adsabs/AstroCLIMB huggingface dataset:
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Overview of the geographic and geological key features in Elysium Planitia on Mars. Overlaid on color-coded Mars Global Surveyor (MGS) Mars Orbital Laser Altimeter (MOLA) data, this map highlights the main lava flow-fields, nearby mission landings sites (InSight as an orange star and Curiosity as red star), and the Cerberus Fossae. Modified after J. R. C. Voigt et al. (2023).
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: PSR cumulative size–frequency distribution (left) and cumulative area–frequency distribution (right) for 80°–90°N (solid thick black line) and 80°–90°S (dotted black line). In each panel, the total north polar distribution (solid thick black line) is compared to that in nine equal-area annuli moving out from the north pole (dark blue to red thin lines) with outer radii of 101.33, 143.31, 175.51, 202.67, 226.59, 248.21, 268.10, 286.61, and 304.00 km.
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: Solid lines: median and interquartile range of standardized roughness at various baselines (labeled in meters) as a function of 1600 m-baseline slope in 40 highland NAC DEMs at all latitudes. The shaded region is the interquartile range for the 50 m LOLA roughness in the highlands at absolute latitudes <60°.
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: Hurst exponent over 100–800 m baselines (1 km pix−1). The color scale ranges from the 2nd to the 98th percentile. Right: same as Figure 9, but for the Hurst exponent of the k-means classes.
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 standardized roughness as a function of topographic slope at 1600 m baseline. Each panel shows the roughness for a particular baseline (50–1600 m) with curves colored by Tavg for the 2nd, 10th, 25th, 50th, 75th, 90th, and 98th percentiles of Tavg. The shaded region and error bars represent the interquartile ranges.
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: South polar standardized roughness as a function of topographic slope at 1600 m baseline. Each panel shows the roughness for a particular baseline (50–1600 m) with curves colored by Tavg for the 2nd, 10th, 25th, 50th, 75th, 90th, and 98th percentiles of Tavg. The shaded region and error bars represent the interquartile ranges.
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: Solid lines: median and interquartile range of standardized LOLA roughness at various baselines (labeled in meters) as a function of 1600 m-baseline slope in the north (left) and south (right) polar regions.
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: Total area within each k-means class for the north and south polar regions with Poisson error bars.
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: Box plots of LOLA 1064 nm normal albedo (left) and 1600 m-baseline slope (right) for the k-means classes. Each box shows the median (horizontal line), mean (plus symbol), interquartile range (box edges), and 9th/91st percentiles (whiskers).
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: New 20 m pix−1 map of PSRs within 80°–90°N.
Paper: Implications of Differentiated Late Accretion for the Volatile Inventory of the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Varun Manilal
Figure caption: Contribution of differentiated late accretion via a (A) 1% ME and (B) 3% ME impactor to the C–N–H–S–Se–Te of the BSE at IW–4, IW–2, and IW–1. The contribution to the C–N–H inventory of the BSE was limited, whereas the entire S–Se–Te inventory could be established. Note that the symbols for S–Se–Te overlap.
Paper: Implications of Differentiated Late Accretion for the Volatile Inventory of the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Varun Manilal
Figure caption: Fractional distribution of C–N–H–S–Se–Te between the atmosphere, MO, and core of a (A) 1% ME and (B) 3% ME impactor at IW–4, IW–2, and IW–1. The impactor’s MO-degassed atmosphere contains the majority of the C–N–H inventory, whereas most of the S–Se–Te resides in its core. Note that the symbols for C–N–H and S–Se–Te overlap at IW–2 and IW–1.
Paper: Implications of Differentiated Late Accretion for the Volatile Inventory of the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Varun Manilal
Figure caption: Comparison of C–N–H–S–Se–Te abundances in the BSE with the contribution of a chondritic late accretion event comprised of 0.3%–0.5% ME of CM and EL chondrites. Data sources: (1) BSE: C (B. Marty et al. 2020); N and H (M. M. Hirschmann 2018); S, Se, and Te (Z. Wang & H. Becker 2013). (2) CM and EL chondrites: C, N, H, S, Se, and Te (C. M. O. Alexander 2022). Note that the H content of EL chondrites (represented by a downward-pointing arrow) is assumed to be near zero (C. M. O. Alexander 2022). The error bars for the BSE represent one standard deviation from the mean values. The shaded regions for CM and EL chondrites indicate the lower and upper bounds, based on contributions of 0.3% and 0.5% ME, respectively, from chondritic materials.
