adsabs/AstroCLIMB huggingface dataset:
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Distribution of meteorite analogs found in the present study. Meteorite abbreviations are H-, L-, and LL-ordinary chondrites; carbonaceous chondrites (CC); HEDs; aubrites and enstatite chondrites (A/EC); and indeterminate (IND). The source regions of the NEOs are indicated with different colors.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Left: spectra of NEOs 2013 CW32, 2016 CM194, 2017 WX12, and 2019 SH6. All the spectra show absorption bands centered at ∼0.9 and 2.0 μm due to the minerals olivine and pyroxene. Spectra have been offset for clarity. Right: continuum-removed spectra of the same objects. The mean spectrum of an S-type from DeMeo et al. (2009) is also shown.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: (Top) The raw photometric data of 2023 DZ2 in apparent observed magnitude showing all data collected in the campaign with the various photometric filters used indicated with different plotting colors (see legend). The vertical dotted line shows the time of closest approach when 2023 DZ2 reached its peak brightness. (Middle) Reduced magnitude with the observer-to-object distance dependence on the brightness removed. Two H–G model curves are shown, one with the G and HV, α = 0 values fixed to 24.3 and 0.15, respectively, obtained from JPL and the other an attempt at fitting the H–G model to the photometry data collected during the entire campaign. We only fit the V-filter data together with the g and unfiltered data (calibrated in the V and G bands) since the V–g, V–clearV, and V–clearG colors for the campaign data were only −0.23, 0.01, and 0.12 mag, respectively (i.e., V ≈ clearV ≈ clearG ≈ g). The fitted values for G and HV, α = 0 values are 24.82 ± 0.24 and 0.46 ± 0.23, respectively. (Bottom) Evolution of absolute magnitudes of 2023 DZ2 for the entire campaign as a function of time.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Echo power spectra obtained on March 25 of 2023 DZ2 using the 70 m DSS-14 antenna at Goldstone to transmit and receive. Echo power in standard deviations of the noise is plotted as a function of Doppler frequency using JPL/Horizons solution 11. The solid curve denotes echo power in the opposite sense of circular polarization relative to that transmitted, and the dashed curve shows echo power in the same sense. The frequency resolution is 1.0 Hz, and the figure shows a weighted sum of 19 runs.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: (Top) The LS periodogram of the combined filter data (see Section 3). The arrow shows the strongest periodogram peak and the rotation period labeled. The rotation period is 6.2745 ± 0.0030 minutes. (Bottom) The combined filter data (from the derived colors; see Section 3) are folded with the best period solution (shown in the top panel) and 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 light-curve amplitude displayed in the top left corner of the panel.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Visible and near-infrared spectra of 2023 DZ. The top spectrum combines spectra from GTC OSIRIS and NASA IRTF SpeX instruments. The bottom spectrum is visible and near-IR data from RAPTORS I and NASA IRTF SpeX. A weak 0.9 μm absorption feature due to pyroxene is visible in the bottom higher-SNR spectrum from the NASA IRTF.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Echo power spectrum obtained on March 25 of 2023 DZ2 using the 34 m DSS-34 antenna at Canberra to transmit and the ATCA to receive. Notation is the same as in Figure 4. This shows an integration of 2.1 hr at a frequency resolution of 1.0 Hz.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Diagram of the 2023 March 25 close approach of 2023 DZ2 to Earth. The relative velocity at closest approach is 7.8 km s–1. 2023 DZ2 moves from left to right in this plot.
Paper: 2023 DZ2 Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Lance Benner, Jessie Dotson, Nicolas Erasmus, Davide Farnocchia, Tyler Linder, Joseph R. Masiero, Cristina Thomas, James Bauer, Miguel R. Alarcon, Paolo Bacci, Daniel Bamberger, Adam Battle, Zouhair Benkhaldoun, Guido Betti, Mirel Birlan, Marina Brozovic, Brian Burt, David C. Cantillo, Sunil Chandra, Gregoire Chomette, Ashley Coates, Francesca DeMeo, Maxime Devogèle, Petr Fatka, Marin Ferrais, Paolo Fini, Carel van Gend, Jon D. Giorgini, Dmitry Glamazda, Robert Holmes, Joseph L. Hora, Shinji Horiuchi, Kamil Hornoch, Marco Iozzi, Cristóvão Jacques, Emmanuel Jehin, Hai Jiang, Galina Kaiser, Peter Kušnirák, Eduard Kuznetsov, Julia de León, Alexios Liakos, Javier Licandro, Tim Lister, Jing Liu, Andy Lopez-Oquendo, Martina Maestripieri, Donovan Mathias, Marco Micheli, Shantanu P. Naidu, Alessandro Nastasi, Alin Nedelcu, Elisabeta Petrescu, Marcel Popescu, Stephen B. Potter, Petr Pravec, Juan Sanchez, Toni Santana-Ros, Miquel Serra-Ricart, Nick Sioulas, Adrian Sonka, Alessio Squilloni, Maura Tombelli, Madalina Trelia, David E. Trilling, Elizabeth Warner, Guy Wells, Lorien Wheeler, Mike Wiles
Figure caption: Heliocentric osculating orbit of 2023 DZ2 viewed from the northern ecliptic pole.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Mean terminator distances for the bow shock ((i), (ii), and (iii)) and the induced magnetospheric boundary ((iv), (v), and (vi)) for all dayside crossings from 2007 May 1 to November 30. Values have been split into three longitude bands for 0°–120°, 120°–240°, and 240°–360°, and the mean value has been calculated for all crossings within each longitude band. (i) and (iv) are mean values for all latitudes within the band split, (ii) and (v) are for the areas defined as having “strong” crustal magnetic fields (see Table 3) in each band split, and (iii) and (vi) are regions with “weak” crustal magnetic fields. Green points are for boundary crossings before the global dust storm, red are for the peak and decay phases of the storm, and blue shows data after the global dust storm has ended (Table 4). Boundary positions are calculated by using the 2D model.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Mean terminator distance of the induced magnetospheric boundary calculated per 10° × 10° bin across the Martian surface, for all dayside crossings of the IMB from 2007 May 1 to November 30. Base map is the Martian topography for reference to surface features. Topography obtained by the digital elevation model of the Mars Global Surveyor’s Mars Orbiter Laser Altimeter (USG 2023).
