adsabs/AstroCLIMB huggingface dataset:
Paper: Physical Characterization of Near-Earth Asteroid (52768) 1998 OR2: Evidence of Shock Darkening/Impact Melt
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Neil Pearson, Bryn Bowen
Figure caption: Telescopic VNIR spectrum of 1998 OR2 with laboratory spectra of Chergach, a shock-darkened H5 ordinary chondrite. All Chergach and 1998 OR2 spectra were continuum removed prior to mixing and comparisons. Chergach light and dark lithology spectra were obtained as endmembers and were mathematically mixed in different ratios to find the best match for 1998 OR2. The plotted gradient goes from pure dark lithology (darkest points) to pure light lithology (lightest points) in 10% increments. The best match for 1998 OR2 was found to be 63% dark lithology and 37% light lithology and is represented by the blue line.
Paper: Physical Characterization of Near-Earth Asteroid (52768) 1998 OR2: Evidence of Shock Darkening/Impact Melt
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Neil Pearson, Bryn Bowen
Figure caption: VNIR spectra (0.45–2.49 μm) of NEA (52768) 1998 OR2 shown with the average S- and Q-type spectra (left) and the Xn- and Ch-type spectra from the Bus–DeMeo taxonomy (right). Shaded regions show the standard deviation of the average spectrum.
Paper: Physical Characterization of Near-Earth Asteroid (52768) 1998 OR2: Evidence of Shock Darkening/Impact Melt
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Neil Pearson, Bryn Bowen
Figure caption: Lomb−Scargle periodogram of possible rotational periods for (52768) 1998 OR2. Two peaks of roughly equal power exist at 0.2855 and 0.2424 cycles hr−1, corresponding to periods of 3.503 and 4.126 hr, respectively.
Paper: Physical Characterization of Near-Earth Asteroid (52768) 1998 OR2: Evidence of Shock Darkening/Impact Melt
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Neil Pearson, Bryn Bowen
Figure caption: VNIR spectra of (52768) 1998 OR2 shown with the RELAB McKinney shock-darkened chondrite spectrum (RELAB c2mh01; Milliken 2020). The spectrum of 1998 OR2 was scaled to the median absolute albedo of the McKinney spectrum to match what was returned by M4AST.
Paper: Jupiter's Temperature Structure: A Reassessment of the Voyager Radio Occultation Measurements
Authors: Pranika Gupta, Sushil K. Atreya, Paul G. Steffes, Leigh N. Fletcher, Tristan Guillot, Michael D. Allison, Scott J. Bolton, Ravit Helled, Steven Levin, Cheng Li, Jonathan I. Lunine, Yamila Miguel, Glenn S. Orton, J. Hunter Waite, Paul Withers
Figure caption: Temperature profile of Jupiter derived from radio occultation observations by Voyager 1 ingress and egress and Voyager 2 egress. Data for Voyager 2 ingress are unavailable (see text).
Paper: Jupiter's Temperature Structure: A Reassessment of the Voyager Radio Occultation Measurements
Authors: Pranika Gupta, Sushil K. Atreya, Paul G. Steffes, Leigh N. Fletcher, Tristan Guillot, Michael D. Allison, Scott J. Bolton, Ravit Helled, Steven Levin, Cheng Li, Jonathan I. Lunine, Yamila Miguel, Glenn S. Orton, J. Hunter Waite, Paul Withers
Figure caption: Updated temperature profiles of Jupiter derived from radio occultation observations by the Voyager 1 ingress and egress and the Voyager 2 egress, together with the Galileo probe measurements. Data for the Voyager 2 ingress are unavailable (see text).
Paper: Jupiter's Temperature Structure: A Reassessment of the Voyager Radio Occultation Measurements
Authors: Pranika Gupta, Sushil K. Atreya, Paul G. Steffes, Leigh N. Fletcher, Tristan Guillot, Michael D. Allison, Scott J. Bolton, Ravit Helled, Steven Levin, Cheng Li, Jonathan I. Lunine, Yamila Miguel, Glenn S. Orton, J. Hunter Waite, Paul Withers
Figure caption: Comparison of Voyager 1 radio occultations (RSS) and IRIS retrieved temperatures. Ingress profiles are shown in red; egress profiles are shown in blue. The newly derived RSS profiles are solid lines, and the old versions are dotted lines. The profiles retrieved from IRIS zonally averaged spectra are shown as dashed (when the new T(p) was used as a prior) and dotted–dashed (when the old T(p) was used as a prior) lines. Uncertainties on the IRIS retrievals are shown as the gray lines in panel (b). Note how the IRIS retrievals converge in the 80–600 mb range, where they offer maximal constraint on the T(p), but diverge at higher pressures, where they are more strongly influenced by the choice of prior.