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: Average NIR spectrum of Gault from this study with the RELAB laboratory spectra of potential meteorite analogs Dhajala (RELAB c1dp11, H3.4), Suwahib (c1tb124, H3.7), and Kabo (c1tb136, H4). All three meteorites have minimal thermal metamorphism (H3.4–H4) and were among the best analogs in the RELAB database as measured with a χ2 analysis by M4AST. A mineralogical comparison of these meteorites with Gault’s average mineralogy can be found in Table 3.
Paper: Implications of Differentiated Late Accretion for the Volatile Inventory of the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Varun Manilal
Figure caption:  ﹩{D}_{{i}}^{{\rm{metal}}/{\rm{silicate}}}﹩ values of C–N–H and S–Se–Te at IW​​​​​​−4, IW−2, and IW−1. The ﹩{D}_{{i}}^{{\rm{metal}}/{\rm{silicate}}}﹩ of C and H increase with decreasing fO2, whereas those of N decrease. The ﹩{D}_{{i}}^{{\rm{metal}}/{\rm{silicate}}}﹩ values of S–Se–Te are broadly similar at IW−2 and IW−1, whereas those at IW−4 are an order of magnitude lower.
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 evolution of incoming stellar radiation at the top of the atmosphere (STOA, panel (a)), surface temperature (b), and vertically integrated water vapor (c) and ozone column densities (d) on Proxima Centauri b in a 1:1 SOR (solid lines) and a 3:2 SOR (dashed lines) over 120 days, corresponding to almost 11 orbits. Orange and blue lines indicate the 0∘ and 180∘ hemispheres, respectively. The global average values are shown as the black line. From the peaks in STOA, we identify the periastron and apastron passages for the 3:2 SOR, denoted as the dotted and dash–dotted gray vertical lines and specified on the x-axis. The separation between two successive periastron or apastron passages represent an orbital period for Proxima Centauri b, independent of the exact 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: Synthetic emission spectra using different orbital phase angles for (a) Proxima Centauri b in a 1:1 SOR and (b) Proxima Centauri b in a 3:2 SOR. Colors represent the orbital phase and the corresponding time step of the simulation, using daily output (see Table 2). We use PSG with the GlobES 3D mapping tool to translate 3D CCM data into synthetic emission spectra.
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: Temporally averaged chemical lifetimes for ozone in the planet in a 3:2 SOR. We show the Chapman termination reaction (R4) in black and the rate-limiting steps of the dominant HOx cycles in blue (R9) and cyan (R11). The lifetimes are calculated as spatial means for the equatorial region (15∘S–15∘N), the northern high latitudes (60∘N–90∘N, and the southern high latitudes (90∘S–60∘S), based on the spatial distributions in Figure 4. The gray line shows the timescale between periastron and apastron passage (5.593 days).
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: Zonal-mean meridional distribution of the mole fraction ﹩{\chi }_{{O}_{3}}﹩ for (a) Proxima Centauri b in a 1:1 SOR, and (b) Proxima Centauri b in a 3:2 SOR, both temporally averaged. Overplotted black contour lines correspond to the age-of-air tracer in days, to diagnose atmospheric circulation. The age-of-air tracer is initialized at 0 s everywhere and reset whenever a parcel of air reaches the lowest atmospheric layers (below ~2km or P >  700 hPa). In this way, the age-of-air tracer measures the amount of time (in days) since an air parcel was last found in the lowest layers of the atmosphere, probing the main features of the atmospheric circulation.
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 vertically integrated H2O(g) column density for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere.
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: Orbital evolution (not to scale) of phase angles and corresponding surface temperature distributions on emission disks as observed by a distant observer. Proxima Centauri b at an orbital inclination of 70∘ is shown in (a) a 1:1 SOR and (b) a 3:2 SOR. The temperature ranges vary with the time step, as indicated by the upper limit of the color maps.
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 vertically integrated OH column density for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere.
