adsabs/AstroCLIMB huggingface dataset:
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Momentum enhancement, β (from Raducan et al. 2023) and the catastrophic disruption threshold, ﹩{Q}_{D}^{* }﹩ (this study) for Dimorphos-sized ellipsoidal targets, with boulder packing between 0 vol% and 50%. β is calculated from numerical simulations using the DART impact conditions (580 kg at 6 km s−1) (Raducan et al. 2023). The observed change in the orbital period of Dimorphos, of ≈33 minutes (Thomas et al. 2023), corresponds to β = 2.2–4.9, depending on the mass of the asteroid, which is still uncertain.
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Fraction of ejected material as a function of specific impact energy (Q  r ), for 6 km s−1 impacts into ≈150 m rubble-pile asteroids with varying boulder packing (0%–50%). The intersection between the trend through the simulation data (denoted by the dashed lines) and the 50% fraction ejected (denoted by the dotted lines) gives the ﹩{Q}_{D}^{* }﹩ for the specific target.
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Same as in Figure 5 but for 45°, 6 km s−1 impacts into ≈50 m rubble-pile asteroids with varying boulder packing (0%–50%).
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Same as in Figure 5 but for oblique (45°), 6 km s−1 impacts into ≈150 m rubble-pile asteroids with varying boulder packing (0%–50%).
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Same as in Figure 5 but for oblique (45°), 6 km s−1 impacts into ≈100 m rubble-pile asteroids with varying boulder packing (0%–50%).
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Same as in Figure 5 but for vertical, 6 km s−1 impacts into ≈50 m rubble-pile asteroids with varying boulder packing (0%–50%).
Paper: Lessons Learned from NASA’s DART Impact about Disrupting Rubble-pile Asteroids
Authors: S. D. Raducan, M. Jutzi, C. C. Merrill, P. Michel, Y. Zhang, M. Hirabayashi, A. Mainzer
Figure caption: Same as in Figure 5 but for vertical, 6 km s−1 impacts into ≈110 m rubble-pile asteroids with varying boulder packing (0%–50%).
Paper: Pwyll and Manannán Craters as a Laboratory for Constraining Irradiation Timescales on Europa
Authors: M. Ryleigh Davis, Michael E. Brown
Figure caption: Average spectra of Pwyll crater, its dark proximal ejecta, bright ray ejecta, and the nearby surrounding terrain along with their best-fit spectral models. The NIMS pixels included in the average spectra are shown in the inset map with the crater interior in red, the dark proximal ejecta in orange, the bright ray ejecta in blue, and the older background terrain in green. A laboratory-derived spectrum of pure water ice with 200 μm grains from Mastrapa et al. (2008) is also included for comparison. For clarity, the spectra are offset by +0.0, +0.1, +0.2, +0.3, and +0.4, respectively.
Paper: Pwyll and Manannán Craters as a Laboratory for Constraining Irradiation Timescales on Europa
Authors: M. Ryleigh Davis, Michael E. Brown
Figure caption: Average spectra and best-fit spectral models of Manannán crater and its dark proximal ejecta, bright ray ejecta, and the nearby surrounding terrain along with Belus linea. The NIMS pixels included in the average spectra are shown in the inset map with the crater interior and dark proximal ejecta in orange, the bright ray ejecta in blue, the older background terrain in green, and Belus linea in purple. For clarity, the spectra are offset by +0.0, +0.1, +0.2, and +0.3, respectively.
Paper: Pwyll and Manannán Craters as a Laboratory for Constraining Irradiation Timescales on Europa
Authors: M. Ryleigh Davis, Michael E. Brown
Figure caption: Global mosaic of Europa showing the locations of Pwyll and Manannán craters. Pwyll crater, one of Europa’s youngest impact features, is ∼27 km in diameter, surrounded by a dark ring of proximal ejecta, and has an extensive bright ray ejecta which extends as far as 1000 km and stands in stark contrast to the darker reddish surface of Europa’s trailing hemisphere. Manannán crater is ∼23 km in diameter, also has a dark, red ring of proximal ejecta, and is surrounded by a much less extensive bright ray system which extends up to ∼120 km and covers nearby young terrain, including chaos terrains in Dyfed Regio and the triple band Belus linea. The location of the trailing hemisphere apex (0◦  N, 270◦  W) is indicated with a star. This mosaic map, created by Steve Albers, blends an existing color map from NASA/JPL/Björn Jónsson created using color images from Voyager and Galileo, the high-resolution black and white mosaic from USGS, and additional higher-resolution imagery from Galileo and Juno.