Paper: The Nature of Low-albedo Small Bodies from 3 μm Spectroscopy: One Group that Formed within the Ammonia Snow Line and One that Formed beyond It
Authors: Andrew S. Rivkin, Joshua P. Emery, Ellen S. Howell, Theodore Kareta, John W. Noonan, Matthew Richardson, Benjamin N. L. Sharkey, Amanda A. Sickafoose, Laura M. Woodney, Richard J. Cartwright, Sean Lindsay, Lucas T. Mcclure
Figure caption: BD–BD plot for ST and NST objects. Also shown are laboratory measurements of hydrated carbonaceous chondrites from Takir et al. (2013) and Bates et al. (2021). The NST and ST asteroids are largely separated from one another when plotted in this space, and the meteorites are found in areas where ST asteroids are more numerous. Two ST observations with artifacts near 3.2 μm are found in the NST area, but inspection and fits to BC confirm them as ST.
Paper: The Nature of Low-albedo Small Bodies from 3 μm Spectroscopy: One Group that Formed within the Ammonia Snow Line and One that Formed beyond It
Authors: Andrew S. Rivkin, Joshua P. Emery, Ellen S. Howell, Theodore Kareta, John W. Noonan, Matthew Richardson, Benjamin N. L. Sharkey, Amanda A. Sickafoose, Laura M. Woodney, Richard J. Cartwright, Sean Lindsay, Lucas T. Mcclure
Figure caption: Three NST asteroids compared to the Raponi et al. (2020) global average spectrum of comet 67P. The asteroids show an absorption band of similar depth and shape as the cometary spectrum, suggestive of similar compositions. The spectra are offset from one another for clarity.
Paper: The Nature of Low-albedo Small Bodies from 3 μm Spectroscopy: One Group that Formed within the Ammonia Snow Line and One that Formed beyond It
Authors: Andrew S. Rivkin, Joshua P. Emery, Ellen S. Howell, Theodore Kareta, John W. Noonan, Matthew Richardson, Benjamin N. L. Sharkey, Amanda A. Sickafoose, Laura M. Woodney, Richard J. Cartwright, Sean Lindsay, Lucas T. Mcclure
Figure caption: The KDEs for all of the asteroids in our sample (gray; left), as well as the ST (blue; center) and NST (red; right) groups separately. The two groupings of objects are clearly separated using this technique even when accounting for the errors on individual spectra.
Paper: The Nature of Low-albedo Small Bodies from 3 μm Spectroscopy: One Group that Formed within the Ammonia Snow Line and One that Formed beyond It
Authors: Andrew S. Rivkin, Joshua P. Emery, Ellen S. Howell, Theodore Kareta, John W. Noonan, Matthew Richardson, Benjamin N. L. Sharkey, Amanda A. Sickafoose, Laura M. Woodney, Richard J. Cartwright, Sean Lindsay, Lucas T. Mcclure
Figure caption: The 3 μm band shapes as seen in the new observations; (194) Prokne is an example of the ST (or Pallas-type) shape, (375) Ursula is the Themis-type shape, (10) Hygiea is the Ceres-type shape, and (596) Scheila is interpreted to have no band. Objects with BCs at wavelengths >3.0 μm are grouped as NSTs in this work. These spectra have had a linear continuum removed and are offset from one another for clarity.
