adsabs/AstroCLIMB huggingface dataset:
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Example of a strong feature viewed under different imaging geometries (images are shown in the orientation at which they were taken and reviewed). Feature 37917 is outlined in green in the two images. For reference, the dark rocks in the upper left corner of the left panel marked with a red cross appear in the lower left corner of the right panel. The image on the left has an incidence angle of 41° and an emission angle of 3°. The image on the right has an incidence angle of 46° and an emission angle of 44°. In each image, the green box is approximately 18 m × 18 m. Both are cropped from OCAMS PolyCam images, with north upward on the left and north leftward on the right.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Expected emission angle, incidence angle, and GSD for feature R0015 at images 27−30 in the TAG trajectory. The blue line in the left panel represents the potential emission angles, the red line in the left panel represents potential incidence angles, and the blue line in the right panel represents potential GSDs. Error bars represent the minimum and maximum values observed in the Monte Carlo testing.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: NFT uses the DTM of the TAG site, Nightingale (left), together with the estimated relative position and velocity of the spacecraft, to estimate the location and time of the spacecraft's intersection with the surface of Bennu. The DTM contains the information to convert the displacements to a 3D model of the surface (right). The DTM is oriented with north upward. The DTM is a 127 × 127 array, 30.48 m on each side.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: The features used in measurements for each image collected during rehearsals and TAG. Blue open circles represent features used during TAG, red filled circles represent features used during Checkpoint rehearsal (CPR), light-blue dots represent features used during Matchpoint rehearsal (MPR), and gray bars represent expected image outages. In both rehearsals and in TAG, nearly all of the MLNs that were unused were only in the catalog for off-nominal trajectories resulting from ODM errors.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: The NFT hazard map is an additional layer of the TAG site DTM that provides the unsafe surface locations for TAG. If the NFT estimate uncertainty had included too large an unsafe area, a wave-off, resulting in a backaway burn, would have been triggered. The map is 30.48 m on each side, with north upward. The highlighted red areas are the locations in and around Nightingale that were deemed unsafe for TAG due to surface slope or tip-over hazard. The remaining gray areas were deemed safe for contact.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Example correlation performance of test images vs. expected TAG image conditions for feature M0004. Blue circles represent the expected TAG image conditions, green crosses represent the test images that scored highly, yellow crosses represent test images that scored in a passing but degraded range, and red crosses represent test images that scored below the passing threshold of 0.45. This feature performed with an average correlation score of 0.77 during the actual TAG event, indicating that this methodology provides robust validation.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: The first image of Nightingale (image 28) that was taken for processing after the Matchpoint maneuver. The targeted TAG location is in the upper portion of the image. The hazard map boundary is shown along with the measured feature locations in the image. This image covers approximately 35.4 × 26.6 m of the surface. North is toward the lower right corner of the image.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Left panel: comparison between a circumbinary orbit computed without radiation pressure (blue line) and one where radiation pressure is included and computed for a 50 cm radius particle (green line). The black line marks the orbit of Dimorphos around Didymos. Right panel: comparison between a satellite orbit computed without radiation pressure (blue line) and one where radiation pressure is included and computed for a particle having a radius of 1 cm (green line). The black line marks the orbit of Dimorphos around Didymos.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Left panel: orbital elements of the particle of Figure 9 (blue line) compared with the elements of a cloned particle where the Y-coordinate was changed by 5 cm with respect to the particle of Figure 9. Right panel: time evolution of the Cartesian coordinates of the trajectory depicted in Figure 9 (orange line) compared to the cloned particle with a ΔV of 0.87 cm s−1 (blue line).
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Left panel: snapshot of a simulation showing the initial evolution (151 s after the impact) of a group of 500 particles (∼5 cm in size) with the full dynamical model. The assumed reference frame (nonrotating) is initially oriented along the principal inertia axes of the central body at time zero. The arrow shows the direction to the Sun. Right panel: detail, centered on Dimorphos, from the same simulation as in the left panel (93 s after the impact).
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Left panel: full trajectory of the longest-living particle. Right panel: detail of the final orbits from the left panel. The blue circle represents the orbit of Dimorphos around Didymos.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Orbits that are stable over 2 yr of numerical integration. The black line marks the orbit of Dimorphos around Didymos. Note that in these simulations, the SRP is neglected. As mentioned in the text, this accounts for the observed stability.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Circumbinary (green line) and circumprimary (purple line) orbits initially started on inclined trajectories (i = 45°). Due to the nodal precession, the orbits form a belt around the primary.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Semimajor axis (top panel), eccentricity (middle panel), and equatorial inclination (bottom panel) of the trajectory shown in Figure 9.