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Orbit of Mars Express in Mars Solar Orbital coordinates in two-month intervals from 2007 April to December.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Ionosphere profile for electron density, calculated from MARSIS data. Colors indicate different dust storm phases, with red being the pre-global dust storm (May 29), black the start of the global storm (June 29), and blue during the global dust storm (July 29).
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Mean terminator distances per 10° × 10° bin for the bow shock (a)–(c) and the induced magnetospheric boundary (d)–(f), split by storm phase outlined in Table 4.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Radial crustal magnetic field strength from the G110 model at 120 km altitude, taken from Gao et al. (2021).
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Potential causes of the depression in the induced magnetospheric boundary over crustal fields found in the 2007 global dust storm. Not to scale.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Number of induced magnetospheric boundary crossings per bin used in Figure 6.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Number of bow shock crossings per bin used in Figure 5.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Tumbler lightcurves of NEOs included in the photometric study.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Partial lightcurves of NEOs included in the photometric study.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Flat lightcurves of NEOs included in the photometric study.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: (a) The radar shape, the starting DTM for all of the synthetic asteroids. (b) Shape 2 was the first truth model used in testing. It lacked albedo variation, so it was of limited benefit during testing. (c) The shape 3 truth model was used for most of the testing. This model comprised the source data for almost all of the baseline and sensitivity tests. The entire surface was rough with large boulders and provided no location that met the prelaunch expectations for a suitable sample collection site. These roughness attributes were modeled according to observations of the asteroids Itokawa and Eros (see Barnouin et al. 2020, for details). (c) The shape 4 truth model was used for two tests that fully simulated the DTM generation that would be conducted once at Bennu (Weirich 2022).
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: This shows the observational geometries for the (a) original DRM and (b) expanded DRM. These only show the Preliminary Survey and Detailed Survey images. The image pixel size is as follows: cyan is 30–60 cm, blue is 10–15 cm, and black is 4–5 cm. The polar plot is an effective way to describe the viewing geometries by displaying both the azimuth angle and zenith angle. The polar plot shows the position of the spacecraft (squares) and the position of the Sun (circle). Both plots are viewed from the surface looking up. The radial grid lines indicate azimuth, where north is 0° and east is 90°. The concentric grid lines indicate the zenith angle, with 0° being straight up. This example is based upon the testing TAG site, which was at −8° latitude.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: Two synthetic images rendered from shape 3 of the testing site. The left image depicts a typical image that would be taken from the original Baseball Diamond portion of the Detailed Survey mission phase. The latitude of the terrain is 0°. The right image is in the same location but illuminated as if it were at −70° latitude. One can see that the shadows are much longer, with many south-facing slopes no longer illuminated. The white box denotes the evaluation region that is depicted in Figure 4.
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Example of the axes retrieval by VADER in a LUKE image (4241 one zoomed in—see Table 1 for definition of images). The orange rectangle is the one identified by VADER as the area in which the dark hemisphere is inscribed. The long axis “a” is as long as the rectangle side used to retrieve it, whereas the short axis “b” is half of the rectangle side used for its computation. Note that, with respect to Figure 1, the dark areas are those bright in Figure 1 (i.e., in the original LUKE image); this is due to the thresholding described in the text.
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Zoom-in of images acquired by LUKE just (a) before and (b) after the CA, showing the plume partially covering the surface of Dimorphos. (c) Image liciacube_luke_l2_1664234241_00007_01 adequately zoomed in and contrasted, showing the plume shadow over the dayside hemisphere of Dimorphos. The shadow is visible on the lower left side of the ellipse. The green circle is the centroid of the blue ellipse, which is the same as that computed for the 4241 image with VADER.