north polar region of Enceladus, north of Aladdin Crater and west of Samarkhand Sulci (shown in the global image mosaic of Enceladus (Bland et al. 2018)). The craters exhibit raised floors but have retained their sharp rims, showing how viscously relaxed impact craters are morphologically distinct from mantled impact craters. As shown in panel (c), many craters on Vesta are interpreted to be mantled by regolith (e.g., Marchi et al. 2014), and in some locations, the regolith is thought to be at least 1 km thick (Jaumann et al. 2012; Denevi et al. 2016). An example is shown in an image taken by the Dawn Framing Camera, NASA Photojournal image PIA15822 (NASA/JPL-Caltech/UCLA/MPS/DLR/IDA). Panel (d) displays examples of “muted” impact craters in the equatorial region of Enceladus that may be partly mantled, identified by Kirchoff & Schenk (2009). This figure shows the global mosaic of Enceladus at 8.°5S, 179° W. *The term “muted craters” was used by Kirchoff & Schenk (2009) to describe impact craters that may be partially mantled with plume fallout material, and that also may have experienced some viscous relaxation. Panel (e) presents examples of degraded craters on Callisto. This figure shows a portion of Galileo Solid-State Imaging (SSI) System image 2913r. The largest crater in this panel exhibits a lobate-shaped mass-wasting deposit on the crater floor. Similar mass-wasting deposits have been identified within many of Callisto’s craters (Chuang & Greeley 2000). Panel (f) presents examples of muted craters on Miranda, as shown in part of Voyager 2 ISS image c2684626 (Figure 6(d)).
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Voyager 2 ISS images of Miranda with annotated nomenclature. See Figure A1 for the unannotated version of this figure and Figure A2 for the specific regions covered by each image. (a) Image c2684617 (284 m pixel−1), showing Inverness and Verona Rupes along Miranda’s limb. (b) Image c2684611 (313 m pixel−1), showing Arden and part of Inverness. (c) Image c2684629 (237 m pixel−1), showing Elsinore, Inverness, and the cratered terrain. (d) Image c2684626 (247 m pixel−1), showing Inverness, Arden, and the cratered terrain. (e) Image c2684620 (270 m pixel−1), showing Elsinore and the cratered terrain. (f) Image c2684614 (298 m pixel−1) showing the cratered terrain and small sections of all three coronae.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Annotated Voyager 2 ISS images showing locations of additional regolith and mass-wasting deposits. See Figure 2 for locations of geologic features. (a) Image c2684409 (1151 m pixel−1) showing regolith that appears to mantle scarps within Arden Corona in some locations. (b) A portion of image c2684626 (247 m pixel−1), showing the locations of dark material along crater and scarp walls. (c) A portion of image c2684629 (237 m pixel−1), showing a crater with a central deposit. (d) A portion of image c2684617 (284 m pixel−1), showing the non-muted crater Alonso, which has a central deposit. (e) A portion of image c2684629 (237 m pixel−1) that shows “Crater B” as defined in Croft & Soderblom (1991). The positive topography feature within the crater may be a central mound deposit of regolith, an uplifted floor, or a central peak. (f) A portion of image c2684617 (284 m pixel−1) showing locations of a bright layer, identified by Smith et al. (1986), along the top of scarp walls.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Comparison between muted impact craters and scarps on Miranda’s cratered terrain and cratered terrains on other icy bodies. Examples of craters on other planetary bodies that have been modified by mantling, degradation, and/or viscous relaxation are shown in Figure 4. (a) Muted impact craters (yellow stars) and “muted” scarps (blue arrows) on Miranda, shown in Voyager 2 ISS image c2684629 (Figure 6(c)). (b) Craters on Saturn’s moon Dione, shown in Cassini Imaging Science Subsystem (ISS) image N1714687700_1. (c) Craters on Saturn’s moon Rhea, shown in Cassini ISS image N1734911170_1. (d) Craters on Jupiter’s moon Ganymede, shown in Galileo Solid-State Imaging (SSI) image 3600r. (e) Craters on Saturn’s moon Mimas, shown in Cassini ISS image N1734911170_1. (f) Craters on Pluto’s moon Charon, shown in New Horizons LORRI image lor_0299175682. (g) A portion of Cassini ISS image N1716178094, showing normal faults within Ithaca Chasma on Tethys. (h) A portion of Cassini ISS image N1637520407, showing normal faults within Avaiki Chasmata on Rhea. (i) A portion of Cassini ISS image N1662199979, showing normal faults within the Wispy Terrain on Dione.