adsabs/AstroCLIMB huggingface dataset:
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: DRACO telescope wavefront error measured at 632.8 nm with a helium neon laser in the interferometer after accounting for the effects of gravity sag on system alignment. This was the final on-axis measurement of the system during alignment before installation of the focal plane.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Contour plot of camera calibration model differences between Star Cal B results (incorporating flight-derived focal length and iFOV values and a distortion with several nonzero parameters) as compared to the pre-launch model (assuming ground-derived focal length and iFOV values and no distortion). The plot has the image origin at the lower left.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Timeline of DART light-curve observations relative to mutual events in the Didymos system and the deep space network (DSN) track used to stream the data back to Earth. The light curve was timed to observe eclipses of both Didymos and Dimorphos.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: DRACO images, aligned on the background stars and then added together to produce a high-SNR image. Didymos can be seen as the streak in the upper right. The image consists of 7478 images obtained over a 9.25 hr period on 2022 September 12.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: A stray light “glow” was observed surrounding bright extended sources. The left column of this figure shows windows of bias-subtracted (for Vega only) and flat-fielded (all) images centered on specific objects. The images in the right column are linearly stretched as follows: Vega (0–300 DN), Jupiter (0–10 DN), Didymos (0–50 DN), Dimorphos (0–50 DN). In the case of Jupiter, Didymos, and Dimorphos, the extent of the “glow” is relatively constant compared to the size of the object, with a maximum value ∼1% of the peak signal. The right column shows the DN levels across the profiles indicated in the left column. On the x-axis, 0 is the center of the profile. The profiles shown for Dimorphos are oriented so as to avoid the halo associated with Didymos. Some of the panels shown in the left column are windows of a larger image. In all cases, the origin of the complete image is at the lower left corner. The north pole of Jupiter is located to the upper right. The north poles of Didymos and Dimorphos are located to the lower left.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Left: brightness measurements of seven stars from 12,900 images of the M34 star cluster, obtained as the stars wandered across the central 512 × 512 pixels of the detector. The image origin is at the lower left, with detector A on the bottom. The colors indicate the variation of each star’s brightness measurement as a percentage difference from the star’s average. The spatial structures show sensitivity differences in both detectors (A and B), as well as differences in the main ghost ring. Right: the same segment of the high-fidelity flat field shown with a linear stretch from 0.9 to 1.1, showing how the regional differences in the left panel align with features in the flat, most noticeably the removed pupil ghost.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Left: original M34 photometry shown in Figure 39. Right: photometry measured from the same images reduced using the new flat field. The photometry in these measurements is consistent across the FOV.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Off-axis PST of the DRACO flight spare unit. Top: PST within 1° of the on-axis position. The performance was well below the requirement and agreed well with predictions. Bottom: PST out to 30° off-axis. Note that the detector noise floor (dashed line) limits the maximum measurable attenuation.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: (a) V magnitude of the star HD 16719 in M34, acquired during the 4 hr Streaming Test activity. The magnitude varied by <0.17% and was consistent between the detector halves to 0.03%. (b) The star wandered across the central 512 × 512 pixels of the detector. No significant differences were observed across the frame. The horizontal line shows the division between detectors A (bottom) and B (top). The color bar shows percentage difference from the average star brightness.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Left: map of the full detector, showing regions identified with sensitivity differences. The labels indicate the average difference within each region and represent the correction factor that is applied to the high-fidelity flat. Right: the new flat field, with the correction factors included.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Graphical overview of the DRACO image calibration pipeline.
Paper: Where Is That Crater? Best Practices for Obtaining Accurate Coordinates from LROC NAC Data
Authors: Robert V. Wagner, Megan R. Henriksen, Madeleine R. Manheim, Heather M. Meyer, Maria E. Banks, Erick Malaret, Erwan Mazarico, Emerson J. Speyerer, Mark S. Robinson
Figure caption: Top and middle: plots of NAC absolute offsets vs. time for 15 spacecraft landing/impact sites with well-constrained true positions (Wagner et al. 2017). All sites are on the lunar nearside, within 40° of the equator. The top panel shows offsets as an angular pointing error in degrees of spacecraft orientation error (assuming no spacecraft position error); the middle panel shows the offsets as meters on the surface (i.e., not adjusted for spacecraft altitude). All points are measured using smithed SPKs. Bottom: the evolution of the LRO periapse and apoapse over the same period as the top panels. Source data are available in Data behind the Figure, along with image and object IDs, observed coordinates, and offsets in both cross- and down-track directions.(The data used to create this figure are available in the                       .)
