adsabs/AstroCLIMB huggingface dataset:
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: The spectrum of Uranus as observed with TripleSpec, demonstrating the complex structure of methane absorption both within and outside of atmospheric windows. Note the change in scale on the y-axis between plots, the strong contamination between 1.48 and 1.63 μm, and the minimal flux in K band (order 3).
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Leading quadrant TripleSpec nightly average spectra of Miranda, presented at native resolution. All spectra are normalized to unity at 1.72 μm. Spectra are offset vertically in increments of +3.5 and +1 in the left panel and increments of +3.5, +2, +1, and +0 in the right panel. The subobserver longitude range spanned by each spectrum is denoted in the legend.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Anti-Uranus quadrant nightly average (left) and grand-average (right) TripleSpec spectra of Miranda. Spectra are offset vertically in increments of +3, +1.5, and +0 in the left panel and increments of +4.5, +3.5, +2.5, +1.5, and +0.5 in the right panel.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Sub-Uranus quadrant TripleSpec nightly average spectra of Miranda. Spectra are offset vertically in increments of +3.5, +1.5, and +0 in the left panel and increments of +3, +1.5, and +0.5 in the right panel.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Trailing quadrant TripleSpec nightly average spectra of Miranda. Spectra are offset vertically in increments of +4, +2, and +0 in the left panel and increments of +3.5, +2, +1, and +0 in the right panel.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: an annotated image of the Uranian system as observed with the TripleSpec K  s -band slit-viewing camera on 2020 September 7 (UT). Uranus, its ring system, and all five classical satellites are clearly visible in this 15 s exposure. The dark negative image above the slit is the result of subtracting a previous slit-viewer frame to decrease the sky background. Right panel: the orientation of the inner Uranian system as seen from Earth when the slit-viewer image was taken, at the beginning of acquisition of the UT200907 spectrum. The projected orbit of Miranda is shown, with markers denoting Miranda’s position when the centers of certain quadrants are facing Earth during each orbit. The axial tilt of the Uranian system is clear from the projected longitude–latitude grid on Uranus, with the north pole pointing toward the viewer. While the subobserver latitude may differ between Miranda and Uranus by a few degrees, this diagram is generally representative of the typical geometry during our 2019–2021 observations.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: A diagram summarizing the previously observed planetocentric and longitudinal trends in the surface compositions of the classical Uranian moons, excluding Miranda (Buratti & Mosher 1991; Grundy et al. 2003, 2006; Cartwright et al. 2015, 2018).
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: (A) Uninterpreted image of asteroid Lutetia as observed on 2010 July 10 by the OSIRIS camera on board Rosetta (Sierks et al. 2011). (B) Regional geological mapping obtained in (A). For the description of each geological unit (Achaia—Ac, Noricum—Nc, Narbonensis—Nb, Etruria—Et, Baetica—Bt), we refer to Massironi et al. (2012). (C) Uninterpreted image of the Rosetta Sais landing site on comet 67P/Churyumov–Gerasimenko (Sierks et al. 2015) taken on 2016 September 30 a few seconds before landing. (D) Geological map of (C). For a detailed description of each geological unit, we refer to Pajola et al. (2017a).
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: The DRACO simulated images obtained at 200 s (A), 120 s (B), 20 s (C), and 5 s (D) before DART impact. For all panels, Didymos is represented by the scaled shape model of Ryugu, while Dimorphos is the scaled version of Itokawa. Images are 512 × 512 pixel windows like those that will be streamed directly to Earth in real time.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: The LEIA simulated images obtained at T0, 12 s before LICIACube CA, at CA, 12 s after CA, and 60 s after CA. As for the DRACO simulated images, Didymos is represented by the scaled shape model of Ryugu, while Dimorphos is the scaled version of asteroid Itokawa. The white arrows point at Dimorphos in all panels. All images show the real targets’ dimensions in the LEIA 2048 × 2048 detector.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: The five NEAs observed from close range so far. Asteroids Eros (34 × 11 × 11 km size), Itokawa (0.5 × 2.9 × 2.1 km), and Toutatis (4.8 × 2.4 × 2.0 km) belong to the same S-type class as asteroid Didymos. Ryugu (1.04 × 1.02 × 0.88 km) is a C-type asteroid, while Bennu (0.57 × 0.54 × 0.51 km) belongs to the B-type class.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: Phase angles and resolutions of the LEIA acquisitions that will be taken from T0 – 50 s to T0 + 290 s. The red curve shows resolution as a function of time. The black curve shows phase angle as a function of time.