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Trajectory of a fragment during a simple close approach to Dimorphos (left panel) and a more complex one characterized by a temporary capture around the asteroid (right panel).
Paper: Dynamical Evolution of Ejecta from the DART Impact on Dimorphos
Authors: Alessandro Rossi, Francesco Marzari, John Robert Brucato, Vincenzo Della Corte, Elisabetta Dotto, Simone Ieva, Stavro Lambrov Ivanovski, Alice Lucchetti, Elena Mazzotta Epifani, Maurizio Pajola, Giovanni Poggiali, Angelo Zinzi
Figure caption: Impact time distribution for the three considered sets of 5 cm–sized particles: spherical (blue line), ellipsoidal with regular rotation (red line), and ellipsoidal with random rotation (black line).
Paper: CAMEMBERT: A Mini-Neptunes General Circulation Model Intercomparison, Protocol Version 1.0.A CUISINES Model Intercomparison Project
Authors: Duncan A. Christie, Elspeth K. H. Lee, Hamish Innes, Pascal A. Noti, Benjamin Charnay, Thomas J. Fauchez, Nathan J. Mayne, Russell Deitrick, Feng Ding, Jennifer J. Greco, Mark Hammond, Isaac Malsky, Avi Mandell, Emily Rauscher, Michael T. Roman, Denis E. Sergeev, Linda Sohl, Maria E. Steinrueck, Martin Turbet, Eric T. Wolf, Maria Zamyatina, Ludmila Carone
Figure caption: Initial temperature profiles for K2-18b and GJ 1214b. The solid lines indicate the initial temperature profiles for each planet while the shaded regions indicate the range of equilibrium temperatures T eq in the temperature-forced case (see Equation (4)).
Paper: CAMEMBERT: A Mini-Neptunes General Circulation Model Intercomparison, Protocol Version 1.0.A CUISINES Model Intercomparison Project
Authors: Duncan A. Christie, Elspeth K. H. Lee, Hamish Innes, Pascal A. Noti, Benjamin Charnay, Thomas J. Fauchez, Nathan J. Mayne, Russell Deitrick, Feng Ding, Jennifer J. Greco, Mark Hammond, Isaac Malsky, Avi Mandell, Emily Rauscher, Michael T. Roman, Denis E. Sergeev, Linda Sohl, Maria E. Steinrueck, Martin Turbet, Eric T. Wolf, Maria Zamyatina, Ludmila Carone
Figure caption: Chemical abundance profiles for K2-18b and GJ 1214b to be used in case 3. These are publicly available in the CAMEMBERT repository (see Section 4.2).
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2015 April 13 to 2015 April 14. (a) Data showing all light-curve components, folded with the synodic orbital period. (b) Secondary (orbital) light-curve component, derived after subtraction of the primary light-curve component, showing the mutual events between the components of the binary system. The horizontal line indicates the mean level outside mutual events (corresponding to C 0). (c) Primary light-curve component.
Paper: ExoCAM: A 3D Climate Model for Exoplanet Atmospheres
Authors: Eric T. Wolf, Ravi Kopparapu, Jacob Haqq-Misra, Thomas J. Fauchez
Figure caption: Sensitivity scatter plots for hab1 (left) and hab2 (right) simulation sets. The global mean shortwave net cloud forcing (longwave + shortwave) is plotted against the global mean clear-sky greenhouse effect. The control simulation is indicated by the orange cross. Sensitivity tests are indicated by the blue diamonds, with significant outliers labeled.
Paper: ExoCAM: A 3D Climate Model for Exoplanet Atmospheres
Authors: Eric T. Wolf, Ravi Kopparapu, Jacob Haqq-Misra, Thomas J. Fauchez
Figure caption: Sensitivity scatter plots for hab1 (left) and hab2 (right) simulation sets. The global mean column integrated ice water cloud amount is plotted against the global mean column integrated water vapor amount. The control simulation is indicated by the orange cross. Sensitivity tests are indicated by the blue diamonds, with significant outliers labeled.
Paper: ExoCAM: A 3D Climate Model for Exoplanet Atmospheres
Authors: Eric T. Wolf, Ravi Kopparapu, Jacob Haqq-Misra, Thomas J. Fauchez
Figure caption: Sensitivity scatter plots for hab1 (left) and hab2 (right) simulation sets. The global mean shortwave cloud forcing is plotted against the global mean longwave cloud forcing. The control simulation is indicated by the orange cross. Sensitivity tests are indicated by the blue diamonds, with significant outliers labeled.
