adsabs/AstroCLIMB huggingface dataset:
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Total integration time required to cover a given percentile of the sky distribution of pre-Patroclus L5 encounterable Jupiter Trojans down to a specified size (assuming p = 0.05) and as a function of epoch within the search window. The first panel presents results for DECam covering the 10th percentile region, while the second panel shows the same for Subaru/HST. The third and fourth panels correspond to the LSST camera, considering both the 10th and 80th percentile regions. The color map is truncated between 1 km and 500 m. Vertical dotted lines indicate the epoch of maximum topocentric search area and the time of opposition.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: (Top) Ecliptic barycentric coordinates of synthetic L5 Trojans accessible to Lucy during a pre-Patroclus encounter. These Trojans cluster on the sky ∼6 yr prior to the encounter window. (Bottom) Time evolution of the search area for pre-Patroclus encounterable L5 Jupiter Trojans. The sinusoidal lines represent the observable areas from Cerro Pachón, while the smooth transparent lines are the areas calculated in the barycentric frame. From bottom to top, the solid lines indicate, respectively, the 10th, 50th, and 80th percentile areas. The vertical green shaded band indicates the ∼150 day search window. The bottom right plot provides a zoom-in view centered on the 2026–2027 clustering window, which is marked in the bottom left plot with a box. The right-hand axis of the zoomed-in plot indicates the mean solar elongation of the synthetic Trojans. The mean solar elongation is shown as a gray dashed line, and the full range between minimum and maximum elongation is shaded in gray.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Expected number of L5 Jupiter Trojans within the volume accessible to Lucy during the pre-Patroclus (top) and post-Patroclus (bottom) encounter windows. White contours indicate values of NE = 0.001, 0.01, 0.1, 1, and 10. Vertical black dotted lines show equivalent absolute magnitudes Hr for different object diameters, assuming a 5% albedo. While the likelihood of a new flyby target along the nominal trajectory is very low, moderate Δv maneuvers can enable additional subkilometer flybys, particularly during the pre-Patroclus window.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: (Top) Heliocentric distance of Lucy over time. Red vertical lines indicate the third EGA3 and the Patroclus–Menoetius flyby (P+M). Gray shaded regions mark the pre- and post-Patroclus encounter windows explored in this study. (Bottom) Lucy’s position relative to the L5 cloud distributions (fr, fλ, and fβ) after EGA3. The white dashed lines show the relative position of μr(t), μλ, and μβ, while the shaded blue regions indicate the 1σ, 2σ, and 3σ boundaries. The encounter windows are defined by Lucy’s entry and exit relative to the spatial extent of the L5 cloud, as well as by operational constraints associated with the Patroclus encounter.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Expected number of encounterable L5 Jupiter Trojans under different assumptions for the faint-end break magnitude Hr,B2 and the corresponding power-law slope α3. The values are normalized to a reference case assuming D = 700 m (p = 5%) and Δv = 50 m s−1, which yields NE ∼ 1 during a pre-Patroclus scenario. Hashed vertical and horizontal bars indicate uncertainty ranges from our nominal values, i.e., from K. Uehata et al. (2022) and F. Yoshida & T. Terai (2017), respectively. The horizontal gray line and shaded band represent the break magnitude reported by I. Wong & M. E. Brown (2015).
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Orbital distribution model of the L5 Jupiter Trojans. The three panels show the distributions of semimajor axis (a), eccentricity (e), and inclination (i). Histograms correspond to background Trojans from the MPC catalog that are brighter than the completeness limit, evaluated at four different epochs. The blue curves represent fitted models, with best-fit parameters μa = 5.2 au, σa = 0.05 au, σe = 0.06, and σi = 12﹩\mathop{.}\limits^{\unicode{x000b0}}﹩78.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Time evolution of the spatial separation between Lucy’s nominal trajectory and trajectories modified with a given Δv budget during the pre- (top) and post-Patroclus (bottom) encounter windows. The shaded gray regions mark the defined encounter windows. Left and right columns correspond to Δv = 50 m s−1 and Δv = 25 m s−1, respectively. Each colored curve represents a different azimuthal direction θ, grouped into 90° bins and vertically offset for clarity. Dashed curves show the linear approximation.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Projected sky distribution of encounterable pre-Patroclus L5 Jupiter Trojans in ecliptic coordinates as observed from Cerro Pachón at the middle point of the search window. The white solid lines indicate the 10th, 50th, and 80th percentile regions, and the red dots represent one-tenth of the synthetic Jupiter Trojans used to calculate them. The green solid lines are the ecliptic and equatorial planes.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Schematic diagram of the local cylindrical coordinate system along a spacecraft’s trajectory. The vectors ﹩\hat{{\boldsymbol{u}}}(t)﹩ and ﹩\hat{{\boldsymbol{w}}}(t)﹩ define the plane orthogonal to the velocity vector v(t) when ϕ = 90∘.
