adsabs/AstroCLIMB huggingface dataset:
Paper: Validation of the Survey Simulator Tool for the NEO Surveyor Mission Using NEOWISE Data
Authors: Joseph R. Masiero, Dar W. Dahlen, Amy K. Mainzer, William F. Bottke, Jennifer C. Bragg, James. M. Bauer, Tommy Grav
Figure caption: Detections of NEO 2020 TK3 in the NEOWISE Reactivation Year 7 data that were identified by the NSS. This object was seen in two sequential image sets (top and bottom) with center times separated by only 11 s. The left and right columns show the W1 and W2 images for each detection, respectively, and the NSS-predicted position for the object is marked by the colored circle overlaid on each image. The object was moving at 70.5 deg day−1 at the time of observation; it is noticeably trailed in the 7.7 s long W2 exposures, and motion with respect to the background is apparent. Detection 2 is near the edge of the field of view, resulting in the image being cut off in the figure.
Paper: Validation of the Survey Simulator Tool for the NEO Surveyor Mission Using NEOWISE Data
Authors: Joseph R. Masiero, Dar W. Dahlen, Amy K. Mainzer, William F. Bottke, Jennifer C. Bragg, James. M. Bauer, Tommy Grav
Figure caption: Histogram showing the comparison of NSS-predicted astrometric positions in R.A. (blue) and decl. (orange) to the measurements reported to the MPC for 1,624,795 detections of 128,462 main belt asteroids observed by NEOWISE during the 2010 fully cryogenic mission. The vertical dashed lines show the offset and 3σ scatter provided by MPC’s analysis of observation residuals for the submitted C51 observations to predictions from orbits of known objects. The offsets and random scatter in the observation error from the NSS code are comparable to the values found by the MPC’s analysis.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: Arc length of NEOs discovered by the NEOWISE mission at the time that the MPC issued a Minor Planet Electronic Circular, which we use as a proxy for the object having sufficient data to constrain an orbit. Vertical dotted lines indicate 14 and 28 days. In total, 89% of the NEOs discovered by NEOWISE had arcs less than 14 days, while 99% had arcs less than 28 days.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: Left: NEO Surveyor detections of PHAs larger than 140 m for 5 yr of observations as a function of sky position. The density of detections is greatest in the direction of the Sun. Right: detections of MBAs for 5 yr of observations. In both figures, the bands of enhanced detections are the result of small overlaps between Stacks.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: Top: distribution of track lengths for NEAs ≥140 m found by NEO Surveyor. Bottom: distribution of lengths of individual tracklets for these objects.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: Top: distribution of phase angles for NEAs detected over the 5 yr baseline mission, grouped by size. Bottom: number of detections per NEA as a function of size.
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: Left panel: diurnal cycle of the surface temperatures at two latitudes, dotted lines at 45° north and solid lines at 0°, and two longitudes in orange at 0° west longitude and blue at 90° west longitude (from Bauch et al. 2021). The arrows with numbers at the top of the left panel correspond to the approximate respective positions displayed in the right panel. Right panel: position of the 0° west longitude in orange and the 90° west longitude in blue in the orbital plane of Mercury around the Sun during the first year (top panel for positions numbered 1–6) and during the second year (bottom panel for positions numbered 7–12; adapted from Langevin 1997). The gray ellipse represents the orbit of Mercury around the Sun as seen from the north.
Paper: Libration- and Precession-driven Dissipation in the Fluid Cores of the TRAPPIST-1 Planets
Authors: Dhananjhay Bansal, Hannah S. Christie, Mathieu Dumberry
Figure caption: Orbital inclination (I), mantle obliquity (ε  m ), and fluid core spin offset (θ  c ) as a function of time for each TRAPPIST-1 planet resulting from secular perturbations.
Paper: Libration- and Precession-driven Dissipation in the Fluid Cores of the TRAPPIST-1 Planets
Authors: Dhananjhay Bansal, Hannah S. Christie, Mathieu Dumberry
Figure caption: Eccentricity (left scale) and libration amplitude (right scale) as a function of time for each TRAPPIST-1 planet resulting from secular perturbations.
