adsabs/AstroCLIMB huggingface dataset:
Paper: Solar Wind Sputtering of Secondary Ions from Water-ice-covered Regolith Analogs
Authors: Micah J. Schaible, Gabriella K. Dotson, Roshan Trivedi, Advik D. Vira, Kevin P. Hand
Figure caption: SSI spectra for SiO2 at room temperature before cooling (green), after depositing ∼50 monolayers of D2O (black), and after sputtering the dosed sample to a fluence >3 × 1016 H﹩{}_{2}^{+}﹩ cm–2 (red). While SiOH+ is the dominant Si-containing molecular ion at room temperature, only water-group ions are seen in the freshly dosed sample, and SiOD+ is slightly more abundant than SiOH+ in the dosed–sputtered spectra due to radiation-induced interactions between the deposited molecules and the underlying substrate.
Paper: Solar Wind Sputtering of Secondary Ions from Water-ice-covered Regolith Analogs
Authors: Micah J. Schaible, Gabriella K. Dotson, Roshan Trivedi, Advik D. Vira, Kevin P. Hand
Figure caption: Secondary ion spectra for SiO2, normalized to Si+, at room temperature before dosing (green), after dosing the sample with D2O (red), and after irradiating the dosed sample several times and rewarming to room temperature (black). The ratios of SiOD+/SiOH+ and SiD+/Si+ are seen to significantly increase after D2O exposure and irradiation, thus indicating that the deposited D2O undergoes a dissociative bonding reaction with the surface.
Paper: Solar Wind Sputtering of Secondary Ions from Water-ice-covered Regolith Analogs
Authors: Micah J. Schaible, Gabriella K. Dotson, Roshan Trivedi, Advik D. Vira, Kevin P. Hand
Figure caption: The XPS survey scans for pyrite after polishing and subsequently sputter-cleaning the sample surface show that carbon contamination and surficial oxygen are readily removed by low-fluence Ar+ bombardment.
Paper: Prediction of Sulfate Hazes in the Lower Venus Atmosphere
Authors: Peter Woitke, Manuel Scherf, Christiane Helling, Paul Rimmer, Martin Ferus, Helmut Lammer, Fabian Weichbold, Kateřina Němečková, Petr Eminger, Jaroslav Kačina, Tereza Constantinou
Figure caption: Left: equilibrium drift velocity v°dr (or final fall speed) of particles as a function of particle radius a and height z in the Venus atmosphere, where we have assumed a material density of ρ  m  = 1.83 g cm−3, the mass density of sulfuric acid H2SO4. Right: the growth timescale by condensation of sulfuric acid on a particle’s surface τ gr = V / (∂V/∂t) in the Venus atmosphere. Here we have assumed a large supersaturation S → ∞ and H2O to be the key molecule that limits the growth with a constant concentration of 30 ppm. The blue dashed line shows where the growth timescale equals the sinking timescale τ sink = H  p /v°dr. Liquid H2SO4 is expected to evaporate below 45–50 km (∼350 K); see D. V. Titov et al. (2018).
