adsabs/AstroCLIMB huggingface dataset:
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Sketch of the impact setup. (a) Accelerator and impact bed with microscope slides to the side, trapping airborne dust and wires to provide an inhomogeneous electrical field. Camera on the right (distance bed–camera not to scale). (b) Cross section of the accelerator unit; about 20–50 impactors are released from a particle reservoir by rotating (gear motor) a portioning wheel. They fall in the path of the plunger and are launched when it is accelerated by the solenoid; the aperture guides the impactors to the soil.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Thermal fracture is likely an important process on Psyche’s surface. The timescale of cracking will depend on the magnitude of the elastic forces countering thermal stress. The Paris law coefficient of C = 10−12 m [MPa ﹩\sqrt{{\rm{m}}}﹩]−m  is from industrially produced metals and so is unlikely to be representative of Psyche’s surface material. Horizontal dashed lines are the number of Earth years needed to reach that number of seasonal cycles, and a 0 is the initial crack size.
Paper: Releasing Atmospheric Martian Dust in Sand Grain Impacts
Authors: T. Becker, J. Teiser, T. Jardiel, M. Peiteado, O. Muñoz, J. Martikainen, J. C. Gomez Martin, G. Wurm
Figure caption: Image of an impact, showing the impactor as a white circle as well as a cloud of ejecta.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Plots demonstrating the effect of varying column density (a), velocity (b), and temperature (c) on output spectral line profiles compared to the observed line profile of NaCl aperture 1 on 2015 June 9.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Each row shows NaCl/KCl emission (far left) for each date of observation in this study, followed by a series of images of SO2 emission taken concurrently. For all images, all scans (sunlight and/or eclipse) are combined. The SO2 images from left to right show SO2 emission across the emission line, where the leftmost image is emission on the blueshifted side of the line wing, the middle image is emission at the center of the line, and the rightmost image is emission on the redshifted side of the line wing. See de Pater et al. (2020) for more detailed analysis.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Flux density vs. time for four different SO2 transitions on 2016 July 26 when Io was observed moving from eclipse into sunlight. The flux densities have been determined from the center line emission maps of each ∼3 minutes scan (i.e., maps integrated over 0.4 km s−1) by integrating the flux density on each map over the disk of Io. The gray dotted line represents the beginning of eclipse egress (when Io first moves into sunlight), after which the SO2 atmosphere reforms.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Example continuum image from 2016 July 26, where the lower left white circle is the HPBW, and the white circle in the center of the image is determined to be the edge of the disk of Io, which is then used to determine Io’s size and location in the corresponding spectral line images.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: (a) NaCl emission (260.2 GHz) from 2016 July 26, (b) SO2 emission (262.2 GHz) in eclipse taken concurrently with panel (a), (c) KCl emission (344.8 GHz) from 2018 March 20, and (d) SO2 emission (346.6 GHz) in eclipse taken concurrently with panel (c). All maps were integrated over 0.4 km s−1 at the line center.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Example plot of Δχ 2 model fits to NaCl (260.2 GHz) observed on 2016 July 26 for temperatures ranging from 0 to 2000 K, column densities ranging from 1012 to 1014 cm−2, and a velocity of 120 m s−1. The top left inset indicates the aperture modeled, and the top right inset shows the line profile with the best-fit line model. These plots were made for each aperture analyzed in this work and are shown in Figures 12 and 13 in the Appendix.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Plots of Δχ 2 = 4.61 contours for each aperture, with NaCl apertures on the left and KCl apertures on the right. Detailed plots of each aperture are shown in Figures 12 and 13 in the Appendix.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Top row: KCl emission from 2018 March 20 imaged over all scans (a) and separated into sunlight (b) and eclipse (c) scans. Bottom row: NaCl emission from 2016 July 26 imaged over all scans (d) and separated into sunlight (e) and eclipse (f) scans. All images from the same dates are imaged on the same color scale for easy comparison, and the rms error is noted in the bottom corners of each image.
Paper: NaCl and KCl in Io’s Atmosphere
Authors: Erin Redwing, Imke de Pater, Statia Luszcz-Cook, Katherine de Kleer, Arielle Moullet, Patricio M. Rojo
Figure caption: Approximate locations of NaCl and KCl emission apertures from all observations. Purple circles are approximate KCl locations, green circles are approximate NaCl locations, and red circles are approximate locations where NaCl and KCl were observed concurrently. Base map from Williams et al. (2011).