Paper: Where Is That Crater? Best Practices for Obtaining Accurate Coordinates from LROC NAC Data
Authors: Robert V. Wagner, Megan R. Henriksen, Madeleine R. Manheim, Heather M. Meyer, Maria E. Banks, Erick Malaret, Erwan Mazarico, Emerson J. Speyerer, Mark S. Robinson
Figure caption: Portion of the README file for NAC_DTM_NEWCRATER4 (available at https://wms.lroc.asu.edu/lroc/view_rdr/NAC_DTM_NEWCRATER4), with key accuracy metrics and special processing note highlighted.
Paper: Where Is That Crater? Best Practices for Obtaining Accurate Coordinates from LROC NAC Data
Authors: Robert V. Wagner, Megan R. Henriksen, Madeleine R. Manheim, Heather M. Meyer, Maria E. Banks, Erick Malaret, Erwan Mazarico, Emerson J. Speyerer, Mark S. Robinson
Figure caption: Box plots showing positioning uncertainties for LROC NAC DTMs created by the LROC team, grouped by the year in which the DTM was produced. The offsets are measured relative to LOLA data. Red lines indicate desired accuracies for elevation, latitude, and longitude.
Paper: Where Is That Crater? Best Practices for Obtaining Accurate Coordinates from LROC NAC Data
Authors: Robert V. Wagner, Megan R. Henriksen, Madeleine R. Manheim, Heather M. Meyer, Maria E. Banks, Erick Malaret, Erwan Mazarico, Emerson J. Speyerer, Mark S. Robinson
Figure caption: Positions of Lunar Ranging Retroreflector at the Apollo 11 landing site as measured from 57 NAC images. Background image (M175124932R) and red filled circle are aligned to the true coordinates (Wagner et al. 2017); circle colors indicate the mission phase. Horizontal span of points is ∼40 m; vertical span is ∼50 m.
Paper: Where Is That Crater? Best Practices for Obtaining Accurate Coordinates from LROC NAC Data
Authors: Robert V. Wagner, Megan R. Henriksen, Madeleine R. Manheim, Heather M. Meyer, Maria E. Banks, Erick Malaret, Erwan Mazarico, Emerson J. Speyerer, Mark S. Robinson
Figure caption: Flowchart showing the best data products to use for measuring accurate locations. The left column shows the best products to use when finding coordinate locations of features nearing the size of the pixel scale. The right column shows the best product to use when elevations are required, as well as horizontal coordinates. The individual LOLA points used to make the improved LOLA DTMs (available for some south polar locations) are more accurate than the NAC DTMs; however, because LOLA DTMs are interpolated between those points, the NAC DTMs are generally more detailed (except in shadows). The NAC DTMs also have associated orthophotos to aid with feature identification.
Paper: Where Is That Crater? Best Practices for Obtaining Accurate Coordinates from LROC NAC Data
Authors: Robert V. Wagner, Megan R. Henriksen, Madeleine R. Manheim, Heather M. Meyer, Maria E. Banks, Erick Malaret, Erwan Mazarico, Emerson J. Speyerer, Mark S. Robinson
Figure caption: Reporting coordinates of a site. Report includes an image of the target, geographic coordinates to an appropriate number of decimal places, and pixel coordinates of the site within a raw NAC image. The landing ellipse (red circle) has a radius of 25 m. The image is ∼200 m across.
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: Premission strategic planning. The Science Operations Teams identified four main surface units in the mission area (a) and a starting location for the mission (light blue marker). The UAS Science Operations Team identified regions of interest for each surface unit (colored outlines, (a)) and developed a draft mission plan (white flight lines and green landing markers, (a)) in order to achieve the mission objectives in the prescribed timeline. The UAS landing suitability map (b) was created by combining three different ground surface parameters using the DEM. Darker green represents more suitable landing locations, lighter green represents less suitable locations, and areas with no data are unsuitable for landing. The (a) orthomosaic and (b) DEM hillshade base maps are from a 2015 survey by Loftmyndir ehf. and a 2018 UAS survey (S. P. Scheidt & C. W. Hamilton 2021). The black dashed line is the road used to access the site. Surface unit polygons are modified from J. R. C. Voigt et al. (2021a). The landing suitability analysis was conducted using the more detailed 2018 UAS survey, which only covered the lava flow margin in the southern half of the map extent.