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Annotated version of Figure 12 in Greenberg et al. (1991), which shows the relative size–frequency distribution (R-plot) of non-muted and muted impact craters within the cratered terrain on Miranda’s Uranus-facing (centered at ∼0° longitude) and anti-Uranus (centered at ∼180° longitude) hemispheres (see Figure 2 for locations of geologic features with respect to these hemispheres). Muted craters that are smaller than ∼7 km are not visible in available images. Larger Log R values correspond to higher spatial densities of craters. Because most impact crater populations throughout the solar system are approximated by a cumulative power law index of −3, this value is chosen for normalization of the data, and deviations from this value appear as variations from a horizontal line. See Barlow (1988) for more details on interpreting crater R-plots. As described in Greenberg et al. (1991), the densities of muted craters on Miranda’s Uranus-facing and anti-Uranus sides are similar, but non-muted crater densities are higher on its Uranus-facing side. Greenberg et al. (1991) notes that there is a concentration of small fresh (and therefore non-mantled) craters in a local region offset from the sub-Uranus point, but the specific location was not provided.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Comparison between the maximum regolith thickness estimates for Miranda and other planetary bodies where regolith layers have been observed and measured. These regolith thickness estimates are for surficial regolith and not megaregolith. Miranda’s regolith thickness estimates derived from crater d-D ratios (Section 3.1), the crater size–frequency distribution (CSFD) of muted craters (Section 3.2), and the central mound within Alonso Crater (Section 3.3) are shown as white stars. *As described in Section 3.3, Miranda’s regolith thickness estimated from the central mound technique may represent an upper limit and has important caveats. **As described in Section 3.1, the highest estimate for regolith thickness within the muted craters (1.2 km) may be most representative of the true thickness in this region.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: (a) A portion of Voyager 2 ISS image c2684626 (Figure 6(d)), in Miranda's cratered terrain. (b) A portion of Voyager 2 ISS image c2684629 (Figure 6(c)), in the cratered terrain between Inverness and Elsinore Coronae. (c) Annotated version of (a) showing the locations of muted and non-muted craters. (d) Annotated version of (b) showing the locations of muted and non-muted craters.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: The d-D ratios of impact craters shown in Figure A3 for the six muted craters (Figure A5) and five non-muted craters (Figure A4 craters). The average d-D ratio estimate for impact craters in general on Miranda is 0.132 (Schenk 1989) (black dots). In comparison with this value, we estimate that the average d-D ratio is ﹩{0.15}_{-0.03}^{+0.02}﹩ for non-muted craters and ﹩{0.10}_{-0.02}^{+0.03}﹩ for muted craters in Miranda’s South Polar Terrain Chasma region (Table 2).
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: (a) Labeled diagram of a non-muted impact crater without the presence of regolith. (b) Diagram of a muted impact crater that is mantled by regolith.
Paper: 3D Radiative-transfer Simulations of the Ejecta Plume Anticipated from DART Impact
Authors: Ludmilla Kolokolova, Jian-Yang Li, 荐扬 李, Mark van Selous, Tony Farnham, Lev Nagdimunov
Figure caption: Geometry of DART ejecta cone (note its hollow nature) and trajectories of the spacecraft. The figure indicates the angles Θplume, Φplume, Θtilt, and Φtilt which describe the geometry of the ejecta cone.