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Annotated version of the geologic map of Miranda’s imaged southern hemisphere (Croft & Soderblom 1991). The locations of heat flux estimates for Miranda are shown (Beddingfield et al. 2015a, 2022b). The Global Rift System is made up of the large fault scarps including Verona Rupes, Argier Rupes, the 340° Chasma, and the SPT Chasma (see the canyon materials geologic units). See Figure 6 for the highest-resolution Voyager 2 ISS images of Miranda and their locations. As summarized in Croft & Soderblom (1991), the geologic map units of Miranda are as follows. Mh: heavily mantled cratered terrain, Ml: lightly mantled cratered terrain, Pf: flow material in Elsinore, Ps: southern ridged plains in Elsinore, Pn: northern ridged plains in Elsinore, Pd: dark material in Arden and Inverness, Pm: medium albedo material in Arden, Pl: light albedo material in Arden and Inverness, Pv: very dark albedo material in Inverness, Pw: wisp-like light material in Inverness, Rl: light albedo canyon slope material, Rm: medium albedo canyon slope material, Rd: dark albedo canyon slope material, Rf: fractured canyon floor material, Rh: hummocky canyon floor material, Cf: fresh impact craters, and Ce: elongate/chain craters.
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: Examples of muted scarps and craters with more subtle features, and non-muted scarps and craters with more prominent features. Verona Rupes appears to be a non-muted scarp (orange arrows), with little evidence for mantling material on its surface. Individual corrugations are observable on the face of Verona Rupes, indicating the exposure of “bed-ice” material. In contrast, the Argier Rupes is muted (blue arrows) and has small impact craters, which may be secondary craters. Similarly, Alonso Crater (orange star) is non-muted, whereas Prospero Crater (blue star) is muted. This figure covers a portion of Voyager 2 ISS image c2684617 (284 m pixel−1).
Paper: Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source
Authors: Chloe B. Beddingfield, Richard J. Cartwright
Figure caption: (a) Illustration showing that a fresh crater can become a mantled crater when located in a deposition-dominated environment, a degraded crater when in an erosion-dominated environment, or a relaxed crater if viscous relaxation has taken place. (b) Examples are shown of a fresh crater (Beddingfield et al. 2021b), a mantled crater (Beddingfield et al. 2018), and a degraded crater (Beddingfield et al. 2021b), all on Mars, as well as a relaxed crater on Enceladus (Bland et al. 2018).
Paper: Discovery of the Closest Saturnian Irregular Moon, S/2019 S 1, and Implications for the Direct/Retrograde Satellite Ratio
Authors: Edward Ashton, Brett Gladman, Matthew Beaudoin, Mike Alexandersen, Jean-Marc Petit
Figure caption: Offset of S/2019 S 1 relative to Saturn (red dot). Colored circles represent a detection of the moon, with the dashed line showing the best-fit orbit (as seen from moving Earth; hence the Saturnocentric orbit does not close). Each color represents a different calendar year, with the 2019 (purple) arc starting from 2019 July 1. Also shown is the projected orbit of the outermost regular moon, Iapetus, during the same time frame (gray dotted line). Three shaded circles centered on Saturn, with radii of 12′ (red), 18′ (yellow), and 24′ (green), indicate plausible regions of severe, moderate, and mild scattered light (see text).