Paper: ExoCAM: A 3D Climate Model for Exoplanet Atmospheres
Authors: Eric T. Wolf, Ravi Kopparapu, Jacob Haqq-Misra, Thomas J. Fauchez
Figure caption: Sensitivity scatter plots for hab1 (left) and hab2 (right) simulation sets. The global mean column integrated water cloud amount (liquid + ice) is plotted for the substellar hemisphere mean value against the antistellar mean value. The control simulation is indicated by the orange cross. Sensitivity tests are indicated by the blue diamonds, with significant outliers labeled.
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Numerical modeling of Didymos-shaped rubble piles’ evolution under spin-up by the YORP effect, a torque caused by the scattering of sunlight and reemission of thermal radiation from an irregularly shaped body (Rubincam 2000), showing the sensitivity of the structural stability to the spin state and the different possible evolutionary pathways (adapted from Zhang et al. 2021). Top: a strength-dominated case with a bulk density of 1820 kg m−3 and bulk cohesion of ∼39.0 Pa; bottom: a gravity-dominated case with a bulk density of 2170 kg m−3 and bulk cohesion of ∼15.0 Pa. Particles are color-coded by their translational speeds. The spin period T spin of the body is given below each frame. The body was subject to spin acceleration in the beginning and then evolved without external influence after its structure failed (as indicated by the two long arrows; the spin rate decreases in the reconfiguration process owing to angular momentum conservation). In both cases, the rubble-pile structures can be stable at Didymos’s current spin with a small increment of ∼0.5 Pa in the bulk cohesion. The results were obtained by soft-sphere discrete-element modeling using the numerical code pkdgrav (Schwartz et al. 2012).
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Left: image of the asteroid Ryugu by Hayabusa2's Optical Navigation Camera (ONC) and its biggest boulder, Otohime Saxum. Right: model of the Didymos system. The size of Dimorphos is about the size of the biggest boulder on Ryugu.
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Numerical simulation results: (a, b) Bern’s smoothed particle hydrodynamics or SPH code (adapted from Raducan & Jutzi 2022); (c, d) iSALE-2D (adapted from Raducan et al. 2019) showing the target profile after DART-like impacts into porous Dimorphos-like targets, with varying cohesion (Y 0). DART-like impacts into strong targets (Y 0 >1 kPa) can be modeled using simplified target geometry (half-space). On the other hand, impacts into weak targets (Y 0 < 1 kPa), which have a larger cratering efficiency and larger crater formation times (up to 2 hr), require that the entire geometry of the target is numerically resolved. In these impact scenarios, the curvature of the target is important. Moreover, impacts into targets of cohesion less than about 10 Pa create structures dissimilar to cratering, producing global deformation of the target at the same time (Raducan & Jutzi 2022).
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Distance from Hera to Didymos/Dimorphos and AFC image resolution. ECP: Early Characterization Phase; PDP: Payload Deployment Phase; DCP: Detailed Characterization Phase; COP: Close Observation Phase; EXP: Experimental Phase; T: Transitions.
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: Overview of the Hera mission at the Didymos system.
Paper: The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Authors: Patrick Michel, Michael Küppers, Adriano Campo Bagatin, Benoit Carry, Sébastien Charnoz, Julia de Leon, Alan Fitzsimmons, Paulo Gordo, Simon F. Green, Alain Hérique, Martin Juzi, Özgür Karatekin, Tomas Kohout, Monica Lazzarin, Naomi Murdoch, Tatsuaki Okada, Ernesto Palomba, Petr Pravec, Colin Snodgrass, Paolo Tortora, Kleomenis Tsiganis, Stephan Ulamec, Jean-Baptiste Vincent, Kai Wünnemann, Yun Zhang, Sabina D. Raducan, Elisabetta Dotto, Nancy Chabot, Andy F. Cheng, Andy Rivkin, Olivier Barnouin, Carolyn Ernst, Angela Stickle, Derek C. Richardson, Cristina Thomas, Masahiko Arakawa, Hirdy Miyamoto, Akiko Nakamura, Seiji Sugita, Makoto Yoshikawa, Paul Abell, Erik Asphaug, Ronald-Louis Ballouz, William F. Bottke, Dante S. Lauretta, Kevin J. Walsh, Paolo Martino, Ian Carnelli
Figure caption: PALT optical box design.