adsabs/AstroCLIMB huggingface dataset:
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: Comparison between the ground-based entry point (“Fireball”), the telescopic-only solution (“Astrometry”), and the combined solution (“Joint”) at a reference height of 95.455 km. The footprint ellipses represent 3σ errors. The telescopically estimated ellipses are oriented in the direction of trajectory propagation, with the telescopic-only solution having a major/minor 1σ length of 0.609/0.024 km and the combined solution of 0.107/0.014 km.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: Left: measured fireball lightcurve as a function of height from the Caistor camera (blue crosses) as compared to the total light production estimated from the semiempirical model (solid black line). The individual lightcurves for eroding fragments (green dashed line), dust (red dashed line), and dust released from eroding fragments (purple dashed line) are also shown. The modeled light production from the ablation of the main mass is given by the dashed black line. Right: the measured point-to-point velocities for each camera as compared to the model estimate of the velocity for the main (leading) fragment as a function of height.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: Comparison of modeled WRF winds and radiosonde wind profiles. The winds from the WRF model at the terminal point are shown in red, and the 400 samples of the model are shown in semitransparent black lines. The wind measurements from Buffalo on 2022 November 19 at 00 and 12 UTC are also shown for comparison.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: Left: point-to-point velocity measurements for each camera. The horizontal black line shows the cutoff height for the dynamic mass measurement of the meteorite main mass (right). Right: details of the dynamic mass fit on the velocity measurements; see text for details.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: The amount of mass remaining in the main fragment as a function of dynamic pressure. This shows the mass loss by fragmentation mode, leading to a release of either an eroding fragment (EF) or dust (D). The fireball height is color-coded. A drag coefficient of Γ = 1.0 was used to compute the dynamic pressure for consistency with previous work (J. Borovička et al. 2020). The last fragmentation in which 0.3 kg of mass was released into dust is below the lower limit and not shown.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: Dark-flight model estimate of possible fall locations of the main mass of WJ1 in and around St. Catharines, Ontario. The ground ranges for each hypothesized shape are labeled. Nominal locations for each mass are labeled. Individual points show each Monte Carlo clone in the dark-flight simulation (5 kg: yellow; 10 kg: green; 20 kg: red).
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: Difference in latitude between the ground tracks of the fireball and the asteroid trajectory. As the fireball traveled almost directly due east, only the difference in the latitude (cross-track) is shown. The two data sets are shown: (a) the black curve shows the difference between the fireball trajectory and the asteroid trajectory, and (b) the height color-coded points show the difference of camera measurements with the asteroid trajectory.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: The total trajectory fit residuals per camera measurement relative to the best-fit trajectory as a function of length from the first observed point.
Paper: Telescope-to-Fireball Characterization of Earth Impactor 2022 WJ1
Authors: Theodore Kareta, Denis Vida, Marco Micheli, Nicholas Moskovitz, Paul Wiegert, Peter G. Brown, Phil J. A. McCausland, Hadrien A. R. Devillepoix, Barbara Malečić, Maja Telišman Prtenjak, Damir Šegon, Benjamin Shafransky, Davide Farnocchia
Figure caption: The location and extent of the five Doppler radar returns (labeled (a)–(e) and described in the text) as well as the dark-flight fall curves of small meteorites ejected in fragmentation episodes.
Paper: Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Samantha N. Hasler, L. C. Mayorga, William M. Grundy, Amy A. Simon, Susan D. Benecchi, Carly J. A. Howett, Silvia Protopapa, Heidi B. Hammel, Daniel D. Wenkert, S. Alan Stern, Kelsi N. Singer, Simon B. Porter, Pontus C. Brandt, Joel W. Parker, Anne J. Verbiscer, John R. Spencer
Figure caption: Geometric albedo of Uranus compared with select filter transmission curves of Voyager, New Horizons, and HST. Filter transmission curves have been normalized to a max value of 0.5 for display purposes. The expected filter-integrated values for the New Horizons and HST observations are shown with squares and diamonds, while the actual observations made with the HST campaign are shown in circles with error bars (see Section 2.4). New Horizons data add much needed spectral coverage at critical phase angles.