Paper: Discovery of the Closest Saturnian Irregular Moon, S/2019 S 1, and Implications for the Direct/Retrograde Satellite Ratio
Authors: Edward Ashton, Brett Gladman, Matthew Beaudoin, Mike Alexandersen, Jean-Marc Petit
Figure caption: Predicted orbits of S/2019 S 1 (top panel), Ijiraq (middle panel), and Kiviuq (bottom panel) from 1990 to 2026 at 1 day intervals. When a moon is within 20° of opposition it is represented by a large blue dot, when it is not within 20° it is represented by a smaller faded dot. The boundary of the red, yellow, and green zones are indicated on each panel.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Histogram plots for various predicted quantities on encounter day (2019 January 1). The model assumes ﹩{ \mathcal I }=2.54﹩ tiu and ε = 0.9. The vertical axis corresponds to the number of facets. Of the shown panels: (far left) Distribution of surface temperatures, (middle left) total received flux, (middle right) flux received as reradiation from the surrounding landscape, and (far right) surface conductive flux in which a negative value corresponds to the surface-directed flow of energy from the interior. In the last of these, note the trailing wing corresponding to the intense flux ring seen evident in Figure 9.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Predicted temperatures based on the simple theory of Section 2. Each panel shows the predicted temperatures as a function of distance from the Sun (r) and thermal inertia (﹩{ \mathcal I }﹩). All models assume A = 0.06 and ε = 0.9. The background flux consists entirely of the microwave background. The panels depict the (left panel) predicted summer season temperatures T  s,s , (middle panel) predicted interior temperatures T int, and (right panel) predicted winter season temperatures T  s,w . The vertical hatched lines show the location of 44 au, and various isotemperature lines of interest are shown with white curves.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Predicted surface temperatures on encounter day (2019 January 1) on the assumption ﹩{ \mathcal I }=2.54﹩ tiu and ε = 0.9. The upper left shows a view of the body on approach while the lower left depicts the view of Arrokoth during the CA08 observation. The upper- and lower-right panels are the same model but rotated to emphasize the view of the equatorial regions.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Subsolar latitude on Arrokoth (λ  ss , top panel) and its instantaneous distance from the Sun (r, bottom panel) over the course of one Arrokoth orbit and consistent with the body’s 99.°1 obliquity. The encounter-day properties are shown with a vertical hatched line. These are solutions based on the study found in Porter et al. (2018).
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Four views of the conductive flux (Λ ≡ K∂ z  T  i ) at encounter day. The arrows on the color bar show the range of flux values (also see Figure 7). The white line shows the transition from inward to outward conductive flux. The four views are in the same orientation as those shown in Figure 6. The intense surface-directed ring follows the temperature terminator (see Figure 6).
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: A Lucy–Richardson stacked deconvolved image from the LORRI CA06 sequence (images LOR_0408626328 through LOR_0408626336). A single longitude/latitude graticule centered on the spin pole is overlaid. The negative-spin pole faced the Sun during the New Horizons flyby. Thus, this view corresponds to the “southern” hemisphere.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Percent of sky self-obscured for the 105 merged shape model. The views shown are approximately from the approach trajectory (CA03, top panel) and departure trajectory (CA07, bottom panel). This references discussions found in both Sections 3.1–3.2, as well as Appendix A.
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: View of Arrokoth (CA07) taken by the LORRI camera on its departure trajectory approximately 10 minutes prior to the second REX scan (Grundy et al. 2020). The lit crescent seen here would have appeared somewhat diminished during the actual REX scan (∼10° shift in viewing geometry).
Paper: A Near-surface Temperature Model of Arrokoth
Authors: Orkan M. Umurhan, William M. Grundy, Michael K. Bird, Ross Beyer, James T. Keane, Ivan R. Linscott, Samuel Birch, Carver Bierson, Leslie A. Young, S. Alan Stern, Carey M. Lisse, Carly J. A. Howett, Silvia Protopapa, John R. Spencer, Richard P. Binzel, William B. McKinnon, Tod R. Lauer, Harold A. Weaver, Catherine B. Olkin, Kelsi N. Singer, Anne J. Verbiscer, Alex H. Parker
Figure caption: Four views of the temperature at a depth of ∼1 m at encounter day. The arrows on the color bar show the range of temperature values at this depth. The four views are the same orientation as those shown in Figure 6.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: (A) Photometric reduced magnitude with the observer-to-object distance dependence on the brightness removed. The H-G model fit is shown, with the derived G and H V values shown in the top-right corner. (B) The Lomb–Scargle periodogram of the combined filter data. The arrow shows the strongest periodogram peak with the lightcurve period (i.e., half the rotation period) and the rotation period labeled. The rotation period of P = 30.55 ± 0.12 hr matches the strongest lightcurve amplitude for the second harmonic of the period. (C) The combined photometric data folded with the best period solution and with a Fourier series fit shown as a solid burgundy line. The burgundy triangles show the minimum and maximum values of the fit and are used to determine the lightcurve amplitude displayed in the top-left corner of the panel.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: Impact probability evolution as a function of the uncertainty in the ζ coordinate on the 2029 B-plane. The solid curve represents the theoretical evolution with the nominal set of observations to the known 38,000 km miss distance. The dashed curve is the theoretical evolution of an impacting trajectory. The dotted vertical lines mark the orbit updates during the campaign. The crosses represent the corresponding impact probabilities. The triangles correspond to the impacting clone, introduced as the impact probability that departed from the dashed curve. Dates are in the YYMMDD compressed format.