adsabs/AstroCLIMB huggingface dataset:
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Results of OTES spot offset analysis. The rms error was calculated between ATPM 9.24 μm brightness temperatures (assuming a constant mean thermal inertia value) and OTES 9.24 μm brightness temperatures for the Checkpoint (A), Matchpoint (B), and TAG (C–F) data sets. The location of lowest rms error is shown with the black asterisk in each frame. Figures C and D compare results using the OLA v20 and v21 DTMs, with the best solution offset in different locations as expected due to the known offset between the DTMs.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Thermal inertia results from this work (Matchpoint, Checkpoint, and TAG data) overlaid on thermal inertia values from Recon A and Recon B observations (Rozitis et al. 2022).
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: NE–SW striking wrinkle ridge from the NT2022 database located in Mare Serenitatis (4.009°W 45.997°N) shown in Diviner RA data (A; Powell et al. 2023), δCPR (B; Fassett et al. 2024), and LROC NAC data (C; LROC NAC M1304401329RE). Boulder fields on this ridge exhibit visibly high albedo in LROC NAC data (C) with corresponding elevated δCPR and RA pixel values. A direct comparison of RA and δCPR median values for 419 wrinkle ridges with δCPR coverage (i.e., Figure A2) demonstrates that agreement between individual ridge RA and δCPR medians, such as this one, is uncommon.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: A recently active wrinkle ridge from the NT2022 wrinkle ridge database in Mare Cognitum (19.89°W 12.46°S) shown in LROC NAC image data (A; NAC M1175531291) and overlain by LRO Diviner RA data (B; Powell et al. 2023). This wrinkle ridge segment ranges from ∼30 to 100 m in width and exhibits multiple high-albedo boulder fields along strike (C; red inset). Diviner RA pixels remain elevated along the ridge as a result of the exposed boulder fields.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: An example of a topographically muted lunar wrinkle ridge with increased boulder populations (11.12°S, 37.04°W). Unlike those ridges documented in NT2022, this ridge does not exhibit a crisp boundary between the wrinkle ridge scarps and the surrounding terrain or any crosscutting relationships with small surrounding craters. Hence, this ridge was not included in the NT2022 recently active wrinkle ridge database, but the presence of boulder fields on the ridge scarps and crest may indicate potential recent tectonic activity (NAC M147225042RC, M147225042LC).
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: Quantitative relationship between δCPR and RA median values for 419 recently active wrinkle ridges across the lunar nearside maria. The lack of a correlation between these two data metrics is likely due to some combination of the nonphysical data artifacts associated with the Mini-RF monostatic data set, the low signal-to-noise ratio of the Mini-RF data set, and the sensitivity of S-band radar data to subsurface rock fragments.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: E–W striking wrinkle ridge cluster from the NT2022 database located in NE Mare Imbrium (4.009°W 45.997°N) shown in LROC NAC data (A; LROC NAC M1274280167RE) and Diviner RA data (B; Powell et al. 2023). Similar to other wrinkle ridges in Mare Imbrium, these structures do not exhibit visible boulder populations on their scarps or crests in LROC NAC data (C; red inset) even though they appear to be recently active based on the presence of meter-scale graben (D; yellow inset). Similarly, the Diviner RA pixels associated with each ridge are not elevated relative to the background terrain.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: Recently active wrinkle ridge from the NT2022 database (38.23°W 18.72°N) that appears to have been reactivated as recently as ∼90 Ma based on crosscutting relationships with a ∼15 impact crater (purple inset; Fassett et al. 2022). The presence of additional crosscut impact craters (green inset) and small-scale extensional features (blue inset) support the interpretation that this and other morphologically similar ridges in NT2022 are recently formed or reactivated.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: A comparison of wrinkle ridge median RA (A), 95th percentile RA (B), and median δCPR values (C) collected over a sample set of recently active wrinkle ridges in SE Mare Humorum (n = 51 ridges in RA, n = 24 ridges in δCPR). The agreement between the results of these two sampling strategies indicates that a standardized buffer is a suitable approximation for true wrinkle ridge widths. A visual representation of these two data collection methods is presented in supplemental information (Figure A3).