Paper: Spacecraft Geometry Effects on Kinetic Impactor Missions
Authors: J. Michael Owen, Mallory E. DeCoster, Dawn M. Graninger, Sabina D. Raducan
Figure caption:  β histories for weak target asteroid material strength (top row) versus strong (bottom row) for our menagerie of models performed in Spheral. The columns are organized by impactor geometry, with DART CAD models in the left column, cylinders in the middle column, and three-sphere geometries in the right column (the sphere result is plotted in each frame for reference). Note that the timescales in the top row are much longer than those in the bottom, because the weak representation of the asteroid produces ejecta over much longer times.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: (A) Three landslides (named Sarnus, Gallicum, and Danuvius) observed on the surface of asteroid Lutetia (from Massironi et al. 2012). (B) Mass movement examples as observed inside the Psyche crater on Eros. (C) The single ∼100 m-long mass movement (highlighted with the yellow arrows) is observed on the surface of Bennu (Jawin et al. 2020), entering a crater (the rim is indicated with white arrows).
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: (A) Examples of kilometer-long grooves and lineaments on the surface of asteroid (21) Lutetia (from Massironi et al. 2012). (B) The global distribution of lineaments on NEA (433) Eros (Buczkowski et al. 2008). (C)–(E) Examples of linear through-going fractures on the Bennu boulders ((C), (D) Molaro et al. 2020a, 2020b) and on Ryugu ((E), Sasaki et al. 2019). The white arrows point out the identified fractures.
Paper: Spacecraft Geometry Effects on Kinetic Impactor Missions
Authors: J. Michael Owen, Mallory E. DeCoster, Dawn M. Graninger, Sabina D. Raducan
Figure caption: (y, z) plane slices through the initial conditions for our various impactor geometries. The insets for the non-DART scenarios are zoomed-in because those impactors are much smaller than the actual DART geometry.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: (A) The boulder-rich surface of NEA Itokawa, as observed by Hayabusa. (B) The Itokawa global SFD of boulders as obtained by Mazrouei et al. (2014). (C) Boulders’ size grading on Bennu, as observed on a centimeter-scale OCAMS-Polycam (Rizk et al. 2018) image. (D) The southernmost region of asteroid Ryugu. The biggest boulder, called Otohime Saxum, has a size (160 m) that is comparable to the size of Dimorphos.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: (A) The cratered surface of Eros, as imaged by the NEAR/Shoemaker spacecraft. White arrows point to the asteroid’s multiple craters. (B) The surface of NEA Ryugu as observed by Hayabusa2. The largest crater identified on its surface is indicated with a white arrow. (C) An image of asteroid Bennu as observed by OSIRIS-REx draped over a low-resolution shape model in the Small Body Mapping Tool (Ernst et al. 2018). The largest equatorial crater is identified with a red circle and a white arrow.
Paper: Spacecraft Geometry Effects on Kinetic Impactor Missions
Authors: J. Michael Owen, Mallory E. DeCoster, Dawn M. Graninger, Sabina D. Raducan
Figure caption: DART spacecraft geometry initial conditions. The left panel shows the input CAD geometry for the spacecraft, the middle panel shows the polyhedral Voronoi reconstruction of the ASPH nodes in the Spheral (colored by material), and the right panel shows the CTH materials.