Paper: Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Samantha N. Hasler, L. C. Mayorga, William M. Grundy, Amy A. Simon, Susan D. Benecchi, Carly J. A. Howett, Silvia Protopapa, Heidi B. Hammel, Daniel D. Wenkert, S. Alan Stern, Kelsi N. Singer, Simon B. Porter, Pontus C. Brandt, Joel W. Parker, Anne J. Verbiscer, John R. Spencer
Figure caption: Hubble images from 2023 September 17 in the F845M, F657N, and F467M filters, taken as part of program GO17294. The approximate image UTC start times are listed for each frame (rounded down to the nearest minute), and the F845M and F657N images have an unsharp mask applied to enhance cloud features. Hubble images have been rotated from their native pixel orientation so that celestial north is oriented up (as indicated by the arrow in the bottom left corner).
Paper: Observations of Uranus at High Phase Angle as Seen by New Horizons
Authors: Samantha N. Hasler, L. C. Mayorga, William M. Grundy, Amy A. Simon, Susan D. Benecchi, Carly J. A. Howett, Silvia Protopapa, Heidi B. Hammel, Daniel D. Wenkert, S. Alan Stern, Kelsi N. Singer, Simon B. Porter, Pontus C. Brandt, Joel W. Parker, Anne J. Verbiscer, John R. Spencer
Figure caption: Top: observing geometry of Uranus in 2023 from (a) New Horizons and (b) from Earth where celestial north is up. A diagram of the phase-angle (α) geometry between New Horizons, Uranus, and the Sun is shown in the top left. Bottom: destriped MVIC frames of Uranus from scan 0557172410 on 2023 September 16. From left to right, each panel is centered on detections (or nondetections) of Uranus in the blue, red, NIR, and CH4 filters. The data are presented in the native pixel orientation.
Paper: Solar Wind Ion Sputtering from Airless Planetary Bodies: New Insights into the Surface Binding Energies for Elements in Plagioclase Feldspars
Authors: Liam S. Morrissey, Stefan Bringuier, Caixia Bu, Matthew H. Burger, Chuanfei Dong, Denton S. Ebel, George E. Harlow, Ziyu Huang, Rosemary M. Killen, Francois Leblanc, Amanda Ricketts, Orenthal J. Tucker, Daniel W. Savin
Figure caption: Anorthite SPs for each element type from the (001), (010), and (110) surfaces. The images are oriented so the +z direction comes out of the page and show a subsection of the complete surface simulated. Calcium atoms are in blue, aluminum atoms are in red, silicon atoms are in pink, and oxygen atoms are in yellow. Each elemental species is numbered by its SP. The spheres representing each element are scaled based on the corresponding atomic radii. The figures were created using the OVITO visualizer for MD simulations (A. Stukowski 2009).
Paper: Solar Wind Ion Sputtering from Airless Planetary Bodies: New Insights into the Surface Binding Energies for Elements in Plagioclase Feldspars
Authors: Liam S. Morrissey, Stefan Bringuier, Caixia Bu, Matthew H. Burger, Chuanfei Dong, Denton S. Ebel, George E. Harlow, Ziyu Huang, Rosemary M. Killen, Francois Leblanc, Amanda Ricketts, Orenthal J. Tucker, Daniel W. Savin
Figure caption: Albite SPs for each element type from the (001), (010), and (110) surfaces. The images are oriented so the +z direction comes out of the page and show a subsection of the complete surface simulated. Sodium atoms are in blue, aluminum atoms are in red, silicon atoms are in pink, and oxygen atoms are in yellow. Each elemental species is numbered by its SP. The spheres representing each element are scaled based on the corresponding atomic radii. The figures were created using the OVITO visualizer for MD simulations (A. Stukowski 2009).