Paper: Pwyll and Manannán Craters as a Laboratory for Constraining Irradiation Timescales on Europa
Authors: M. Ryleigh Davis, Michael E. Brown
Figure caption: (a) Enhanced color image constructed from Galileo/Solid State Imager (SSI) images of Pwyll crater and the surrounding regions on Europa’s trailing hemisphere. The dark, red crater and proximal ejecta are seen near the center of the image surrounded by an extensive bright ejecta blanket with rays extending over a thousand kilometers from the impact site. This bright ice-rich ejecta stands in stark contrast to the darker, reddish surface of Europa’s trailing hemisphere. This image is from NASA/JPL/University of Arizona. (b) Galileo/SSI image of Pwyll crater, taken with the clear filter. This image is from NASA/JPL/DLR. (c) Galileo/SSI image of Manannán crater, taken with the clear filter. This image is from NASA/JPL/DLR. In all three panels, north is toward the top of the image. For panels (b) and (c), the Sun illuminates the surface from the right.
Paper: DART Impact Ejecta Plume Evolution: Implications for Dimorphos
Authors: Andrew F. Cheng, S. D. Raducan, M. Jutzi, T. L. Farnham, E. Dotto, V. Della Corte, E. Mazzotta Epifani, A. Rossi, I. Gai, J. Deshapriya, P. Hasselmann, I. Bertini, A. Zinzi, S. Ivanovski, J. Brucato, Giovanni Poggiali, A. Lucchetti, M. Pajola, G. Zanotti, M. Amoroso, A. Capannolo, G. Cremonese, M. Dall'Ora, S. Ieva, G. Impresario, M. Lavagna, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, P. Tortora, M. Zannoni
Figure caption: Cumulative mass ﹩{{\boldsymbol{M}}}_{{\bf{ej}}}\left({\boldsymbol{v}}\right)﹩ ejected above velocity  v , for four target cases with strength from 5 Pa to 5 kPa. The ejecta cumulative mass curves for these cases appear in order of increasing strength from top to bottom at the lowest velocities under 1 m s−1. That is, ﹩{{\boldsymbol{M}}}_{{\bf{ej}}}\left({\boldsymbol{v}}\right)﹩ is greatest for the lowest target strength case and least for the highest-strength case. The total ejected mass is similarly greatest for the lowest-strength case.
Paper: DART Impact Ejecta Plume Evolution: Implications for Dimorphos
Authors: Andrew F. Cheng, S. D. Raducan, M. Jutzi, T. L. Farnham, E. Dotto, V. Della Corte, E. Mazzotta Epifani, A. Rossi, I. Gai, J. Deshapriya, P. Hasselmann, I. Bertini, A. Zinzi, S. Ivanovski, J. Brucato, Giovanni Poggiali, A. Lucchetti, M. Pajola, G. Zanotti, M. Amoroso, A. Capannolo, G. Cremonese, M. Dall'Ora, S. Ieva, G. Impresario, M. Lavagna, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, P. Tortora, M. Zannoni
Figure caption: Extinction optical depth profiles for 500 and 5000 Pa target cases, at image times T+158 s and T+175 s. Image resolutions are indicated. Top row: profiles for the 500 Pa case at T+158 s and T+175 s. Bottom row: profiles for the 5000 Pa case at T+158 s and T+175 s. The peak optical depth value is greatest at z0 = 0 and takes lower values for larger z0.