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: Simulated LFRs for Proxima Centauri in a 1:1 SOR (PCb 1:1) and a 3:2 SOR (PCb 3:2). By showing both the zonal-mean meridional distribution in panel a and meridional-mean zonal distribution in panel b, we show that lightning flashes are contained to the dayside hemisphere for planets in a 1:1 SOR and are found on both hemispheres for planets in a 3:2 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: Mean vertically integrated NO3 column density for Proxima Centauri b in (a) a 1:1 SOR, (b) a 3:2 SOR with daytime on the 0∘ longitude hemisphere, and (c) a 3:2 SOR with daytime on the 180∘ longitude hemisphere.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: A comparison of the spectra and gaseous SNRs for an exo-Earth with varying amounts of cloud abundance. The high, mean, low cloud abundance labels correspond to exo-Earth atmospheres constructed using MERRA-2 data from the dates 1999 July 7, 2011 January 20, and 1987 February 15 respectively. A clear sky scenario is also shown for reference. The simulations are done with a 6 m HWO template with an exposure time of 24 hr considering that the planet is 10 pc away and placed at quadrature. The reflected light continuum and the atmospheric SNRs increase with cloud abundance.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: The planetary and optical throughputs for all the four instruments considered for the comparison.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Three different numerical simulations of Phobos’s passage through the 3:1 tesseral resonance with the rotation of Mars at 2.9 RM. The slightly different initial conditions were chosen so as to result in the present orbit of Phobos after this resonance. The changes in Phobos’s e and i during this resonance passage are consistent across many simulations, enabling us to estimate Phobos’s precrossing orbital parameters with confidence. Under our standard model assumptions (QM = 80, k2M = 0.14), this crossing happened about 16 Myr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Three different numerical simulations of Phobos’s passage through the Touma (2:3) semisecular resonance with the Sun at 2.94 RM in a model with a fixed orbit of Mars. The purple line shows a case with initial i = 0 that has an eccentricity that is too low for resonance capture. The green line plots the case with higher initial e that results in resonance capture. A case with the same initial e but also substantial i also avoids capture (cyan). Using standard assumptions, this crossing happened about 20 Myr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Different resonances potentially encountered by Phobos in the past. Tesseral resonances with the rotation of Mars are plotted in red, semisecular resonances with the Sun in teal, and MMRs with Deimos in purple. While the tesseral and Deimos resonances are labeled by the ratio of Phobos’s mean motion to the Martian rotation rate and Deimos’s mean motion, respectively, semisecular resonances are quantified by the ratio of Phobos’s apsidal precession rate to the Martian mean motion. The dashed line shows the present semimajor axis of Phobos.
Paper: In Search of the Potentially Hazardous Asteroids in the Taurid Resonant Swarm
Authors: Jasmine Li, Quanzhi Ye, 泉志 叶, Denis Vida, David L. Clark, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Frank J. Masci, Josiah Purdum, Benjamin Racine, Avery Wold
Figure caption: Simulated Taurid swarm asteroids with V < 21 (blue dots) and ZTF footprint (filled orange squares) on 2022 October 29 and 31. The ZTF search covers 99% of the simulated asteroids. The locations of the Sun and the Moon are marked with a yellow circle and a gray half-filled circle, respectively.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Generation of the initial hypothesis map. Top: flowchart summarizing the data and data products used to produce the geologic origin cube, uncertainty map, and photogeologic map. Bottom: conceptual image of the geologic origin cube. The x- and y-axes correspond to spatial dimensions on the map, and each plane represents a different geologic origin. The likelihood of a geologic origin for a location increases with pixel value. Conversely, uncertainty increases with the number of layers having a value greater than 0 at a location. For any particular pixel, the more layers having a value. The rover disambiguates the geologic origin for each terrain by visiting regions of high uncertainty. Six different geologic origins were considered (four are shown for illustrative purposes). As the rover queries the terrain, it updates the hypothesis map and then uses the updated map to plan the next leg of the traverse.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Tetracorder fitting procedure. (a) A few examples are shown out of hundreds of compounds and mixtures that are continuum removed and fitted (b) to the unknown spectrum (red) using a modified least-squares procedure. Green boxes are the continuum wavelengths for the specific 2.2 μm feature in each library spectrum. Blue lines represent the continuum used for continuum removal. In this example, this spectral region only shows absorption due to kaolinite, but other regions may show absorptions due to other compounds, enabling many compounds to be found in a spectrum. From R. N. Clark et al. (2003), public domain images.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Site 1. (a) RGB color composite image of the site showing three dominant color units: the Black Point Lava Flow near the top, the reddish Moenkopi shale left of center, and the tan Kaibab rocks at the bottom. North is up. (b) View of the Black Point Lava Flow in the distance from the Kaibab formation. The boulder in the foreground is about 30 cm across. (c) The rover on red Moenkopi shale.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Site 2. (a) RGB composite of the Blue Canyon. Yellow inset location of inset. (b) Inset showing the tan Dakota Sandstone at the bottom of the image and the dark, layered Mancos Shale at the top. North is to the top left. (c) The rover traversing rugged terrain in the Mancos Shale.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Science interpretation algorithm to constrain geologic origin. Detection of minerals (where abs = absorption) with few possible origins or multiple minerals with similar origins increases the confidence in geologic origin, whereas detection of single minerals with multiple possible origins increases the uncertainty.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: (a) RGB composite of the Yellow Cat Flat. The yellow outline denotes the site boundaries. (b) Aerial view of the northwest portion of the field site, showing strong color variability exposed at the site. (c) Eastward view across the field site to the cliff-forming Yellow Cat member.