Paper: Challenges in Forming Phobos and Deimos Directly from a Splitting of an Ancestral Single Moon
Authors: Ryuki Hyodo, Hidenori Genda, Ryosuke Sekiguchi, Gustavo Madeira, Sébastien Charnoz
Figure caption: Outcomes of collision between Phobos and Deimos. Masses of the largest remnant (M lr;  red points), the second-largest remnant (M slr;  blue points), and the debris ring (M ring = M tot − M lr − M slr where M tot = m Pho + m Dei; black points) as a function of impact velocity are shown. The red and blue horizontal dashed lines indicate the masses of Phobos and Deimos, respectively. The open circles are the results of N-body simulations (Leinhardt & Stewart 2012; the cases of the impactor-to-target mass ratio of γ = 0.1 and θ imp = 45°). The open squares are the results obtained from our SPH impact simulations. In our impact simulations, the masses of the target and the impactor are m Pho and m Dei, respectively. θ imp = 45° is used.
Paper: Challenges in Forming Phobos and Deimos Directly from a Splitting of an Ancestral Single Moon
Authors: Ryuki Hyodo, Hidenori Genda, Ryosuke Sekiguchi, Gustavo Madeira, Sébastien Charnoz
Figure caption: Initial distribution of e Dei and a Dei. Each black point shows the initial conditions of our numerical simulations (600 points). The left, middle, and right panels show cases of a Pho = 5.0, 5.5, and 6.0R Mars, respectively. We set e Pho = 0.15–0.35, e Dei = 0.0–0.2, and a Dei = 6.5–7.5R Mars, following Bagheri et al. (2021). a Dei is obtained from Equation (11) with e pho and e Dei randomly distributed within the ranges. The blue, green, and red curves indicate a Dei for e Pho = 0.15, 0.25, and 0.35, respectively.
Paper: Challenges in Forming Phobos and Deimos Directly from a Splitting of an Ancestral Single Moon
Authors: Ryuki Hyodo, Hidenori Genda, Ryosuke Sekiguchi, Gustavo Madeira, Sébastien Charnoz
Figure caption: Orbital elements, a and e, of the debris particles obtained by using the data of SPH simulations (top panels) and corresponding surface densities using the equivalent circular orbital radius, a eq (bottom panels). From left to right, cases of v imp = 100, 200, and 300 m s−1 are shown.
Paper: Challenges in Forming Phobos and Deimos Directly from a Splitting of an Ancestral Single Moon
Authors: Ryuki Hyodo, Hidenori Genda, Ryosuke Sekiguchi, Gustavo Madeira, Sébastien Charnoz
Figure caption: Cumulative distribution of the time taken to collide in years. Blue, green, and red lines represent cases of a Pho = 5.0, 5.5, and 6.0R Mars, respectively. Two distinct timescales of collisions are seen; t col ∼ 10−2–10−1 yr and t col ≳ 30 yr. Less than 10% of our runs at 1 × 104 yr still do not experience a collision between the moons.
Paper: Challenges in Forming Phobos and Deimos Directly from a Splitting of an Ancestral Single Moon
Authors: Ryuki Hyodo, Hidenori Genda, Ryosuke Sekiguchi, Gustavo Madeira, Sébastien Charnoz
Figure caption: Cumulative distributions of impact velocity (left) and impact angle (right) obtained from our numerical simulations. Blue, green, and red colors indicate a Pho = 5.0, 5.5, and 6.0R Mars, respectively. In the right panel, the black curve shows the cumulative of ﹩P({\theta }_{\mathrm{imp}})=\sin (2{\theta }_{\mathrm{imp}})﹩, which has a peak at θ imp = 45°.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: Sources of major axis orientation measurement errors include photon noise, angular measurements of square pixel data, and the subpixel positioning of the PSF on the pixel grid. Simulations of a point source show that the square pixels only significantly affect measurements at certain angles, and that subpixel PSF positioning has a negligible effect when the PSF FWHM is similar to typical PS1 imagery.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: The lines show the theoretical maximum possible host–companion angular separations (i.e., Hill radii) for representative S- and C-type asteroids located in the inner and outer main belt, observable at m  V  = 14–18 at opposition, corresponding to asteroid size. At the top are estimates of the number of main belt objects following the size–frequency power-law distribution from Ryan et al. (2015) and scaled to a total population of 1 million. The known binary asteroids show the different parameter spaces favored by each method of discovery. Better sampling in the direct imaging parameter space is needed to understand the real distribution of companion separations, which will provide constraints to main belt companion orbital stability and/or formation and evolution mechanisms.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: These figures show a simulated PS1 image (0.″26 pixel scale) and its corresponding cross section, of a binary object with a 1 mag contrast ratio, 1.″04 FWHM, and 0.″78 apparent separation. While the companion is not resolved, its presence is evident from the asymmetric elongation of the combined profile.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: Simulations show that it is possible to detect companions at low contrast ratios despite a stronger and brighter effect from nonsidereal trailing. Here the binary system has a contrast ratio of 1 mag, separation of 1.5 pixel (0.