Paper: Solar Wind Ion Sputtering from Airless Planetary Bodies: New Insights into the Surface Binding Energies for Elements in Plagioclase Feldspars
Authors: Liam S. Morrissey, Stefan Bringuier, Caixia Bu, Matthew H. Burger, Chuanfei Dong, Denton S. Ebel, George E. Harlow, Ziyu Huang, Rosemary M. Killen, Francois Leblanc, Amanda Ricketts, Orenthal J. Tucker, Daniel W. Savin
Figure caption: Ejecta emission energy probability distributions using the Thompson model for different SBEs for (A) a sample of Na SPs sputtered from different albite surfaces and (B) for all O SPs sputtered from a (001) anorthite surface.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption:                         (a) Spectra of the 3 μm region extracted from a continuum-removed data cube. These spectra are representative of the spectral diversity observed in the M3 global mode data set. The spectra are offset for clarity, and the color codes are the same as the colors used in the water maps in subsequent figures. Because M3 spectra end at 3 μm, the data with wavelengths less than 3 μm were reflected about 3 μm (gray zone from 3 to 3.8 μm) to form a feature that could be analyzed by the spectral feature shape algorithm of Tetracorder (Clark et al. 2003, 2024b). (b) Reference spectra from the USGS spectral library 6 (Clark et al. 2007) convolved to M3 global mode (85 channel) resolution. These spectral features were selected because they cover the range of observed spectral features in the M3 data set. The minerals used are 2.72 μm: pyrophyllite PSY1A; 2.75 μm: muscovite GDS113; 2.76 μm: illite GDS4; 2.81 μm: tourmaline HS282.2B; 2.82 μm: thenardite GDS146; and 2.83 μm: psilomelane HS139.3B. The M3 global mode does not have the spectral resolution to uniquely identify these minerals, so they are positions only. There is a trend with most phyllosilicates in the USGS spectral library to be at the shorter wavelengths and for sulfates to occur at the longer wavelengths, but this is not universal, and exceptions are used here to cover the possible ranges. The color of the spectra are the same as the colors used in the hydroxyl maps in subsequent figures. (c) The spectra from Figure 4(b) are shown with the continuum removed and scaled to approximately the same band depth. Tetracorder removes the continuum and normalizes the band depth relative to the reference spectra and compares positions and shapes independent of depth. The weakly concave black curve at the top shows the curvature induced by a 10 K error in temperature of the thermal emission for a 400 K surface. Note that the OH feature widths are smaller than the 2.66–2.83 μm continuum interval for the thermal emission curve. The induced error due to a 10° thermal emission error would be less and thus negligible. (d) The M3 global mode gain correction curves vs. instrument detector temperature. The gain factors cover the range from 145 K (blue) to 170 K (red). The actual series used has a resolution of 0.1 K. From Lundeen et al. (2011).
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption:                         (a) Simple cylindrical map of 3 μm water absorptions. The color scheme follows the colors in Figure 4(a). North is up with longitude and latitude as in Figures 1 and 6. (b) Derived 3 μm water absorption map, from Figure 5(a), with nearside enlarged to show details. The color scheme follows the colors in Figure 4(a). North is up with longitude and latitude as in Figures 1 and 6.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption:                         Narrow hydroxyl absorptions for the six band shapes and positions shown in Figure 4(b) and using the same color scheme as in Figure 4(b). Bluer colors are shorter-wavelength absorptions, while red colors are longer-wavelength absorptions spanning the range from 2.72 to 2.83 μm. North is up in this simple cylindrical map. This is a Tetracorder standard product.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: M3 mosaic of global mode data, simple cylindrical projection from −90 to +90 latitude, −180 to 180 longitude. The original mosaic was produced at 0.33 km pixel−1 giving a 32,760 × 16,380 pixel, 85 band image cube. Using this data cube, spectral features were mapped. The apparent reflectance levels were not corrected for phase. Phase angle also affects observed band depths. (A) 1.55 μm apparent reflectance, not corrected for phase angle. (B) Continuum-removed broad 2 μm absorption characteristic of the 2 μm pyroxene absorption. (C) The narrow 2.82 μm absorption attributed to hydroxyl. (D) Continuum-removed absorption band depth after thermal removal of the broad 3 μm water absorption.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: The 1.9 μm water band position. These are very weak absorptions, typically less than about 2% band depth, increasing toward the poles. North is up in this simple cylindrical map. This is a Tetracorder standard product.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Image of the lunar surface with rover and astronaut tracks showing that the disturbed soil is darker and different in color than the surface, indicating changes in grain size and/or composition with depth. Contrast has been increased from the original to show the tracks better.