adsabs/AstroCLIMB huggingface dataset:
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Crossover flybys over selected young geological terrains provide repeated coverage for SUDA to perform compositional mapping and monitor changes in between flybys. (a) E14 and E51 flybys provide the best coverage of Thera and partial coverage of Thrace; the later flyby would be in the extended mission. These two flybys are of top priority for the SUDA measurement plan. (b) Goirias Chaos will be studied during four flybys, providing an evenly timed coverage. (b) Rathcroghan Chaos will be studied during three flybys, with E6 providing the best coverage at 35 km altitude.
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Simulated plume dust impact rate as a function of altitude above Europa. With a plume gas ejection speed of 700 m s−1, plume grains are gravitationally bound and will fall back onto the surface in relatively close proximity to the source. For a reliable plume identification, an impact rate of ∼10  s−1 is preferable, which translates to an altitude of 100–150 km above the plume source location. From B. S. Southworth et al. (2015).
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: A screenshot of the graphical representation of the planetary system architecture at the top of the Alpha Centauri system overview page (Section 2.1.1). This is a triple-star system, with a confirmed planet (shown as a solid purple circle) orbiting Proxima Centauri, two candidate planets (shown as blue circles with white question marks) orbiting Proxima Centauri, and a false-positive planet (shown as a red circle with a white X) orbiting Alpha Centauri B.
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: An overview of the layout of the NEA Atmospheric Spectroscopy environment (Section 2.1.2). The table in the top left lists the available spectra in the NEA, the table in the top right lists the data from the selected spectrum in the top left table, and the plot in the bottom panel displays all the selected spectra in the top left table—in this case, Spitzer, Hubble, and JWST transmission spectroscopy of WASP-39 b.
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: The number of planets has been growing exponentially for decades. Here we show the decade leading up to 2025 and a projection of the expected yield of exoplanets for the following decade (see Section 5.1 for a discussion of the future landscape).
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: Examples of reconnaissance spectra (left) and high-resolution imaging of TOI-3569 (right) obtained by TFOP and shared with the community on ExoFOP (Section 2.2).
Paper: The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage
Authors: Jessie L. Christiansen, Douglas L. McElroy, Marcy Harbut, David R. Ciardi, Megan Crane, John Good, Kevin K. Hardegree-Ullman, Aurora Y. Kesseli, Michael B. Lund, Meca Lynn, Ananda Muthiar, Ricky Nilsson, Toba Oluyide, Michael Papin, Amalia Rivera, Melanie Swain, Nicholas D. Susemiehl, Raymond Tam, Julian van Eyken, Charles Beichman
Figure caption: Example of ground-based time series photometry of TOI-3569 obtained by the TFOP and shared with the community on ExoFOP (Section 2.2).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: For a differentiated projectile with D = 100 km, v = 16 km s−1, and θ = 30°, panel (a) shows the postimpact distribution of crustal thickness and (b) shows the postimpact distribution of iron ejecta from the projectile core. Panel (c) shows the postimpact distribution of projectile ejecta for an impact with the same parameters as in panels (a) and (b) except with an undifferentiated projectile. Panels (d)–(f) are the same as panels (a)–(c) except for a projectile with D = 50 km. All panels display global maps in an equirectangular projection with an arbitrary coordinate system oriented relative to the impact. The projectile approached from the left (uprange) and proceeded to the right (downrange). Gridlines demarcate acrossrange latitude in 30° increments and downrange longitude in 60° increments. The locations of the initial contact point for the impact and the corresponding point antipodal to the impact are annotated in red in panel (b). Panels (b), (c), (e), and (f) show that projectile ejecta converges at the antipodal point to the impact following great circle trajectories; projectile material is also prevalent on a trajectory immediately downrange of the impact zone (close to 0° acrossrange latitude).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Bar charts showing the postimpact projectile core thickness near the antipode of the impact site for differentiated projectiles. We show the peak thickness within 10° of the antipode (red) and the mean thickness within 2° (orange) and 5° (blue) of the location of the near-antipodal peak thickness. Charts are distributed in columns and rows according to the projectile velocity and diameter. The x-axis in each bar chart shows simulations with different impact angles (90° = head-on collision). Includes mistracked tracers. See Table B3.
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Current observed lunar remanent magnetic field strength (L. L. Hood et al. 2021, 2022). Several large impact basins are outlined in white and are potentially associated with antipodal magnetic signature groupings, which are marked with yellow arrows.
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Snapshots of a CTH simulation with parameters D = 175 km, v = 20 km s−1, θ = 45°, and a differentiated projectile (Run 23). The projectile approaches from the upper right, impacting at an oblique 45° angle from the tangent surface plane. Images show slices through the impact plane of a full 3D CTH simulation.
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Dependence of ejecta patterns on projectile size. Plots are for impacts at v = 16 km s−1 and θ = 45°, with each column of plots representing a different projectile diameter (D = 50 km, 100 km, or 175 km). The top row of plots (panels (a)–(c)) displays the postimpact distribution of projectile iron ejecta for simulations with differentiated projectiles. The bottom row of plots (panels (d)–(f)) displays the postimpact distribution of projectile rock ejecta for undifferentiated projectiles. All panels display global maps in an equirectangular projection with an arbitrary coordinate system oriented relative to the impact. The projectile approached from the left (uprange) and proceeded to the right (downrange). Gridlines demarcate acrossrange latitude in 30° increments and downrange longitude in 60° increments. The location of the initial contact point for the impact and corresponding point antipodal to the impact are annotated in red in panel (a).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Bar charts showing the postimpact projectile core thickness near the antipode of the impact site for differentiated projectiles. We show the peak thickness within 10° of the antipode (red) and the mean thickness within 2° (orange) and 5° (blue) of the location of the near-antipodal peak thickness. Charts are distributed in columns and rows according to the projectile velocity and diameter. The x-axis in each bar chart shows simulations with different impact angles (90° = head-on collision). Excludes mistracked tracers. See Table B3.
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: As Figure 4, but displaying the postimpact projectile material thickness near the antipode of the impact site for undifferentiated projectiles. Includes mistracked tracers. See Table B4.
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: As in Figure A7, but displaying the postimpact projectile thickness near the antipode of the impact site for undifferentiated projectiles. Excludes mistracked tracers. See Table B4.
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Dependence of ejecta patterns on impact velocity for a 100 km diameter projectile impacting at 60°. As in Figure A1 but with fixed D = 100 km, θ = 60°, and with each column representing a different impact velocity (v = 12 km s−1, 16 km s−1, 20 km s−1).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Dependence of ejecta patterns on impact velocity for a 100 km diameter projectile impacting at 45°. As in Figure A1 but with fixed D = 100 km, θ = 45°, and with each column representing a different impact velocity (v = 12 km s−1, 16 km s−1, 20 km s−1).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Dependence of ejecta patterns on impact velocity for a 100 km diameter projectile impacting at 30°. As in Figure A1 but with fixed D = 100 km, θ = 30°, and with each column representing a different impact velocity (v = 12 km s−1, 16 km s−1, 20 km s−1).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Dependence of ejecta patterns on impact angle for a 100 km diameter projectile. As in Figure A1 but with fixed D = 100 km, v = 16 km s−1, and with each column representing a different impact angle (θ = 30°, 45°, 60°).