Paper: Libration- and Precession-driven Dissipation in the Fluid Cores of the TRAPPIST-1 Planets
Authors: Dhananjhay Bansal, Hannah S. Christie, Mathieu Dumberry
Figure caption: Dissipation induced by libration in the fluid core of each TRAPPIST-1 planet.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: New Horizons CA06 LORRI and CA04 LORRI mosaics of Arrokoth (left) and the same observations overlain with geologic mapping (right). The mapped geologic units and lineations are defined in the legend. The white dots on the geologic maps indicate the approximate location of the maximum principal axes of inertia for the larger lobe Wenu (Keane et al. 2022). If Wenu were once an isolated body, separate from Weeyo, this axis would correspond to its former spin axis. The blue and red arrows annotating the CA04 mosaic indicate notches on the limbs of the lobes Weeyo and Wenu, respectively.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: (a) CA05 MVIC color observation of Arrokoth, with three MVIC broadband filters registered to the nearest-integer pixel and displayed in order of increasing wavelength, with 400–550, 540–700, and 780–975 nm filters displayed in blue, green, and red, respectively. (b) The same, but with the pixels selected for inclusion in individual mound ROIs highlighted and labeled.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: Comparison of mound properties measured from New Horizons CA04 (squares) and CA06 (circles) observations of Arrokoth. The apparent area, aspect ratio, length, and width are shown in panels (A)–(D), respectively. The gray points denote mounds that are viewed obliquely and present little surface area to the viewer.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: Cumulative normal reflectance distributions of Wenu's nine largest (i.e., most aerially extensive) mounds. Overall, all are photometrically similar. Differences are discussed in the text.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: New Horizons CA06 LORRI image of Arrokoth, depicting its construction from two lobes, Wenu and Weeyo. Wenu, the larger lobe, displays prominent mound units. Other named features that we refer to in the text are noted.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: Comparison of the final object obtained in the nominal simulation with the CA06 version of the geological map of Wenu from Figure 2. The smaller central mounds in the simulation contrast with Arrokoth itself, which displays its largest mounds at the lobe center. This testifies to the need for future work.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: Cumulative color distributions for the mound ROIs. A redder color distribution plots farther to the right. The dashed black curve simulates the effect of MVIC's known noise characteristics for mound tl, indicating that the apparent breadth of the mound's color distribution is entirely attributable to image noise.
Paper: The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
Authors: S. A. Stern, O. L. White, W. M. Grundy, B. A. Keeney, J. D. Hofgartner, D. Nesvorný, W. B. McKinnon, D. C. Richardson, J. C. Marohnic, A. J. Verbiscer, S. D. Benecchi, P. M. Schenk, J. M. Moore
Figure caption: Three snapshots from the nominal PKDGRAV simulation of Wenu's accretion from 30 progenitors ∼5 km in diameter.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: South polar stereographic map of PV (shading) and zonal winds (black contours) on the 300 K surface in dust simulations, averaged over 30 sols either side of the winter solstice. λ = 1 shows absolute PV and zonal wind, and all other panels show the PV and wind anomaly from λ = 1 for the given value of λ. The purple contour indicates the latitude of maximum PV (ϕ PV).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: South polar stereographic map of PV (shading) and zonal winds (black contours) on the 300 K surface in current-eccentricity simulations, averaged over 30 sols either side of the winter solstice. ε = 25 shows absolute PV and zonal wind, and all other panels show the PV and wind anomaly from ε = 25 for the given value of ε. The purple contour indicates the latitude of maximum PV (ϕ PV).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: South polar stereographic map of PV (shading) and zonal winds (black contours) on the 300 K surface in zero-eccentricity simulations, averaged over 30 sols either side of the winter solstice. ε = 25 shows absolute PV and zonal wind, and all other panels show the PV and wind anomaly from ε = 25 for the given value of ε. The purple contour indicates the latitude of maximum PV (ϕ PV).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: North polar stereographic map of PV (shading) and zonal winds (black contours) on the 300 K surface in dust simulations, averaged over 30 sols either side of the winter solstice. λ = 1 shows absolute PV and zonal wind, and all other panels show the PV and wind anomaly from λ = 1 for the given value of λ. The purple contour indicates the latitude of maximum PV (ϕ PV).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Northern winter mean meridional streamfunction averaged over 30 sols either side of the winter solstice for γ = 0.093. ε = 25 shows absolute value of ψ, and all other panels show the anomaly from ε = 25 for the given value of ε.