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Overview of the analyzed data. We report the LRA observations included in this work (colored markers each represent a different LRA; see y-axis), together with the data arcs used for the LRO OD (gray shaded regions). The numbers indicate the number of observations for each LRA in that arc. Markers surrounded by black squares indicate that at least one of the observations was taken during an arc overlap. Overlap intervals are named with capital letters (top of the plot) for later analysis. See text (Section 3.3) for more details on arc overlaps.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Location of LRAs on the Moon as of 2025 August. The color of each LRA denotes its status, and the superscript denotes the LRA design. Astrobotic PM-1 was intended to land in the Sinus Viscositatis region but did not achieve lunar orbit and reentered Earth’s atmosphere. The landing sites for Blue Moon Pathfinder (MK-1), Firefly BG-4, and Artemis III are not available as of 2025 August. See D. Cremons (2025) for updates.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Orbit overlap analysis when the Apollo LRAs are used as fixed control points. We report the rms difference in the radial, transverse, and normal components of the position vector of LRO, during the overlap periods (typical duration 8–10 hr) of Figure 4. The error bars show the rms uncertainty (its maximum between the two overlapping orbits). We report the overlap difference for the full solution (LRA) and when the LRA observations are not used (No LRA). It can be seen that the inclusion of LRA measurement reduces the orbit error in the T (transverse) and N (normal) components for the E overlap.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Ground pattern of successive LOLA shots from different ranges to the surface. When distance increases, the fractional coverage of the sampled swath (gray) improves as the ground speed remains nearly fixed. Near-complete sampling of the swath by the receiver FOVs (colored circles) is achieved at ∼150 km range.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Trajectory differences in the radial (R), transverse (T), and normal (N) directions at the time of each laser shot due to the inclusion of the LRA observations in the analysis, when the Apollo LRAs are used as fixed control points. The error bars report the trajectory formal uncertainty, propagated at the laser shot time, which is an output of the OD filter.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Orbit overlap analysis when the LRO orbit and LRA coordinates are solved simultaneously. We report the rms difference in the radial, transverse, and normal components of the position vector of LRO during the overlap periods of Figure 4. The error bars show the rms uncertainty (the maximum between the two overlapping orbits). We report the overlap difference for the full solution (LRA) and when the LRA observations are not used (No LRA). It can be seen that the inclusion of LRA measurements reduces orbit errors in the T and N components.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Left: photograph of a mini-LRA unit and the elevation angle definition used throughout. Right: azimuthally averaged OCS of the mini-LRA as a function of elevation angle. The mean value is shown in dark blue, and the standard deviation from the radial average is shown in light blue.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Post-fit residuals showing a good convergence of the OD process. Each marker indicates a different LRA. The top panel shows the range residuals; the bottom panel shows the angle residuals. We also report in the white boxes the mean (M) and rms of the residuals.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Downweighted Doppler case. Trajectory differences at the time of each laser shot due to the inclusion of the LRA observations in the analysis, when solving simultaneously for the LRO orbit and the LRA coordinates. The error bars report the formal trajectory uncertainty, output of the OD filter.
Paper: First Use of Laser Ranging to Surface Retroreflectors for Orbit Determination: LRO-LOLA at the Moon
Authors: G. Cascioli, E. Mazarico, D. R. Cremons, M. K. Barker, D. Mao, S. Goossens, V. Viswanathan, S. Bertone, K. Jha, F. G. Lemoine, X. Sun, J. W. Head, D. E. Smith, M. T. Zuber
Figure caption: Comparison of signal strength (received photons per pulse from the surface normalized to the value at 10 km) between the surface reflectance and the LRA reflectance for the same LiDAR operating at 1064 nm in lunar orbit. The dotted black lines show that the signal strength at 10 km from the surface is nearly identical to the signal strength from the LRA at 120 km distance.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: Silicate and carbon phase endmember spectra. VNIR spectra are plotted in reflectance while MIR spectra are plotted in 1-Reflectance and are offset for clarity. (A) VNIR spectra of silicate endmembers. Note the lack of 1 μm feature in the enstatite and forsterite spectra. (B) VNIR spectra of opaque endmembers. Note the differences in spectral slope. (C) MIR spectra of silicate endmembers. Christiansen feature (CF) positions for each endmember are shown via vertical dashed lines of the respective spectrum’s color. (D) MIR spectra of opaque endmembers.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: View of the restrictor funnel assembly atop the sample holder through the chamber’s load/lock door, view of the sample holder through a chamber window, and the raster pattern of the laser for the sample holder well displayed on carbon paper.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: VNIR spectrum of analog sample SCO. The black line denotes the original spectrum. The vertical gray lines and points denote the region of interest for fitting the continuum, 0.68–1.70 μm. The orange dotted line is the calculated continuum. The spectrum after continuum removal is shown with the green dotted–dashed line, and the reflectance minimum at the band center is denoted by the green star. The red dotted line shows the point from which the band depth was calculated, i.e., reflectance = 1.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: Experimental setup. (A)–(B) Beam path for the long- and short-pulse lasers into the ultra-high vacuum chamber. (C) View of the steering mirror, focusing lens, beam entrance window, actuators for steering, and piezo inertia motor controllers.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: VNIR spectra of the SCO series of mixtures before and after simulated weathering. Spectra of mixtures before weathering are denoted by a solid line and spectra of mixtures after weathering are denoted by a dashed line. Note the difference in reflectance values on the y-axis between plots. Figure 5(a)) Base SCO before and after simulated weathering. Figure 5(b)) SCO + opaque mixtures before and after simulated weathering.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: VNIR spectra of the ENST series of mixtures before and after simulated weathering. Spectra of mixtures before weathering are denoted by a solid line and spectra of mixtures after weathering are denoted by a dashed line. Note the difference in reflectance values on the y-axis between plots. (a) Base ENST before and after simulated weathering. (b) ENST + opaque mixtures before and after simulated weathering. (c) ENST + AC mixture before weathering, after short-pulsed laser weathering alone (purple dashed line), and after both short- and long-pulsed laser weathering (yellow dashed line).