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: (A) SSI spectra for pyrite, normalized to the Fe+ intensity and taken at room temperature before cooling (red and black) and after rewarming to room temperature (green). (B) Pyrite SIMS spectra taken immediately after D2O deposition and collected at separate sample positions showing that Fe can be ejected through the ice layer, possibly due to energetic interface interactions. (C) The same two sample spots after irradiation to a fluence of ∼1.5 × 1016 H﹩{}_{2}^{+}﹩ cm–2 showing the presence of all substrate ions mixed with water-cluster ions. (D) Secondary ion spectra vs. fluence where again the maxima in the water-group ion intensities coincides with the appearance of substrate species.
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: (A) SSI intensity vs. irradiation fluence for iron oxide after dosing with ∼20 monolayers of D2O and sputtering at a flux of ∼1 × 1012 H﹩{}_{2}^{+}﹩ cm−2 s−1. The relative abundances of the water-group species remain fairly constant, suggesting that substrate interactions are not as prevalent in the iron oxide sample. (B) Derivative of the secondary ion intensity for a ∼20 monolayer D2O deposition. The maxima of the water-group ions correspond with the appearance of substrate ions, thus indicating the importance of the water/mineral interface.
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: assumed temperature/pressure structure of the Venus atmosphere. Middle: the concentrations of condensed units n cond/n that deposit and are removed from the model when advancing to the next atmospheric height. Right: element abundances with respect to oxygen ϵ  k /ϵ O remaining in the gas phase.
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: Chemically active particles in the lower Venus atmosphere with coagulation and reduced passive material component, assuming only n  p  = 0.5 cm−3 at the lower boundary. The grain charge parameter is set to qa300 = 5.
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: Passive particles in the lower Venus atmosphere without coagulation, for grain charge parameter qa300 = 4. The dashed lines represent the analytical solutions that we obtained from Equation (14). The blue circles and additional black lines show selected measurements as discussed in the text. The data from R. G. Knollenberg & D. M. Hunten (1980) only include the expected opacity of the detected particles with a diameter ≳0.6 μm (a ≳ 0.3 μm). Parameter κ ext is the extinction coefficient of the particles at λ = 600 nm.
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: Timescale analysis of our four models as indicated. The top model is for passive particles without coagulation; see Figure 4. From the models for passive particles with coagulation (Figure 5), the model with q/a = 50 is selected here. The two lower models for active particles correspond to Figures 6 and 7, respectively. The graphs show the inverse characteristic timescales [1 yr−1] of each cloud particle moment L  j  (j = 0, 1, 2, 3) for the four basic physical processes included: diffusion (blue), coagulation (red), settling (orange), and net growth (green). At every height, the sum of these inverse timescales must be zero in steady state. In the two lower models for chemically active particles, we have added horizontal lines at 1.9, 8.9, and 13.5 km to mark the cloud bases of pyrite, Na-sulfate, and K-sulfate, respectively.
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: Chemically active particles in the lower Venus atmosphere with coagulation, for grain charge parameter qa300 = 50.
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: The density of passive particles n  p (z) in the Venus atmosphere with respect to their density over the surface n  p (0) as a function of particle radius a. The eddy diffusion coefficient D(z) is assumed to be given by Equation (10), and the material density is selected to be ρ  m  = 1.83 g cm−3 for this plot. The latter value corresponds to liquid H2SO4, relevant for the uppermost regions in the plot. Solid particles are expected to be porous, which causes the effective mass density to be substantially smaller than in a pure (e.g., basaltic) material with ρ  m  ≈ 2.9 g cm−3.
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: Numerical method to simulate the various physical and chemical processes one by one. The notation 1/2 means to apply half a time step. The nested sequence of the operators assures second-order accuracy in time, as known from fluid dynamics simulations (e.g., P. Woodward & P. Colella 1984).
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: Same as Figure 4, but including coagulation for different values of the grain charge parameter qa300; see Equation (8).