Paper: DART Impact Ejecta Plume Evolution: Implications for Dimorphos
Authors: Andrew F. Cheng, S. D. Raducan, M. Jutzi, T. L. Farnham, E. Dotto, V. Della Corte, E. Mazzotta Epifani, A. Rossi, I. Gai, J. Deshapriya, P. Hasselmann, I. Bertini, A. Zinzi, S. Ivanovski, J. Brucato, Giovanni Poggiali, A. Lucchetti, M. Pajola, G. Zanotti, M. Amoroso, A. Capannolo, G. Cremonese, M. Dall'Ora, S. Ieva, G. Impresario, M. Lavagna, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, P. Tortora, M. Zannoni
Figure caption: Extinction optical depth profiles for 5 and 50 Pa target cases, at image times T+158 s and T+175 s. Image resolutions are indicated. The plume optical depth model is symmetric in z. Top row: profiles for the 5 Pa case at T+158 s and T+175 s. Bottom row: profiles for the 50 Pa case at the same two times. The peak optical depth value is greatest at z0 = 0 and takes lower values for larger z0.
Paper: DART Impact Ejecta Plume Evolution: Implications for Dimorphos
Authors: Andrew F. Cheng, S. D. Raducan, M. Jutzi, T. L. Farnham, E. Dotto, V. Della Corte, E. Mazzotta Epifani, A. Rossi, I. Gai, J. Deshapriya, P. Hasselmann, I. Bertini, A. Zinzi, S. Ivanovski, J. Brucato, Giovanni Poggiali, A. Lucchetti, M. Pajola, G. Zanotti, M. Amoroso, A. Capannolo, G. Cremonese, M. Dall'Ora, S. Ieva, G. Impresario, M. Lavagna, D. Modenini, P. Palumbo, D. Perna, S. Pirrotta, P. Tortora, M. Zannoni
Figure caption: Cumulative distributions of ejected mass M ej(>v) vs. velocity v, where M ej(>v) is scaled by projectile mass and v is scaled by impact velocity. Orange and blue curves show Bern SPH simulations with target cohesion Y 0 = 5 Pa and 50 Pa, respectively. The dashed curve shows point-source scaling relations at cratering strength Y = 5 Pa.
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Laser interferometry. (a) Intensities of lasers vs. elapsed time of deposition. The two blue lasers at θ 1 = 3.°7 (top black line) and θ 2 = 45.°2 (bottom black line) have more fringes and deeper fringes compared to a red laser at near-normal incidence to the sample surface (dashed black line). (b) Intensities of two blue lasers vs. fraction of full deposition allow us to remove the effects of a variable deposition rate. Original laser signals shifted by one period (dashed black lines) enable us to determine the periods of the laser signals.
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Comparison between our k-values (gray lines) and Grundy et al. (2002) k-values (dashed black lines) for CH4 at 30 K. (a) The ν 2 + ν 3 band at 4530 cm−1. (b) The ν 3 + ν 4 band at 4303 cm−1 and the ν 1 + ν 4 band at 4203 cm−1. (c) The 3ν 4 band at 3846 cm−1.
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Comparison between our k-values (gray lines) and Gerakines & Hudson (2020a) k-values (dashed black lines) for CH4 at 30 K. (a) The ν 3 band at 3011 cm−1. (b) The ν 4 band at 1300 cm−1.
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Imaginary part of the optical constants, k, as a function of wavenumber and wavelength for crystalline H2O at 50 K from this work (gray line) and Mastrapa et al. (2008; dashed black line). Shown are the 3350 cm−1 (2.99 μm) ν 3 LO mode, the 3200 cm−1 (3.1 μm) ν 3 TO mode, and the 3100 cm−1 (3.2 μm) ν 1 mode.
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Imaginary part of the optical constants, k, as a function of wavenumber and wavelength for the 3350 cm−1 (2.99 μm) ν 3 LO mode, the 3200 cm−1 (3.1 μm) ν 3 TO mode, and the 3100 cm−1 (3.2 μm) ν 1 mode of crystalline H2O at 150 K (dashed black line), 100 K (gray line), and 50 K (black line).
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Quantities in the reflection model and the path of light from the FTIR, through the sample, and onto the detector.