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: UAS mission. The UAS mission consisted of nine flights (colored solid lines) and six unique landing locations (green circles). Three samples were collected at the sol 102, sol 105, and sol 110 landing locations (red circles). White circles are targets specifically identified in planning for oblique airborne imaging. Mapping surveys were conducted on sols 101, 102, and 105 (dashed outlines). The sample cache was located at the shared landing site of the sol 104, 109, and 112 flights. The sol labels show the location of the UAS at the end of each mission sol. The base map is from a UAS survey of the field site conducted concurrently with (but not as a part of) mission implementation. The coordinate grid has a 500 m interval in WGS 84 UTM Zone 28N.
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: Location of Holuhraun. (a) The Holuhraun region and 2014–2015 lava flow field are located in the central highland of Iceland (yellow box). (b) The UAS mission was implemented along a stretch of the north-central flow-field margin (red box), while science operations were conducted at Dreki, near Askja volcano (star). (c) An airborne image taken from the northeast corner of the red box in (b) looking to the southwest shows the sand sheet in the foreground and 2014–2015 lava flow field in the background.
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: Surface textures in the UAS mission area. (a) Oblique image from sol 101 showing the smooth sediment surface in a topographic low scattered with light-toned boulders. (b) Nadir descent image showing the sol 102 landing area from an altitude of ∼40 m. Lighter and darker sediments are visible as part of a series of ripples. (c) The scoop sampler collects the sol 103 sample and exposes darker sediment beneath the surface. (d) Oblique image of the rougher surface of the younger lava from sol 104. The arrow shows the flow direction of a smoother texture lava breakout from the margin of a region of rougher texture. (e) Oblique image of the smoother surface of the younger lava from sol 104. The arrows show flow direction away from a crease structure located between the arrows. The green circle is the sol 105 landing site. All scale bars are approximate for the center of the oblique images. The scoop in (c) is ∼10 cm wide.
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: Observations from oblique images. (a) The younger lava interior is higher in elevation compared to the margin, and the smoother surface texture is also more continuous and extensive on the interior plateau compared to the margins. Rougher surfaces are located between the interior and margin. Image is from sol 104. (b) Smoother lava texture on a flow margin lobe where the UAS landed on sol 110 (green circle). Image is from sol 109. (c) Pockmarked terrain texture formed by blocks of the older lava protruding through the sand sheet. Sediment is preferentially deposited on the downwind side of larger outcrops, indicating a northeasterly wind direction (arrows). Image is from sol 101. (d) A transition between smoother and rougher texture in the younger lava from sol 112. All scale bars are approximate for the center of the oblique images.
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: Lava landings sols 106–108. (a) Descent image of the sol 105 younger lava landing site (green circle) taken at an approximate altitude of 30 m. The arrow indicates the look direction of (b). (b) Landed image from sol 105 looking south and showing folds on the flow surface with relief of 10–30 cm. (c) Microimage of the younger lava at the sol 105 landing site. The image is ∼10 cm wide. (d) Ascent image from sol 109 taken at 40 m altitude showing the white discoloration where the UAS landed on sol 108 (arrow).
Paper: Evaluating the Use of Unoccupied Aircraft Systems (UASs) for Planetary Exploration in Mars Analog Terrain
Authors: Brett B. Carr, Matthew Varnam, Nathan Hadland, Jahnavi Shah, Joana R. C. Voigt, Samantha Gwizd, Kathryn M. Stack, Fred Calef, Raymond Francis, Udit Basu, Baldur Björnsson, Colin X. Chen, Elisa Dong, Jeffrey E. Moersch, Michael Phillips, Joshua Springer, Catherine D. Neish, Christopher W. Hamilton
Figure caption: Resolution of analog orbiter and UAS mission data products. Surveys and images from the UAS mission significantly improved on the resolution of analog orbiter orthomosaics and DEMs. A location in the northern half of the UAS survey conducted on sol 105 near the sol 104 landing site (Figure 3) is shown in the (a) 0.25 m pixel–1 orbital analog orthomosaic, (b) 1.0 m pixel–1 orbital analog DEM, (c) 0.09 m pixel–1 UAS survey orthomosaic, and (d) 0.3 m pixel–1 UAS survey DEM. This location includes a rougher younger lava surface on the right side, a smoother younger lava surface in the upper center to lower left, and the sand sheet in the upper left. No oblique airborne images were taken by the UAS at this location, but similar terrain nearby was captured in images showing (e) the sand sheet mantling smoother lava in a sol 102 image at 40 m altitude and (f) the rougher lava in a sol 104 image at 60 m altitude. Scale bars in (e) and (f) are approximate for the center of the oblique images. Additional details observable in the UAS data (c)–(f) allowed for interpretations not possible with the orbital analog data (a)–(b) alone.