adsabs/AstroCLIMB huggingface dataset:
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: Hera spacecraft design. The locations of the different payload elements are indicated (AFC = Asteroid Framing Cameras; TIRI = Thermal InfraRed Imager; PALT = Planetary ALTimeter; SMC = Small Monitoring Cameras).
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: The Juventas small platform with the four JuRa antenna booms as deployed for JuRa operations (courtesy of GomSpace Luxembourg Sarl).
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: Schematic showing the wavelength coverage by the filters on Hyperscout-H. Also shown are average spectra of S-type and C-type asteroids.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Comparison between models (125 m pix−1) and MDIS broadband image EW1020581108B (188 m pix−1) in stereographic projection with the origin at the north pole and 0° longitude to the bottom. (a) Simulated image using the MLA+SfS DEM; (b) MDIS image; (c) MDIS image with contours: PSR (magenta), ice stability depth of 0 m (cyan), MDIS-bright boundary (yellow), ice stability depth of 1 m (white), and radar-bright region (red); (d) hill shade of the MLA+SfS DEM with the same contours and black lines defining the inner and outer edges of the floor region used to select MLA reflectance footprints (blue points) for the mixture modeling in Section 3.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: High-resolution polar stereographic models of Prokofiev at 125 m pix−1 with the origin at the north pole and 0° longitude to the bottom. (a) Colorized hill shade of MLA+SfS DEM. (b) Average illumination over one Mercury solar day. Dark blue regions are PSRs. (c) Maximum surface temperature throughout a Mercury solar day. (d) Depth below the surface needed for the long-term stability of ice. Dark blue regions are areas where ice is thermally stable at the surface. Dark red areas are where no ice is stable within the upper 2.5 m, and generally, therefore, where ice is unstable at any depth.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Distribution of MLA reflectance for (1) Prokofiev’s floor outside both the MDIS-bright region and PSRs (“non-MDIS-bright, non-PSR,” orange), (2) Prokofiev’s floor inside the MDIS-bright region but outside PSRs (“MDIS-bright, non-PSR,” black), (3) Prokofiev’s floor PSRs (“PSR,” cyan), (4) a nearby control sample outside Prokofiev (“nearby Prokofiev,” red), and (5) the eight H20 dark deposit PSRs (“dark deposit,” blue). Each histogram has a bin size of 0.05 and is normalized by its total number of points. The error bars are Poisson errors.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Two-dimensional histograms of MLA reflectance as a function of pulse width (left), range (middle), and emission angle (right) for latitudes 55°–83°. The color scale gives the fraction of the number of points in each column of each histogram. The y-axis bin size is 0.02 and the x-axis bin size is 1 ns, 10 km, and 1°. The dashed white lines show the adopted thresholds used for extracting good data: pulse width = 15–90 ns, range = 100–800 km, and emission angle <20°. The middle and right panels have had the pulse width and pulse width + range cuts applied, respectively.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Best-fit values (solid dots) for the ice-bearing footprint fraction, F  i , and subfootprint ice areal fraction, f  i , with their respective 1, 2, and 3σ uncertainty contours (innermost to outermost). Two models are shown assuming that the dark end-member’s reflectance distribution is the same as that of (1) Prokofiev’s floor outside the MDIS-bright region and PSRs (“Prokofiev non-MDIS-bright, non-PSR”; orange lines), or (2) the eight H20 dark deposits hypothesized to be sublimation lags of complex organics (“dark deposit”; blue lines). In both models, f  i  < 1 at high confidence, meaning pure ice is strongly disfavored.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Effect of varying the mixture model parameters: (a) ice-bearing footprint fraction F  i , (b) subfootprint ice fraction f  i , (c) mean ice reflectance r  i , and (d) ice reflectance spread σ  i . These models use the non-MDIS-bright, non-PSR distribution (orange line) as the dark, non-icy end-member for fitting the PSR distribution (cyan line).
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: Best-fit linear mixture models (dashed lines) using (1) the non-MDIS-bright, non-PSR distribution (orange) and (2) dark deposit (blue) as the non-icy end-member to fit the observed PSR distribution (cyan). In both best-fit models, all MLA footprints are ice-bearing (F  i  = 1.00) while the subfootprint ice fraction is (1) f  i  = 0.33 and (2) f  i  = 0.44.
Paper: New Constraints on the Volatile Deposit in Mercury’s North Polar Crater, Prokofiev
Authors: Michael K. Barker, Nancy L. Chabot, Erwan Mazarico, Matthew A. Siegler, Jose M. Martinez-Camacho, Colin D. Hamill, Stefano Bertone
Figure caption: MLA altimetry (blue points) and best-fit median radial profile and interquartile range (orange lines). The red points are the radar-bright MLA footprints.
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: Original velocity distribution for the considered impact simulation from Raducan et al. (2019), truncated at 1 m s−1. The histogram shows the number of objects relative to the total of 11,593 particles within each bin of 1 cm s−1.
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: Error in the NFT's time of touch estimate over the post-Checkpoint images.
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: Comparison between the full polyhedron approach and the patched polyhedron–MacCullagh approach. In the left panel, we illustrate with a black line the initial evolution with time, just after the ejection from the surface, of the distance from Dimorphos computed with the polyhedron model. The negative time is adopted to mark at time zero the moment of patching. The continuation of the polyhedron solution (magenta line) is then compared with MacCullagh’s solution (green line) at subsequent times. The difference between the two solutions is shown in the right panel.