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Pyroxene band position. North is up in this simple cylindrical map. This is a Tetracorder standard product.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Example traverses across CR1 with a longer traverse shown in blue and shorter traverse in pink. Sampling points are marked along both traverses by the pink stars. Yellow stars show the potential landing site area. The darker brown/black areas typically within the craters are PSRs and areas to be avoided when carrying out a traverse.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: (a) Average Earth visibility across the CR1 (E. Mazarico et al. 2011) 120 m pixel−1, where “visible” is Earth visibility of 100% and “not visible” is 0%. (b) Average illumination across the CR1 (E. Mazarico et al. 2011) 120 m pixel−1. (c) Diviner average summer temperature data showing highs of up to 319 K in red and colder temperatures in yellow and green (240 m pixel−1). (d) Diviner winter average temperatures, with the yellow areas showing around 285 K and blue showing areas as cold as 100 K (240 m pixel−1). (e) Oxford thermal model showing ice stability depth, mapped at 120 m pixel−1. (f) Paige model showing ice stability depth, mapped at 120 m pixel−1. (g) M. A. Siegler et al. (2016) ice depth stability model mapped at a resolution 24 m pixel−1. Note the differences in resolution between the three ice depth models and therefore the differing results in the ice stability depths.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Example traverses across GR1 with a longer traverse shown in blue and shorter traverse in pink. Sampling points are marked along both traverses by the pink stars.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: (a) Average Earth visibility across the CR1 (E. Mazarico et al. 2011) 120 m pixel−1, where “visible” is Earth visibility of 100% and “not visible” is 0%. (b) Average illumination across the CR1 (E. Mazarico et al. 2011) is 120 m pixel−1. (c) Diviner average summer temperature data showing highs of up to 318 K in red and colder temperatures in yellow and green (240 m pixel−1). (d) Diviner winter average temperatures, with the red areas showing around 130 K and purple showing areas as cold as 100 K (240 m pixel−1). (e) Oxford thermal model showing ice stability depth, mapped at 120 m pixel−1. (f) Paige model showing ice stability depth, mapped at 120 m pixel−1. (g) M. A. Siegler et al. (2016) ice depth stability model mapped at resolution 20 m pixel−1. Note the differences in resolution between the three ice stability depth models and therefore the differing results.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Mapping features and density of craters at GR1. (a) NAC images across the GR1 region. (b) Boulders and craters mapped across the GR1 region. Note that in regions where there was less lighting or poor albedo contrast it was harder to identify craters. For the middle section shown here that is in darkness, a different image (NAC ID: M146121156RE) was used to map the craters and boulders than shown in (b). There are some areas where no images were found with illumination, and therefore, these areas could not be mapped. Note this affects the traverses mapped in Figure 12. (c) Crater density map across GR1, showing high crater densities in the bottom right of GR1 reaching up to 382.1 craters per 314 m2.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Mapping of features and identifying areas of interest. (a) Raster showing the areas where slopes are less than 10° and where there is 40% or more illumination and Earth visibility in red, and slopes less than 5° and where there is 40% or more illumination and Earth visibility in blue across the GR1 region of interest. (b) The craters and boulders mapped across GR1. (c) Boulders of potential sampling interest highlighted by white circles, located near a crater rim and on crater rim. (d) Mapped boulders and craters on top of rasters shown in (a) and (b).
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Mapping of features and identifying areas of interest. (a) Raster showing the areas where slopes are less than 10° and where there is 40% or more illumination and Earth visibility in red, and slopes less than 5° and where there is 40% or more illumination and Earth visibility in blue across the CR1 region of interest. (b) The craters and boulders mapped across CR1. (c) Boulders of potential sampling interest highlighted by pink circles. (d) The context of those boulders in relation to the mapped craters. (e) Mapped boulders and craters on top of the rasters shown in (a) and (b).
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: (a) Frequency distribution of boulders with distance from the source crater. (b) Scatter graph showing the boulder size in relation to distance from the source crater.
Paper: Mapping Potential Hazards and Identifying Sampling Points within Lunar South Polar Region Areas of Interest
Authors: Sarah J. Boazman, David Heather, Hiroka Inoue, Makiko Ohtake
Figure caption: Topography at GR1. (a) Elevation map over the GR1 region LOLA 5 m pixel−1. (b) Slope map derived from the LOLA elevation map, 5 m pixel−1.