″39), and nonsidereal trailing of 2 pixels (0.″52); companion positioning at ±1 rad produces major axis orientation measurements of ±0.5 rad.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: Main belt binary asteroid separations and contrast ratio distributions produced from 137 companions detected by light curves and 28 companions resolved by direct imaging (Johnston 2019). Direct imaging is better able to explore the binary population where separations are greater than ∼0.1 Hill radius or contrast ratios are greater than ∼4 mag.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: In sidereal tracked observations, a binary asteroid’s PSF is a product of both its members and its nonsidereal rate over the exposure time. The direction of its ellipse major axis may deviate substantially from the known nonsidereal rate depending on the direction, separation, and brightness of the companion.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: The shape measurement technique requires that the nonsidereal trailing is neither too small nor too large; too short of a trail makes it difficult to differentiate anomalous measurements from those that can reasonably be attributed to noise, and trailing that is too long will dominate the measurements such that any anomalies cannot be the result of a real companion within the host’s Hill radius (left). The cross-track profiles are designed to minimize the effects of the trail, though there does appear to be a heightened sensitivity where the trails are longer (right).
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: The shape measurement technique appears to favor cases where the trailing angle is closely aligned with an image’s x-axis (left), with nearly complete insensitivity as the angle approaches the y-axis (left). Cross-track profiles do not appear to have such a bias (right).
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: Baseline hex-bin map showing the likelihood of a single asteroid resulting in the measured residual angle at the given nonsidereal trail length and observing conditions (here PSF amplitude = 5000 DN, FWHM = 1.″5). Measurements that fall in low likelihood bins are possible indicators of asteroid binarity. Mars-crossing asteroid 2577 Litva, which has a known companion that we expect to be able to detect, shows two such “hits.”
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: The cross-track profile of a target asteroid is created by collapsing its PSF in the direction of its nonsidereal motion (left) and is compared to a model profile created from the field stars in the same image, normalized to the same total brightness (right). The deviation between this simulated binary (1 mag contrast ratio) and the corresponding model profile is large and can be quantified with a goodness-of-fit statistic.
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: The effects of seeing are captured in the production of the hex-bin maps in the shape measurement technique, so sensitivity to potential companions falls off at greater seeing (left). However, the presented cross-track profile technique does not compensate for noise, which likely produces more false positives as seeing increases (right).
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: Similar to the effects of seeing, shape measurement sensitivity falls off as the targets become dimmer (left) due to its inclusion in the production of the hex-bin maps, whereas the cross-track profiles likely produce more false positives due to the increase in relative noise (right).
Paper: Searching for Binary Asteroids in Pan-STARRS1 Archival Images
Authors: James Ou, Christoph Baranec, Schelte J. Bus
Figure caption: This cross-track profile of asteroid 68299 is compared to the model profile created from field stars in the same image. The resulting χ 2 statistic is at the 95.1% quantile, contributing to the asteroid’s ranking as a binary candidate.
Paper: High Heat Flux near Miranda’s Inverness Corona Consistent with a Geologically Recent Heating Event
Authors: Chloe B. Beddingfield, Erin Leonard, Richard J. Cartwright, Catherine Elder, Tom A. Nordheim
Figure caption: (a) The DEM that we generated for this study from Voyager 2 ISS images. (b) Annotated and orthorectified version of a portion of Voyager 2 ISS image c2684629. (c) The location of profile lines used for this work. The location of a fault that cuts the profile line topography is shown (pink arrow). (d) The associated profile data across the profile lines shown in panel (c) (black data points) and a flexural model fitting these data (blue line). A small fault, shown by the pink arrow in panel (c), cuts across the flexed portion of the terrain, causing a small section of overprinting small-scale topography in the profile lines that is unrelated to the topography associated with flexure. The topography associated with this fault was removed from the profile lines (gap in black data points). The topography of the three profile lines is available as the data behind the figure.(The data used to create this figure are available.)