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Northern winter mean meridional streamfunction averaged over 30 sols either side of the winter solstice for dust-scale simulations. ε = 25 shows absolute value of ψ, and all other panels show the anomaly from ε = 25 for the given value of ε.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Southern winter mean meridional streamfunction averaged over 30 sols either side of the winter solstice for γ = 0.093. ε = 25 shows absolute value of ψ, and all other panels show the anomaly from ε = 25 for the given value of ε.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Southern winter mean meridional streamfunction averaged over 30 sols either side of the winter solstice for γ = 0. ε = 25 shows absolute value of ψ, and all other panels show the anomaly from ε = 25 for the given value of ε.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Northern winter mean meridional streamfunction averaged over 30 sols either side of the winter solstice for γ = 0. ε = 25 shows absolute value of ψ, and all other panels show the anomaly from ε = 25 for the given value of ε.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: A time series of winter-time polar temperature (latitudinally weighted average temperature over 75°–90° N/S on the 50 Pa surface) according to historical integrations of obliquity. Winter mean is 60 sols averaged about L  s  = 270° (L  s  = 90°) in the northern (southern) hemisphere. (a) Obliquity from Laskar et al. (2004; data obtained at http://vo.imcce.fr/insola/earth/online/mars/mars.html), and temperature changes with obliquity in (b) the northern hemisphere and (c) the southern hemisphere. We have chosen to include only variations based on obliquity owing to the complication of the timing of perihelion with varying eccentricity also, although we show the time series for both γ = 0.093 (solid blue) and γ = 0.000 (dashed red).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter polar temperature (latitudinally weighted average temperature over 75°–90° N/S on the 50 Pa surface) in the northern (left) and southern (right) hemispheres. Winter mean is 60 sols averaged about L  s  = 270° (L  s  = 90°) in the northern (southern) hemisphere. Top: obliquity simulations; bottom: dust-scale simulations.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Southern winter mean meridional streamfunction averaged over 30 sols either side of the winter solstice for dust-scale simulations. ε = 25 shows absolute value of ψ, and all other panels show the anomaly from ε = 25 for the given value of ε.
Paper: Dynamical Interactions and Mass Loss within the Uranian System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Results of the particle injection and survival for the dynamical simulations, showing the outcome after 106 yr (top panel) and 107 yr (middle panel). The horizontal axis is the separation from Uranus in planetary radii, and the vertical axis shows the percentage of the total dynamical simulation that particles survived at that location, represented by the green line. The vertical dotted lines represent the semimajor axes of the major moons, and the vertical dashed lines represent the locations of the rigid and fluid Roche limits. The bottom panel shows the change in eccentricity that occurs for each particle as a function of its initial semimajor axis during the course of the 107 yr simulations.
Paper: Dynamical Interactions and Mass Loss within the Uranian System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Eccentricity as a function of time for the Uranus major moons of Miranda, Ariel, Umbriel, Titania, and Oberon. The eccentricity values were recorded every 100 yr during a 106 yr simulation, as described in Section 3.
Paper: Dynamical Interactions and Mass Loss within the Uranian System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Results of the 107 yr particle injection at higher resolution in the semimajor axis range of 1–5 Uranus radii. As for the top two panels of Figure 3, the green line represents the percentage survival of the injected particle, the vertical dashed lines represent the Roche limit locations, and the blue vertical dotted line represents the semimajor axis of Miranda. The black vertical dotted lines indicate the locations of some MMR locations, corresponding to the values provided in Table 1.
Paper: Dynamical Interactions and Mass Loss within the Uranian System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Loss rate for the injected particles into the Uranus system, shown as a function of time (fractions of 107 yr) and the percentage of particles that survive.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: Top: global map of the 1.05 μm absorption band depth variation on Bennu (Simon et al. 2020a). Bottom: Apophis and Bennu visible–NIR global spectra compared to their closest meteorite analogs. Spectral signatures of Apophis and LL chondrites are distinctive in the visible–NIR and should be easily measured by OVIRS. RELAB IDs for meteorite data include DP-JNG-015/BKR1DP015, DP-JNG-007/BKR1DP007, MT-PFV-137-A/BKR1MT137A CM2, and PH-D2M-032/BKR1PH032.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: Top: NavCam image taken 87 s after the sample collection event, showing the regolith disturbance caused by the OREx spacecraft thrusters. Thruster tracks are indicated by the dashed lines. Bottom: DTM of the OSIRIS-REx sampling site after the TAG event, showing where the thrusters excavated surface material around the central crater. (Image by NASA/Goddard/SVS using data from Lauretta et al. 2022.)