Paper: Anticipated Geological Assessment of the (65803) Didymos–Dimorphos System, Target of the DART–LICIACube Mission
Authors: M. Pajola, O. S. Barnouin, A. Lucchetti, M. Hirabayashi, R.-L. Ballouz, E. Asphaug, C. M. Ernst, V. Della Corte, T. Farnham, G. Poggiali, J. M. Sunshine, E. Mazzotta Epifani, N. Murdoch, S. Ieva, S. R. Schwartz, S. Ivanovski, J. M. Trigo-Rodriguez, A. Rossi, N. L. Chabot, A. Zinzi, A. Rivkin, J. R. Brucato, P. Michel, G. Cremonese, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, A. Cheng, B. Cotugno, M. Dall'Ora, R. T. Daly, V. Di Tana, J. D. P. Deshapriya, I. Gai, P. H. A. Hasselmann, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: An enhanced-RGB color image obtained on the S-type asteroid Ida and its satellite Dactyl, as obtained by the Galileo mission on 1993 August 28. Thanks to such a data set, a systematic difference between two of Ida’s major color terrains has been identified (Geissler et al. 1996; Veverka et al. 1996), as well as a different spectral trend on Dactyl.
Paper: The Lunar Geophysical Network Landing Sites Science Rationale
Authors: Heidi Fuqua Haviland, Renee C. Weber, Clive R. Neal, Philippe Lognonné, Raphaël F. Garcia, Nicholas Schmerr, Seiichi Nagihara, Robert Grimm, Douglas G. Currie, Simone Dell'Agnello, Thomas R. Watters, Mark P. Panning, Catherine L. Johnson, Ryuhei Yamada, Martin Knapmeyer, Lillian R. Ostrach, Taichi Kawamura, Noah Petro, Paul M. Bremner
Figure caption: Example LGN station locations (blue triangles) compared to Apollo (gray circles). LGN stations will be placed across major lunar terranes and enable new interrogation of the deep lunar interior and tectonic evolution. The proposed LGN stations are positioned to take advantage of (1) possible recent lobate scarp seismicity (green lines; Watters et al. 2019) and (2) known DMQ clusters and their antipodes (yellow and cyan stars, respectively). The two most active nearside and farside DMQ clusters (A01 and A33) are highlighted. DMQ cluster epicenters, each exhibiting characteristically repeating waveforms between 550 and 1420 km in depth, are thought to be caused by the tidal forces of the Earth–Moon system at intervals of 27–29 days (Weber et al. 2009). Their antipodes, where core-transmitted phases would be focused, are located on the opposite side of the Moon (Nakamura 2005). The LGN network is designed to geophysically interrogate the internal structure, temperature, composition, and tectonics/seismicity both in the Feldspathic Highlands (unsampled by Apollo) and within the Procellarum KREEP terrane, outlined by the Lunar Prospector thorium abundance (Lawrence et al. 2000). Shaded surface relief is derived from LOLA topography (Smith et al. 2017).
Paper: The Lunar Geophysical Network Landing Sites Science Rationale
Authors: Heidi Fuqua Haviland, Renee C. Weber, Clive R. Neal, Philippe Lognonné, Raphaël F. Garcia, Nicholas Schmerr, Seiichi Nagihara, Robert Grimm, Douglas G. Currie, Simone Dell'Agnello, Thomas R. Watters, Mark P. Panning, Catherine L. Johnson, Ryuhei Yamada, Martin Knapmeyer, Lillian R. Ostrach, Taichi Kawamura, Noah Petro, Paul M. Bremner
Figure caption: (a) Number of core-reflected shear-wave (ScS) phases and (b) number of core-traversing P-wave (PKP) phases detected per year (color bar) from 15 energetic DMQ nest epicenters (white stars) as a function of the location of a VBB seismometer. Black squares indicate LGN station locations. The numbers of (ScS; PKP) core phases detected at these positions are (87; 2), (78; 20), (45; 0), and (17; 35) for PKT, Schickard, Crisium, and Korolev stations, respectively. Vertical dashed lines mark the limit between farside and nearside. Computed for an rms noise level of 1.49e−11 m s−1 in the 0.07–0.14 Hz frequency range following the method described in Yamada et al. (2013).