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: A correlation example where the source of the error is less clear. As in Figure 21, but for image 18 and feature 39. Note that the correlation surface peak is shifted down and left in the right panel, as is the matched location in the left panel. The rendering also has higher contrast than the image.
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: Targeted touch location, expected touch location at the time of Checkpoint, and actual touch location. The locations are displayed on NFT image 30.
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: Potential touch location dispersion based on uncertainties in maneuver execution performance and Checkpoint state estimate. Blue ellipses represent 1σ and 3σ dispersion due to Checkpoint state estimate error, and orange and red ellipses represent 1σ and 3σ dispersions due to maneuver execution 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: Targeted touch location, NFT's final estimated touch location, and actual touch location. The locations are displayed on NFT image 30.
Paper: ExoCAM: A 3D Climate Model for Exoplanet Atmospheres
Authors: Eric T. Wolf, Ravi Kopparapu, Jacob Haqq-Misra, Thomas J. Fauchez
Figure caption: Here we show the spectral outgoing longwave radiation compared between line-by-line calculations with SMART, high-resolution band model calculations with SOCRATES, and n68equiv. We assumed a 2 bar CO2 atmosphere with a 250 K surface temperature, and no other absorbing species. SOCRATES and n68equiv are similar, while the SMART calculations, originally appearing in Kopparapu et al. (2013), feature stronger absorption. The differences in the total absorption strength are likely due to the line wing treatments (Perrin & Hartmann 1989; Meadows & Crisp 1996).
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 surface temperature is plotted against the global mean emission temperature of the atmosphere. 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: Here we show the outgoing longwave radiation and the downwelling stellar flux at the surface compared between the line-by-line calculations from SMART, LBLRTM, and our most recently updated radiative transfer version, n68equiv. The top row shows the flux results, while the bottom row shows the differences between n68equiv and each line-by-line model, respectively. We follow the procedures of Yang et al. (2016) and examine atmospheres that have surface temperatures according to the x-axis, with 1 bar N2, 376 ppm CO2, and that are saturated with water vapor. Our n68equiv version compares favorably against the line-by-line results, and marks a significant improvement over previous versions of ExoRT.
Paper: ExoCAM: A 3D Climate Model for Exoplanet Atmospheres
Authors: Eric T. Wolf, Ravi Kopparapu, Jacob Haqq-Misra, Thomas J. Fauchez
Figure caption: Contour plots showing surface temperature, OLR, 500 mb vector winds, liquid cloud water, and ice cloud water for the hab1 (left) and hab2 (right) simulations, respectively.
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 liquid 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 column planetary albedo is plotted against the global mean planetary emissivity. The control simulation is indicated by the orange cross. Sensitivity tests are indicated by the blue diamonds, with significant outliers labeled.
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 2021 March 6. See the caption of Figure 1 for a description of the content of the panels.
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 2021 February 17. See the caption of Figure 1 for a description of the content of the panels.
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 2021 January 20. See the caption of Figure 1 for a description of the content of the panels.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Rotational NIR spectra of JD1 obtained from LDT at Happy Jack, Arizona. The spectra have been organized from the beginning (first spectrum obtained at 01:39:32 UT on 2019 November 1) to the end of the observation from top to bottom and left to right. Each spectrum has been normalized to unity at 1 μm plus an offset added in the reflectance for clarity. Gray shaded areas indicate wavelengths of telluric absorption. The numbers at the end of each spectrum (around 2.2 μm) indicate the time in hours at which the spectrum was obtained after the first scan. Red numbers refer to those spectra that appear red (positive slope), while blue ones refer to those that look blue (negative slope). The raw and calibration data for these rotational NIR spectra are available as data behind the figure.(The data used to create this figure are available.)
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Doppler-only echo power spectra of JD1 from 2019 November 1–3 using the Arecibo S-band planetary radar system. Echo strength in both the OC (solid line) and SC (dashed line) polarization as transmitted is shown. The echo power on the Y-axis is measured in standard deviations of the background noise. The effective frequency resolution (Δf) is smoothed to 0.05/0.06 Hz. Over the 3 days of observations, diffuse scattering dominates the reflection.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: The SDSS g- (green dots) and r-band (red dots) filter light curves of JD1 as a function of time since the beginning of the observation obtained using the LMI at LDT. These single-peaked light curves show half of JD1's bimodal light curve, shown in cyan dots, from Warner & Stephens (2020). The gap in the LDT data between 1.3 and 1.7 hr corresponds to the observation of the standard star. The g and r light curves are available as data behind the figure, and the raw photometry data are made available on FigShare: https://doi.org/10.6084/m9.figshare.20137265.v1.(The data used to create this figure are available.)
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Left: track of JD1's rotational phase angle 0°, defined as the orientation of the first LDT spectra obtained at 01:39:32.37 UTC on November 1, as a function of days (gray filled circles). The yellow star indicates the time of observing the blue spectra at LDT. The cyan and magenta diamonds illustrate the LCO observations. Right: phase range of each observation per day of the observation. The blue shaded area illustrates the phase range of the blue NIR spectra at LDT. The black line shows the range of the LDT observation, while the diamonds represent each LCO observation in the corresponding phase. The measurement uncertainties are shown in the text.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Visible spectra obtained at Haleakala Observatory, Kula, Hawaii, and Siding Springs, Australia, from LCO. Blue and red lines are the visible spectra obtained on 2019 November 7 and November 21, respectively. Both spectra have been normalized to unity at 0.55 μm. The raw and calibration data for these visible spectra are available as data behind the figure.(The data used to create this figure are available.)
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: Rendering of the ASPECT hyperspectral imager with its four independent channels and data processing unit (DPU; green).