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: (A) NT2022 recently active wrinkle ridges colorized by median δCPR value overlaid onto the LROC WAC global mosaic (∼100 m pixel−1). Due to the limited coverage of the Mini-RF data set, only 419 of the 1116 total wrinkle ridges from the NT2022 database are measured in δCPR data. (B) The overall distribution of wrinkle ridge δCPR median values for every sampled ridge in the NT2022 database.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption:                    NT2022 recently active wrinkle ridges colorized by rock abundance (RA) 95th percentile value overlaid onto the LROC WAC global mosaic (∼100 m pixel−1). (B) The overall distribution of wrinkle ridge RA 95th percentile values for every ridge in the NT2022 database.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Left: outlines of the extent of OTES observations collected during the Checkpoint (yellow), Matchpoint (blue), and TAG (white) observations, overlaid on a Recon A PolyCam mosaic. Gaps along the tracks are due to omitted data that had instrumental phase-inversion issues (Christensen et al. 2019). The dashed white circle marks the approximate rim of Hokioi Crater. The TAGSAM contact point is located approximately where the TAG and Matchpoint observations intersect and form a cross near the top of the image. Northing is given relative to the equator. Easting is given relative to the approximate center of Hokioi Crater. The specific northing/easting center was inconsequential to the analysis. Right: comparison between OTES 9.24 μm brightness temperatures and model-predicted brightness temperatures (using a mean global thermal inertia value and OLA v20 DTM) before and after the ATPM-based pointing adjustment.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Thermal inertia results from the ATPM using the OTES data from Checkpoint rehearsal, Matchpoint rehearsal, and TAG. The dashed white circle marks the approximate rim of Hokioi Crater. Boxes indicate the locations of Figures 3 and 4.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: Mapped wrinkle ridge boundaries overlain onto the 600 m standardized ridge buffers for the subset of recently active ridges in Mare Humorum used to derive the quantitative relationships in Figure 7. Most of the ridges sampled here are contained within the standard buffers, but several exceed their boundaries. For those wider ridges, the buffers were drawn to include the vergent side of the ridge, where the majority of the boulder fields should be located if present.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: PSRs in the north polar region of Ceres based on the global SPG shape model. The color indicates the maximum obliquity at which a location is in shadow through an entire orbit. The grayscale map is the terrain slope. Polar stereographic projection with R = 470 km.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: Variations of the area in permanent shadow as a function of Ceres obliquity and latitude. (a) PSR area for various ranges of latitude versus obliquity. (b) Distribution of PSR area vs. latitude for several obliquity values. The PSR area at 20° obliquity is essentially zero.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: FC images for seven craters. The superimposed color contours represent the extent of PSRs for different values of the axis tilt. The red contour is included to demonstrate that no PSRs exist at 20° axis tilt.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: Zatik crater (NP5, #2) with the FC image stretched so the sunlit ice west of the shadow is visible, whereas the majority of the BCFDs lies in the dark shadow (Figure 3). The topographic contours have intervals of 200 m and are relative to a sphere. Sublimation rates are averaged over one orbit and the spin rotation. The thick gray contour represents the PSR.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: Time-averaged potential sublimation rate for water ice in Bilwis crater (NP4, #1) for various axis tilts and based on equilibrium temperatures. The average is over the spin and orbital rotations. Contours for the sublimation rate are shown in units of mm of ice per Earth year. Thick gray contours represent the PSR. The BCFD best aligns with the PSR at an axis tilt of 10°.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: Contours of maximum equilibrium temperature at 4° axis tilt superimposed on FC images. Gray contours represent the PSRs at the same axis tilt. (Temperatures outside the crates may be unreliable because of the limited extent of the domain).
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: Surface temperatures and potential sublimation rates obtained by solving the one-dimensional heat equation for a latitude of 86° N, an obliquity of 18°, and a Bond albedo of 0.07. The means are time averages over one Ceres orbit.
Paper: History of Ceres’s Cold Traps Based on Refined Shape Models
Authors: Norbert Schorghofer, Robert Gaskell, Erwan Mazarico, John Weirich
Figure caption: The axis tilt (obliquity) of Ceres over the last 25 ka according to Ermakov et al. (2017).
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: Illustration of the possible pathways the TRAPPIST-1 planets can take through escape physics in our model. Interior planets are denoted by dashed curves, and HZ planets are denoted by solid curves. Escape shutoff times are shown by vertical dotted lines, and times of switches from energy-limited to diffusion-limited escape are shown by vertical dotted–dashed lines. Left column: escape is halted by complete planetary desiccation, for an interior planet, T1-c (black), and for an HZ planet, T1-f (orange), both with 1 TO initial water inventory. In these cases the atmospheric water is removed entirely, and the planet is last in diffusion-limited escape before the simulation halts. Middle column: simulations of HZ or outer planets where escape is halted by entrance to the HZ and the subsequent formation of a cold trap, all for initial water inventories of 10 TO. In this case escape could end in either the diffusion-limited (for T1-e; pink) or energy-limited (for T1-g; teal) regime. Right column: escape never shuts off, as the planetary water reservoir is sufficiently large to sustain ongoing escape through the system's lifetime. This end state can only occur for interior planets (and results for T1-b and T1-d with an initial water inventory of 200 TO are shown here), as planets in or beyond the HZ have escape shutoff by the formation of a cold trap. Once again, escape could end in either the diffusion-limited (for T1-b; red) or energy-limited (for T1-d; blue) regime, depending on total received insolation and initial water inventory. Top row: shows water lost (in TO) over time for each of the column cases previously described. Bottom row: shows oxygen produced (in bars) over time for each of the column cases previously described.