Paper: The Lunar Geophysical Network Landing Sites Science Rationale
Authors: Heidi Fuqua Haviland, Renee C. Weber, Clive R. Neal, Philippe Lognonné, Raphaël F. Garcia, Nicholas Schmerr, Seiichi Nagihara, Robert Grimm, Douglas G. Currie, Simone Dell'Agnello, Thomas R. Watters, Mark P. Panning, Catherine L. Johnson, Ryuhei Yamada, Martin Knapmeyer, Lillian R. Ostrach, Taichi Kawamura, Noah Petro, Paul M. Bremner
Figure caption: Global distribution of lunar lobate scarps. These lobate thrust fault scarps (red lines) are found predominantly in the highlands, at all latitudes. Over 3500 of these young fault scarps have been detected thus far in LROC images. LGN proposed stations are marked (stars).
Paper: The Lunar Geophysical Network Landing Sites Science Rationale
Authors: Heidi Fuqua Haviland, Renee C. Weber, Clive R. Neal, Philippe Lognonné, Raphaël F. Garcia, Nicholas Schmerr, Seiichi Nagihara, Robert Grimm, Douglas G. Currie, Simone Dell'Agnello, Thomas R. Watters, Mark P. Panning, Catherine L. Johnson, Ryuhei Yamada, Martin Knapmeyer, Lillian R. Ostrach, Taichi Kawamura, Noah Petro, Paul M. Bremner
Figure caption: Ray path coverage for P (blue), PcP (green), and PKP (red) phases from the known distribution of DMQ clusters, rotated such that the station is fixed at 0° and stacking all stations in the array for LGN (top left) and Apollo (bottom left). Note LGN’s wider coverage in epicentral distance and the denser sampling of the deep interior. The box on the right shows ray coverage for each of the LGN stations separately.
Paper: The Lunar Geophysical Network Landing Sites Science Rationale
Authors: Heidi Fuqua Haviland, Renee C. Weber, Clive R. Neal, Philippe Lognonné, Raphaël F. Garcia, Nicholas Schmerr, Seiichi Nagihara, Robert Grimm, Douglas G. Currie, Simone Dell'Agnello, Thomas R. Watters, Mark P. Panning, Catherine L. Johnson, Ryuhei Yamada, Martin Knapmeyer, Lillian R. Ostrach, Taichi Kawamura, Noah Petro, Paul M. Bremner
Figure caption: (a) The impact of the A16 ascent vehicle recorded on the A16 LP seismometer. The digitization of the instrument is clearly visible as integer steps in the waveform. (b) A spectrogram, in acceleration power spectral amplitude, shows the spectral content and limitation of the 10-bit acquisition noise, shown in the final section of the spectrogram, after the black line. This 10-bit dynamic range also hinders the identification of seismic arrivals in the frequency domain. (c) LGN’s amplitude sensitivity will be a factor of 10 better than Apollo, as well as capturing a larger epicentral distance, enabling core phases to be resolved (e.g., core-reflected shear wave, ScS, core-traversing P-wave, PKP, core-reflected P-wave, PcP) on single records, in contrast to Apollo, which detected only direct P and S phases (Yamada et al. 2013). Red and black points are P and S phases observed from Apollo records, while the expected core phases were all below the instrument resolution and required stacking to detect. Theoretical amplitudes of body waves (color lines) are shown for DMQs as a function of epicentral distance.
Paper: Predicting Asteroid Material Properties from a DART-like Kinetic Impact
Authors: Kathryn M. Kumamoto, J. Michael Owen, Megan Bruck Syal, Jason Pearl, Cody Raskin, Wendy K. Caldwell, Emma Rainey, Angela M. Stickle, R. Terik Daly, Olivier Barnouin
Figure caption: Parallel coordinate plots showing all input variables of the inverse simulations, as well as final ΔV and β. Simulation lines are colored by the difference between the simulation ΔV and the target ΔV, with blue being slower than the truth simulation and red being faster than the truth simulation. White stars indicate the values of the truth simulation. For ϕ, the open star indicates the original truth simulation value of 0.24 while the solid white star indicates the porosity required for an equivalently massive asteroid in our simulations. Plots are shown for (a) all simulations, (b) simulations with initial asteroid mass within 10% of the truth simulation, and (c) simulations with Y s0 within 1 order of magnitude of the truth simulation. Ticks and axis limits in (b) and (c) are the same as in (a).