Paper: Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy
Authors: S. C. Tegler, W. M. Grundy, M. J. Loeffler, P. D. Tribbett, J. Hanley, A. V. Jasko, H. Dawson, A. N. Morgan, K. J. Koga, A. O. Madden-Watson, M. D. Gomez, J. K. Steckloff, G. E. Lindberg, S. P. Tan, S. M. Raposa, A. E. Engle, C. L. Thieberger, D. E. Trilling
Figure caption: Comparison between experimental absorbance (dashed black line) and model (gray line) for the CH4 ν 3 band at 3011 cm−1.
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Top left: spectrum of Iris from the IRSA archive (gray) compared to solar spectrum (yellow). The black line shows the solar-corrected spectrum of Iris found by subtracting the yellow spectrum from the gray spectrum. Top right: emissivity spectrum found by fitting the thermal spectrum only. The tail <6.5 μm is still present, suggesting that reflected sunlight is not the culprit. Bottom: comparison of the spectra of Iris resulting from the two methods of continuum removal explained in Sections 3.1 (blue) and 3.2 (yellow). The shaded colored region indicates ± 1σ. Both spectra are right at the edge of 1σ from the other.
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Left: comparison of a spectrum of Massalia before (red) and after (blue) correction of atmospheric transmission (gray). Right: continuum-removed flux found by fitting a 2D polynomial to the red and blue spectra in the left panel and dividing it out. The continuum-removed spectra are unitless, as they have been normalized. The gray spectrum of atmospheric transmission has units of transmittance. After removing a spurious feature at 6.02 μm that is actually due to the atmosphere (gray arrow), a clear peak at 6.04 μm is visible (blue arrow).
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Left: scaled flux for each asteroid (colors) compared to the best-fit NEATM (black). Right: emissivity of each asteroid found by dividing observed flux by modeled flux. The shaded colored region indicates ±1σ. The gray shaded region indicates atmospheric absorption where transmission is <80% and emissivity is unreliable.
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Left: region of the spectrum used for continuum removal. The gray circles show the points used in the polynomial fit (5.65–6.5 μm). The polynomial fit excludes 5.9–6.25 μm. Right: continuum-removed emissivity for each asteroid. The shaded colored region indicates ±1σ. Iris and Massalia show prominent features near 6 μm (black arrows). Parthenope and Melpomene are too noisy to confidently identify a 6 μm feature.
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Alternative method for removing the continuum flux. A 2D polynomial (black, left) was fit to the asteroid flux (colors, left) between 5.0 and 7.6 μm and divided out, leaving continuum-removed flux (right). The 6 μm feature is still present in the spectra of Iris and Massalia using this method. The shaded colored region indicates ±1σ.
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Output of the SOFIA processing pipeline showing how the spectrum changes with varying PWV values. Shown is Iris spectrum 0144 from flight 816.
Paper: Detection of Molecular H2O on Nominally Anhydrous Asteroids
Authors: Anicia Arredondo, Margaret M. McAdam, Casey I. Honniball, Tracy M. Becker, Joshua P. Emery, Andrew S. Rivkin, Driss Takir, Cristina A. Thomas
Figure caption: Gaussian fits to the Iris and Massalia spectra cropped from 5.9 to 6.15 μm. Band center is the mean of the fit. The dashed gray horizontal line indicates the FWHM.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Frequency of boulders impacting on Didymos and Dimorphos vs. time.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: The black dots represent the positions of the modeled boulders on the sky plane after 800 days of orbital evolution for the ejection parameters of Table 1. The small red open circles are the positions of the boulders observed by J+23 on 2022 December 19, i.e., 83 days after impact. The inset displays a zoomed region 140 × 140 km2 around Didymos's position, showing the location of the modeled boulders (black open circles) within or near the Hill radius. North is up and east to the left in both panels.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Left panel: distribution of the radius of the boulders that remain in orbit after 1550 days of integration. Right panel: distribution of initial velocities of those surviving boulders.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Ejection speeds as a function of the impact time of the modeled boulders on Didymos and Dimorphos.