Paper: 3D Radiative-transfer Simulations of the Ejecta Plume Anticipated from DART Impact
Authors: Ludmilla Kolokolova, Jian-Yang Li, 荐扬 李, Mark van Selous, Tony Farnham, Lev Nagdimunov
Figure caption: Mass distribution within the ejecta cone with the time after impact and the distance from the impact location. Mass is calculated in the logarithmic intervals in distance with 3000 bins from 1 to 50,000 m. The red rectangle outlines the moment of the closest approach of LICIACube to Dimorphos considered in the next section.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Spectrum of 122P/de Vico (Cochran & Cochran 2002) showing cometary gas emission lines and the overlap with the LCO SDSS/Pan-STARRS ﹩g^{\prime} ﹩ and ﹩r^{\prime} ﹩ filters. The continuum was not removed by Cochran & Cochran (2002), as 122P was a very high gas-to-dust ratio comet and the continuum was negligible compared to the emission lines. The ﹩r^{\prime} ﹩-filter (red) is free from the strongest cometary gas emission lines, while the ﹩g^{\prime} ﹩ (green) filter captures many of those. This allows for a good estimate of the different distributions of the gas and dust to be measured separately.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption:  A(0°)f ρ values vs. heliocentric distance (<0 for pre-perihelion observations) for returning comet C/2019 L3 (left) and DNC C/2020 R7 (right), using photometry from LOOK with 5″-radius apertures and the ﹩g^{\prime} ﹩ and ﹩r^{\prime} ﹩ filters. C/2019 L3 shows a power-law increase in activity (proportional to ﹩{r}_{h}^{-3.9}﹩ overall), whereas C/2020 R7's activity plateaued after an initial increase. Such differences are expected for returning vs. DNCs (e.g., A’Hearn et al. 1995).
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Heliocentric distances at the time of discovery of all the LPCs discovered after 1801 from the MPC database. The density of points increased significantly after 1996, which is when many of the major moving object sky surveys began.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Network map of LCO facilities.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: Illumination conditions at Site 011 during 2024 December. Areas along traverses are shown as orange boxes; black arrows point toward the center of de Gerlache. Top-left panel: example of a day for which illumination conditions are somewhat favorable for the western portion of the exploration area. Top-right panel: example of a day for which illumination conditions are favorable for the eastern portion of the exploration area. Bottom-left panel: example of a day for which illumination conditions are favorable for the eastern portion of the exploration area. Bottom-right panel: example of a day for which illumination conditions are favorable for the center/overlapping portion of the exploration area.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Fraction of time locations within Site 007 remain below 110 K. (b) Locations within the 2 km EZ in Site 007 which remain 110 K over a period of time. (c) Fraction of time locations within Site 011 remain below 110 K. (d) Locations within the 2 km EZ in Site 011 which remain 110 K over a period of time.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Craters excavating Shackleton and Slater ejecta in Site 007. (b) Ejecta thicknesses of Shackleton and Slater craters on Site 007. Red points are the craters that excavated slater ejecta while blue points are the ones that have sampled Shackleton ejecta. (c) Craters excavating Cabeus and de Gerlache ejecta in Site 011. (d) Ejecta thicknesses of Cabeus and Shackleton craters on Site 011. Green points indicate the craters that excavated Cabeus ejecta and black points are the craters that ecavated de Gerlache ejecta.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Boulder density distribution (500 × 500 m) of the South Ray crater overlaid on NAC images. (b)–(c) Close view of boulders in Site 007. (d)–(f) Boulder along the rim of the de Gerlache crater in Site 011.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Earth illumination map of Site 007. (b) Locations within the 2 km EZ and within the 10 km EZ in Site 007 from whence the Earth is directly visible over a period. (c) Earth illumination map of Site 011. (d) Locations within the 2 km EZ and within the 10 km EZ in Site 011 from whence the Earth is directly visible over a period.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: de Gerlache crater ejecta thickness over Site 011.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Proposed sampling locations within Site 007. (b) Proposed sampling locations within Site 011.