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: A comparison of the water-loss and oxygen production rates from Krissansen-Totton & Fortney (2022) to this study. Design of the figure is meant to re-create the style published in Krissansen-Totton & Fortney (2022); all shaded regions denote 2σ uncertainties. The red, purple, and blue lines and shaded regions show the results from this study for initial water contents of 1, 15, and 100 TO, respectively, and the gray line and shaded region show the results presented in Krissansen-Totton & Fortney (2022). Left column: comparisons for the interior planet T1-b (see Figure 2 in Krissansen-Totton & Fortney 2022). Right column: comparisons for the HZ planet T1-e (see Figure 3 in Krissansen-Totton & Fortney 2022). Top row: rate of water loss due to thermal atmospheric escape (Tmol yr−1) over time in years. Note that, as water is being lost, the flux is negative. Bottom row: rates of oxygen production (i.e., gain flux; Tmol yr−1) due to water photolysis and subsequent hydrogen escape over time in years. In general, our results are in agreement with those of Krissansen-Totton & Fortney (2022), and our median test case with an initial water inventory of 15 TO (log space average between 0.7 and 300 TO) stays within their model uncertainties for the entire age of the system. Note that, in the T1-e comparisons, our 15 and 100 TO cases display nearly identical evolution and overlap on the plot.
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: Oxygen retention efficiency as a function of initial water content in TO. Top row: interior planets, T1-b, c, and d. Bottom row: outer planets, T1-e, f, g, and h. Coloring shows the percentage of simulations at a particular initial water content that fell in a given oxygen retention efficiency bin (e.g., each column corresponds to one initial water content and sums to 100%). Contours are given for the 50th percentile values (solid white lines) and the 1σ confidence region (dashed white lines).
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: The predicted final water loss and final oxygen produced and retained as a function of initial water content for the TRAPPIST-1 interior planets T1-b (red), c (black), and d (blue). Top row: water lost (in TO) vs. initial water (in TO); the shaded blue-gray region indicates where desiccation occurs. For water contents in the top left panel, all three planets are desiccated, and thus their curves are overlapping. Bottom row: oxygen produced and retained (in bars) vs. initial water. Left column: low initial water contents (1–20 TO). Right column: high initial water contents (30–500 TO). Shaded regions give the 1σ uncertainty ranges (set by the 16th and 84th percentile values of the final-state distributions).
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: The predicted final water loss and final oxygen produced and retained as a function of initial water content for the TRAPPIST-1 HZ and outer planets T1-e (pink), f (orange), g (teal), and h (purple). The layout of the figure is the same as Figure 2.
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: Left: the oxygen left in the atmospheres of T1-b (red) and T1-c (blue) after an estimated removal of 3 TO worth of oxygen from a magma ocean, 100 bars from nonthermal escape, and 10 Tmol yr−1 (∼55 bars Gyr−1) from dry crustal oxidation after the planet becomes desiccated (see text for estimation explanation). Right: the resulting histogram of initial water contents predicted by MCMC when fitting for the scenario that T1-b has lost all oxygen while T1-c retains 0.1 bar of atmospheric oxygen following the estimated removal. The vertical solid black lines on both panels denote the 50th percentile value predicted by the MCMC, while the vertical dashed black lines denote the 68% (1σ) confidence interval. This analysis predicts a minimum initial water content of ﹩{8.2}_{-1.0}^{+1.5}﹩ TO to produce the desired final state, assuming that both planets begin with the same initial water content. The amount of oxygen removal is meant to be an underestimate to produce a conservative lower limit, as additional oxygen removal would increase the minimum initial water required.
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: An illustration of the method used to determine the most probable initial water content for T1-e that would reproduce our predicted present-day content from Agol et al. (2021; Table 3). Same layout as Figure 4, but with linear x-axis scaling; the y-axis is the likelihood that each initial water content (in TO; x-axis) produces the desired final state. The data points that were simulated are shown by the pink points, the bins used in the Riemann sum are shown in gray, the determined 50th percentile or true predicted value is shown by the vertical dashed black line, and the 1σ and 2σ confidence intervals are shown by the shaded dark- and light-blue regions, respectively. The low initial water contents (1–20 TO) are much more finely spaced (step size of 1 TO), which is why the Riemann sum bin widths are not resolvable there. Lines connecting data points are used for the tops of the Riemann sum bins.
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: The likelihood of each initial water content (in TO) needed to reproduce the predicted present-day water contents from Agol et al. (2021) for each of the outer planets. The peaks denote the initial water content on our sampling grid most likely to produce the final content in our predictions. An additional nine simulation suites were ran for T1-e only, between 100 and 200 TO to fill out a smooth, continuous curve, and results from these additional simulations are denoted by triangles.
Paper: The Implications of Thermal Hydrodynamic Atmospheric Escape on the TRAPPIST-1 Planets
Authors: Megan T. Gialluca, Rory Barnes, Victoria S. Meadows, Rodolfo Garcia, Jessica Birky, Eric Agol
Figure caption: All 20,900 stellar mass samples available for simulations to draw from Birky et al. (2021). The y-axis shows the stellar mass in M ⊙ of a given sample, which is arbitrarily assigned an ID on the x-axis. The red solid line denotes the mean stellar mass across all samples, while the dark-blue and subsequent lighter-blue regions denote 1, 2, 3, and 4 standard deviations from the mean, as labeled in the plot. The light-gray shaded region denotes samples greater than 4 standard deviations from the mean, indicating that samples in this region are classified as outliers, such that simulations using stellar masses above 4 standard deviations are removed from the final data set.