Paper: On the Fate of Slow Boulders Ejected after DART Impact on Dimorphos
Authors: Fernando Moreno, Gonzalo Tancredi, Adriano Campo Bagatin
Figure caption: Escape speeds (speeds calculated at 200 km from Didymos) of the boulders ejected (filled circles; left axis). The blue line (right axis) shows the heliocentric distance of Didymos. A clear anticorrelation between escape speeds and heliocentric distance is noticed.
Paper: Increasing the Usability and Accessibility of Voyager 2 Images of Triton
Authors: Michael T. Bland, Emily S. Martin, Alex Patthoff
Figure caption: Examples of Triton’s surface morphology, which is dissimilar from the other ice-covered moons in the outer solar system. (a) Broad double ridges, similar to those on Europa but of much greater size, cross portions of the “cantaloupe terrain.” (Image center 342° E, 25° N.) (b) Darker smooth terrain transitions to bright frost-covered terrain near the southern pole. Several macula (dark spots) in the bright terrain mark the locations of plume deposits. (Image center 27° E, 17° S.) (c) Extensive smooth planitia (plains) disrupt the cantaloupe terrain. A few small craters are notable in their sparsity. (Image center 23° E, 21° N.) Each panel is a portion of our Triton mosaic, which is in orthographic projection at a scale of 600 m pixel−1.
Paper: The Sensitivity of NEO Surveyor to Low-perihelion Asteroids
Authors: Joseph R. Masiero, Yuna G. Kwon, Dar W. Dahlen, Frank J. Masci, Amy K. Mainzer
Figure caption: Cumulative size-frequency distribution (q, gray line) of expected breakup distribution resulting in 2005 UD as the largest fragment (red diamond). Overplotted are cometary fragment distributions determined by Reach et al. (2009; blue triangles) and Steckloff & Jacobson (2016; black circles) for analogous situations.
Paper: The Sensitivity of NEO Surveyor to Low-perihelion Asteroids
Authors: Joseph R. Masiero, Yuna G. Kwon, Dar W. Dahlen, Frank J. Masci, Amy K. Mainzer
Figure caption: Cumulative size-frequency distribution of the objects present today in the hypothesized Phaethon–Geminid Complex formed from the breakup of a proto-Phaethon object (black x’s) and the subpopulation that would be expected to be detected and cataloged by NEO Surveyor (red circles), under the assumption that the largest fragment of the breakup is (155140) 2005 UD. NEO Surveyor will be approximately complete to D ∼ 200 m, and would detect ∼40 members of this population.
Paper: Uranus Orbiter and Probe: A Radio Science Investigation to Determine the Planet’s Gravity Field, Depth of the Winds, and Tidal Deformations
Authors: Marzia Parisi, A. James Friedson, Chris R. Mankovich, Mark D. Hofstadter, Alex B. Akins, Reza Karimi, Damon F. Landau
Figure caption: Estimation results for Uranus’s k 22. Each error bar corresponds to one of the four subcases. Purple, green, and orange bars correspond to Trajectory 1, 2, and 3 subcases, respectively.
Paper: Uranus Orbiter and Probe: A Radio Science Investigation to Determine the Planet’s Gravity Field, Depth of the Winds, and Tidal Deformations
Authors: Marzia Parisi, A. James Friedson, Chris R. Mankovich, Mark D. Hofstadter, Alex B. Akins, Reza Karimi, Damon F. Landau
Figure caption: Estimation results for Uranus’s static zonal harmonics, degree 2–10. Each panel corresponds to one of the four subcases.
Paper: Uranus Orbiter and Probe: A Radio Science Investigation to Determine the Planet’s Gravity Field, Depth of the Winds, and Tidal Deformations
Authors: Marzia Parisi, A. James Friedson, Chris R. Mankovich, Mark D. Hofstadter, Alex B. Akins, Reza Karimi, Damon F. Landau
Figure caption: Estimation results for Uranus’s static zonal harmonics. The uncertainty curves are specific to one of the Trajectory 3 subcases: no occultations and Saturn-like normal mode amplitudes (NO OCC SAT-LIKE).