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: MIR spectra of the ENST endmember and mixtures in 1-Reflectance space. Spectra are offset for clarity. The nonweathered spectra are shown with solid lines, and weathered spectra are denoted by the dashed lines. Feature positions for pure, nonweathered ENST are shown with the vertical, dotted lines (red = CF, gray = RB, blue = TF). Black arrows denote features that shifted significantly from the reference (base, nonweathered silicate) position.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: MIR spectra of the SCO endmembers and mixtures in 1-Reflectance space. Spectra are offset for clarity. The nonweathered spectra are shown with solid lines, and weathered spectra are denoted by the dashed lines. Feature positions for pure, nonweathered SCO are shown with the vertical, dotted lines (red = CF, gray = RB, blue = TF). Black arrows denote features that shifted significantly from the reference (base, nonweathered silicate) position.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: Image panels of silicate endmembers before and after irradiation. From left to right: (1) San Carlos olivine (natural), (2) forsterite (synthetic), and (3) enstatite (synthetic). Each image was taken at 5000x magnification. For the base silicates (prior to irradiation), note the difference between the individual particles of SCO (sharp boundaries, little obvious surface texture, fine particulates, wide range of sizes) and the FORS and ENST synthetic particles (globular, rounded edges, fewer fine particulates).
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: IMIR spectra of the ENST series in 1-Reflectance space. Spectra are offset for clarity. The nonweathered spectra are shown with solid lines, and weathered spectra are denoted by the dashed lines. The position of the 5.2 μm band (EB2, Band 2 in C. H. Kremer et al. 2023) for pure, nonweathered ENST is shown with the vertical, gray dotted line.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: IMIR spectra of the SCO series in 1-Reflectance space. Spectra are offset for clarity. The nonweathered spectra are shown with solid lines, and weathered spectra are denoted by the dashed lines. The positions of OC 1 (5.6 μm) and OC 2 (6 μm) for pure, nonweathered SCO are shown with the vertical, gray dotted lines.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: VNIR spectra of the FORS endmember and series of mixtures before and after simulated weathering. Spectra of mixtures before weathering are denoted by a solid line and spectra of mixtures after weathering are denoted by a dashed line. Note the difference in reflectance values on the y-axis between plots. (a) Base FORS before and after simulated weathering. (b) FORS + opaque mixtures before and after simulated weathering.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: MIR spectra of the FORS endmember and mixtures in 1-Reflectance space. Spectra are offset for clarity. The nonweathered spectra are shown with solid lines, and weathered spectra are denoted by the dashed lines. Feature positions for pure, nonweathered FORS are shown with the vertical, dotted lines (red = CF, gray = RB, blue = TF). Black arrows denote features that shifted significantly from the reference (base, nonweathered silicate) position.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: IMIR spectra of the FORS series in 1-Reflectance space. Spectra are offset for clarity. The nonweathered spectra are shown with solid lines, and weathered spectra are denoted by the dashed lines. The positions of OC 1 (5.6 μm) and OC 2 (6 μm) for pure, nonweathered FORS are shown with the vertical, gray dotted lines.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: Sample contamination from fluorine. (A) TEM image and (B) EDS map of weathered ENST+CB sample taken in bright-field STEM mode. To enhance image contrast of the fluorine map, we applied a linear normalization to the data to set values below the 2nd percentile to 0 and values above the 98th percentile to the maximum number of EDS counts. Image Credits: Brittany A. Cymes and Roy Christoffersen, Johnson Space Center. (C) SEM image and (D) EDS map of weathered SCO sample indicating the presence of fluorine.