Paper: High Heat Flux near Miranda’s Inverness Corona Consistent with a Geologically Recent Heating Event
Authors: Chloe B. Beddingfield, Erin Leonard, Richard J. Cartwright, Catherine Elder, Tom A. Nordheim
Figure caption: (a) Combination of Voyager 2 ISS images c2684620 (top section, 270 m px−1), c2684629 (middle section, 237 m px−1), and c2684617 (bottom section, 284 m px−1) showing parts of Inverness and Elsinore Coronae, the Cratered Terrain, Verona Rupes, Argier Rupes, and the location of our study area (blue star). (b) ISS image mosaic of Miranda's southern hemisphere showing the location of Miranda's three known coronae and the region covered by the DEM generated for this work. The study locations for this work and previous work (Beddingfield et al. 2015a) are also shown.
Paper: High Heat Flux near Miranda’s Inverness Corona Consistent with a Geologically Recent Heating Event
Authors: Chloe B. Beddingfield, Erin Leonard, Richard J. Cartwright, Catherine Elder, Tom A. Nordheim
Figure caption: (a) Estimated elastic thickness on Miranda. (b) Estimated heat fluxes on Miranda assuming a porosity of 0%. (c) Estimated heat fluxes assuming a pure H2O lithospheric composition and porosities ranging from 5%–25%. (d) Estimated heat fluxes assuming an H2O ice lithosphere with small amounts of NH3-hydrates and porosities ranging from 5%–25%. See Table 3 in Appendix A.2 for the full set of estimated values as a table.
Paper: High Heat Flux near Miranda’s Inverness Corona Consistent with a Geologically Recent Heating Event
Authors: Chloe B. Beddingfield, Erin Leonard, Richard J. Cartwright, Catherine Elder, Tom A. Nordheim
Figure caption: Ranges of estimated heat fluxes for icy bodies throughout the solar system, assuming pure H2O ice lithospheres. See Table 2 for ranges of estimated heat fluxes and references.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: The setup of the ICE. Left: overall view of the vacuum chamber (1) and drop mechanism (2). Top and center right: view of the target area, with the empty sample cup (copper) and the ejecta collection plate (3). The arrows point to three (of eight) etched concentric circles used for mass measurements. Bottom right: detailed view of the empty sample cup (4) in its cooling copper block (5). The sample temperature is measured using two thermocouples, one close to the surface of the filled cup and one at half height.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Size distribution of the water ice grains prepared for the ICE impacts. The inset shows a microscope picture of a 75% dust–ice mixture used as target material.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: The ICE data collected. Left: time-lapse images of an impact of the glass projectile into frosted regolith (5.6.15.0 in Table 3). The evolution of the ejecta plume in two dimensions can be followed thanks to the laser sheet illumination. Right: crater pictures of the same impact after venting and opening the vacuum chamber.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Examples of the craters produced during our investigation. (a) Impact 10.18.16.3; glass projectile dropped from a height of 45 cm into dry regolith. In these kinds of impacts, the projectile did not embed itself into the target. For the crater depth measurements, it was removed from the crater (see panel (e)). (b) Impact 10.18.16.0; glass from 50 cm into dry regolith. Here, the projectile partially embedded itself into the target. We left it in place to measure the crater characteristics, so as to modify the crater as little as possible after impact. (c) Impact 10.18.16.1; Teflon from 50 cm into dry regolith. (d) Impact 10.18.16.2; brass from 50 cm into dry regolith. (e) Impact 3.24.15.0; brass from 45 cm into frosted regolith (5% volume water ice). The projectile was removed after impact. (f) The same impact as (e), with the crater rim marked in yellow and the measured lengths b and b 1 used for the crater depth measurements. The sample cup is measured in red and used in each picture to determine the pixel size. The top pictures were used for the crater size measurements, and the side pictures were used for the crater depth measurements. (g) Impact 6.16.16.0; brass from 45 cm into 50% volume water ice mixture. The projectile is partially buried in the target. (h) The same impact as panel (g), with crater size and depth measurement markings. For the crater depth measurements when the projectile was partially embedded, the slopes of the crater were extended to intersect. The point of intersection was chosen as the crater depth.