Paper: A Novel Metric for Assessing Climatological Surface Habitability
Authors: Hannah L. Woodward, Andrew J. Rushby, Nathan J. Mayne
Figure caption: Annual mean climate across 2003–2018 derived from ERA5 for (a) surface air temperature Ts (kelvin), (b) precipitation P (mm yr﹩{}_{\oplus }^{-1}﹩), (c) evaporation E (mm yr﹩{}_{\oplus }^{-1}﹩), (d) net precipitation P − E (mm yr﹩{}_{\oplus }^{-1}﹩), (e) potential evapotranspiration PET (mm yr﹩{}_{\oplus }^{-1}﹩), (f) aridity index AI, and (g) sea ice concentration SIC.
Paper: The Surfaces of Small to Midsize Plutinos: Evidence of an Association between Inclination and Surface Type
Authors: Cameron Collyer, Rosemary E. Pike, Ying-Tung Chen, 英同 陳, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Bryan J. Holler, J. J. Kavelaars, Lowell Peltier
Figure caption: (a) Spectral slope space for the grz data set. In each panel, the solid black line indicates the reddening line, and the dashed black line indicates a constant value of PC2 = −0.13. Orange and blue-green outlines indicate FaintIR and BrightIR surface classifications, respectively. The purple outline indicates that the TNO is a previously confirmed Haumea family member from R. E. Pike et al. (2020). The circle outline indicates surface classification from Col-OSSOS grJ photometry (W. C. Fraser et al. 2023; R. E. Pike et al. 2023). Square outlines indicate surface classification, described in Section 5.2. Points without surface classification outlines have an ambiguous surface class. TNOs with FaintIR/BrightIR classifications in other dynamical classes are plotted with their surface classification only to avoid cluttering the figure. (b) The same as (a) but for the Col-OSSOS data set. (c) The same as (a) but for the H/WTSOSS data set. The triangle outline indicates the TNO is a previously confirmed Haumea family member from E. L. Schaller & M. E. Brown (2008) and C. Snodgrass et al. (2010). (d) Apparent percentage of TNOs in each dynamical class in each program with surfaces classified as FaintIR and BrightIR using same color scheme as (a), but TNOs with ambiguous surface classifications are now indicated in gray. Haumea family members are not included.
Paper: The Surfaces of Small to Midsize Plutinos: Evidence of an Association between Inclination and Surface Type
Authors: Cameron Collyer, Rosemary E. Pike, Ying-Tung Chen, 英同 陳, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Bryan J. Holler, J. J. Kavelaars, Lowell Peltier
Figure caption:  ﹩{{ \mathcal S }}_{g\to r}﹩ and ﹩{{ \mathcal S }}_{r\to z}﹩ spectral slopes shown in Figure 1 (left), broken down by dynamical class, as noted in the legend of each panel. In both panels, the TNOs observed in our Magellan Baade program are outlined with gray squares. Points connected by dashed red lines correspond to measurements of the same TNO at different epochs. Somnus is located above Mors in the left panel.
Paper: The Surfaces of Small to Midsize Plutinos: Evidence of an Association between Inclination and Surface Type
Authors: Cameron Collyer, Rosemary E. Pike, Ying-Tung Chen, 英同 陳, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Bryan J. Holler, J. J. Kavelaars, Lowell Peltier
Figure caption: CDFs in (g − z) for the cold classical, plutino, and nonresonant dynamically excited dynamical classes. The average uncertainty of (g − z) for each group is shown in the bottom right. Approximately 80% of the plutinos, and 80% of the nonresonant dynamically excited TNOs, have (g − z) ≲ 1.4 mag, while approximately 80% of the cold classicals have (g − z) ≳ 1.4 mag.
Paper: The Surfaces of Small to Midsize Plutinos: Evidence of an Association between Inclination and Surface Type
Authors: Cameron Collyer, Rosemary E. Pike, Ying-Tung Chen, 英同 陳, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Bryan J. Holler, J. J. Kavelaars, Lowell Peltier
Figure caption: Top/middle: CDFs in iosc and e for the plutinos in the grz, Col-OSSOS, and H/WTSOSS data sets. Bottom: sin(iosc) vs. e for the plutinos and cold classicals in the three data sets. The contours are iso-excitation lines, where ﹩\epsilon =\sqrt{{\,\rm{sin}\,}^{2}{i}_{osc}+{e}^{2}}﹩. Dynamical excitation increases radially from the lower-left corner. The colors of the points represent surface classification, consistent with the color scheme in Figure 4.