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: Images showing graphite deposition within the chamber after lofting, as discussed in Section 5.2.2. (Left) View through window directly above the sample (laser entry window). Graphite is seen covering the top of the clamp. (Right) View through window situated at 45° with respect to the sample holder. Graphite is seen covering the clamp, the clamp arm, and part of the stainless steel neck below the window.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: Illustration of slope calculation and normalization for VNIR spectra using an example SCO spectrum. The leftmost plot illustrates the lines that were fit to the 0.4–0.55 μm (green, dotted line) and 1.7–2.5 μm (orange, dotted line) regions of the spectrum (black, solid line) to determine spectral slope. The rightmost plot shows the spectrum before (blue, solid line) and after normalization (orange, dotted line) to 1.7 μm.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: (Left) Full view dark-field (DF) image of the irradiated ENST+CB FIB section and (right) DF image of a smaller region on the sample wall. Note the “Swiss-cheese” texture of the cross-section, as well as the enstatite crystal twinning, examples of which are circled in yellow with the direction of the twinning lines marked with red arrows. Image credits: R. Christoffersen and B.A. Cymes, Amentum, NASA Johnson Space Center. FIB section prepared by Z. Rahman, Amentum, NASA Johnson Space Center.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: RELAB images of (left) graphite, SCO+GR, FORS+GR, and ENST+GR, as well as (right) irradiated FORS+CB, ENST+CB, SCO+GR, FORS+GR, and ENST+GR. Photo credits: Dr. Takahiro Hiroi, Brown University.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: RELAB images of silicate endmembers before and after irradiation. Photo credits: Dr. Takahiro Hiroi, Brown University. Photo credits: Dr. Takahiro Hiroi, Brown University.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: RELAB images of (left) FORS+AC, FORS+CB, ENST+AC, and ENST+CB, as well as (right) anthracitic coal, and irradiated FORS+AC, ENST+AC, and ENST+ACSP. Photo credits: Dr. Takahiro Hiroi, Brown University.
Paper: Space Weathering on Carbon-rich Surfaces: Spectral Characterization of Fe-poor Mercury and Carbonaceous Asteroid Analogs
Authors: A. N. Shackelford, K. L. Donaldson Hanna, J. J. Gillis-Davis
Figure caption: RELAB images of (left) carbon black and (right) SCO+CB and SCO+AC mixtures before and after weathering. Photo credits: Dr. Takahiro Hiroi, Brown University.
Paper: Surface Properties of Sediments at the 2014–2015 Holuhraun Lava Flow-field: Insights from Multiwavelength Radar
Authors: Reid P. Perkins, Shannon M. Hibbard, Catherine D. Neish, Christopher W. Hamilton, Bruce A. Campbell
Figure caption: Overview of the 2014–2015 Holuhraun lava flow-field, showing an inset map of Iceland, with the location of the study area represented in the inset as an orange rectangle. The specific location of this study along the northern margin of the flow-field is represented as a rectangle in the main map.
Paper: Surface Properties of Sediments at the 2014–2015 Holuhraun Lava Flow-field: Insights from Multiwavelength Radar
Authors: Reid P. Perkins, Shannon M. Hibbard, Catherine D. Neish, Christopher W. Hamilton, Bruce A. Campbell
Figure caption: 200 MHz GPR Transect 4 (Site 2). (a) The yellow shaded area represents surface sediment layer. (b) Field view looking downhill along the GPR transect, near the end of the profile. Here “m” refers to the vertical and horizontal scale in meters.
Paper: Surface Properties of Sediments at the 2014–2015 Holuhraun Lava Flow-field: Insights from Multiwavelength Radar
Authors: Reid P. Perkins, Shannon M. Hibbard, Catherine D. Neish, Christopher W. Hamilton, Bruce A. Campbell
Figure caption: 200 MHz GPR Transect 1 (Site 1). (a) The yellow shaded area represents sediment layer. (b) Field view looking uphill along the GPR transect, near the start of the profile. Here “m” refers to the vertical and horizontal scale in meters.