Paper: The Surfaces of Small to Midsize Plutinos: Evidence of an Association between Inclination and Surface Type
Authors: Cameron Collyer, Rosemary E. Pike, Ying-Tung Chen, 英同 陳, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Bryan J. Holler, J. J. Kavelaars, Lowell Peltier
Figure caption: Stellar magnitude and color data used to measure linear relations between IMACS and PS1 filters (left column) and IMACS and SDSS filters. The number of stars used to constrain the linear fits is noted in the bottom left of each panel in the left column (the same stars for a given filter type were used for IMACS→PS1 and IMACS→SDSS). See the text for further details.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Spatial distribution model of the L5 Jupiter Trojans in a coordinate system corotating with Jupiter. The first, second, and third panels represent, respectively, the longitude (λ), latitude (β), and radial distance (r) distributions. The histograms correspond to MPC background Trojans brighter than the completeness limit for four different epochs, and the blue lines are the fitted models. The radial distribution includes a vertical offset for visual clarity.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Hr distribution model of L5 Jupiter Trojans. The black line represents the cumulative histogram of MPC-listed L5 Jupiter Trojans of the background population. The blue line shows the model adopted in this work. The black vertical dotted line indicates the observational completeness limit.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Parameters defining the accessible volume during Lucy’s pre- and post-Patroclus encounter windows. Top: optimal polar angle ϕA as a function of azimuthal angle θA. Middle: optimal return time tB for the pre-Patroclus case, shown as a function of θA. Bottom: linear scaling between the initial maneuver magnitude ΔvA and the return impulse ΔvB for the pre-Patroclus trajectory. Black denotes the pre-Patroclus case, while green corresponds to the post-Patroclus scenario. Dashed lines indicate spline interpolations.
Paper: Prospects of a New L5 Trojan Flyby Target for the Lucy Mission
Authors: Luis E. Salazar Manzano, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, 省文 林, Fred C. Adams, Tessa Frincke, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Same as the top panel of Figure 5 but derived from the numerical Monte Carlo simulation of encounter outcomes. Black semitransparent dots represent the measured encounters from all 5000 trials. Hatched lines indicate the size range omitted from the simulation, as we are focused on the largest possible flyby targets and aimed to keep the simulation numerically tractable. Only the NE = 1, 0.1, and 0.01 contours are shown. The color map limits are identical to those in Figure 5.
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: (A) SSI intensity and (B) derivative of the ion intensity vs. fluence for SiO2 dosed with ∼50 monolayers of D2O and sputtered at a flux of ∼1 × 1012 H﹩{}_{2}^{+}﹩ cm−2 s−1. The derivative curves clearly show that the peak rates of change in both the metal ions and the water-group ions coincide, thus indicating an increase in the ejection of water-group ions near the D2O/SiO2 interface. The water-group ion curves have been multiplied by a factor of 50 for clarity. (C) The water-group ions and (D) the silicon-group ion intensities for SiO2 dosed with ∼20 monolayers of D2O and sputtered at a flux of ∼7 × 1012 H﹩{}_{2}^{+}﹩ cm−2 s−1. The behavior is similar to the thicker deposition, but the maxima in the water-group ions occur much sooner and are more pronounced, and the higher ion flux causes clear depletion in the species associated with D2O.
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: XRF maps of the iron oxide sample showing the spatial distributions for the major elemental species present in the sample. The bulk of the sample matches an approximately iron oxide (Fe2O3) composition. The Ca and Ti are highly spatially correlated and match a calcium titanate (CaTi2O4) composition. The Si, Al, and Mg species are also spatially correlated and likely represent matrix material between the iron oxide and calcium titanate grains.
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: (A) SSI spectra for iron oxide at room temperature before cooling (green), after dosing with ∼20 monolayers of D2O (black), and after sputtering the dosed sample to a fluence >3 × 1016 H﹩{}_{2}^{+}﹩ cm−2 (red). Water-group ions dominate the freshly dosed sample, while numerous atomic and molecular metal ions are seen in the room-temperature and sputtered samples. (B) The SIMS spectra, normalized to the Fe+ intensity, before dosing, after D2O deposition and irradiation, and after rewarming to room temperature show only very slight changes in the relative abundance of FeD+, thus indicating that the deposited D2O does not react strongly with the irradiated substrate.