adsabs/AstroCLIMB huggingface dataset:
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Average diurnal variability of the total injection rates (in atoms m−3 s−1) of Al estimated by the CABMOD-MIF model at northern high latitudes (65° < ϕ < 90°, panels (a), (f), (k), and (p)), northern mid-latitudes (15° < ϕ < 65°, panels (b), (g), (l), and (q)), equatorial latitudes (−15° < ϕ < 15°, panels (c), (h), (m), and (r)), southern mid-latitudes (−15° < ϕ < −65°, panels (d), (i), (n), and (s)), and southern high latitudes (−65° < ϕ < −90°, panels (e), (j), (o), and (t)). The left panels represent the average rates between L s = 0° (northern spring/southern fall) and L s = 90° (northern summer/southern winter). Panels in the second column show the average rates between L s = 90° (northern summer/southern winter) and L s = 180° (northern fall/southern spring). Panels in the third column represent the average rates between L s = 180° (northern fall/southern spring) and L s = 270° (northern winter/southern summer). The right panels show the average rates between L s = 270° (northern winter/southern summer) and L s = 360° (northern spring/southern fall).
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the injection rates (in atoms m−3 s−1) of Na (a, b, and c), Mg (d, e, and f), and Al (g, h, and i) estimated by the CABMOD-MIF model for the OCCs and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). The maximum ablation rates of the three metals appear at perihelion and for a latitude of −10°. Note that the color scales are different for each meteoric metal.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Histogram displaying the normalized mass influx rate into Earth’s atmosphere over the mass range considered by the LDEF spacecraft (yellow) and the DMZC for the JFCs constrained with three different observations: SAAMER (orange), Planck satellite (green), and IRAS satellite (purple).
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the relative mass influx of meteors into the Martian atmosphere determined by the MIF model for the OCCs and three orbital positions: aphelion (L s = 71°, (a)), perihelion (L s = 251°, (b)), and first crossing of the ecliptic plane (L s = 325°, (c)).
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Mirror plots of carbon-4 isomeric carbonyls produced by LILBID (top) and EI (bottom). Panel (a) presents 2-butanone, and panel (b) shows butanal spectra. The x-axis represents m/z values, and the y-axis represents normalized relative intensities (arbitrary units). For the full spectrum, see Appendix Figure A2.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Mirror plots of carbon-3 isomeric carbonyl spectra produced by LILBID (top) and EI (bottom). Panel (a) shows a LILBID acetone spectrum and the corresponding spectrum from EI. Panel (b) shows a mirror plot of propanal (isomeric carbonyl of acetone). The x-axis represents m/z values, and the y-axis shows normalized relative intensity (arbitrary units). For full LILBID spectra of acetone and propanal, see Appendix Figure A1.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Mirror plots of carbon-6 isomeric carbonyls produced by LILBID (top) and EI (bottom). The comparison between mass spectra of (a) 2-hexanone and (b) hexanal are shown. The x-axis represents m/z values, and the y-axis represents normalized relative intensities (arbitrary units). For a full spectrum, see Appendix Figure A3.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: (a) Schematic of the LILBID-ToF-MS experiment used for this work. The schematic is taken from Klenner et al. (2019). (b) A high-speed photograph of a pulsed-IR laser irradiating a microliquid water beam in vacuum. (c) Schematic of the process (as shown in panel (b)) of a shock-wave anisotropic dispersion of a water beam into charged fragments. Panels (b) and (c) are taken and adapted from Wiederschein et al. (2015).
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Comparison of LILBID and EI spectra of deuterated acetone-D6. The LILBID (top) produces protonated molecular cations at m/z 65 due to [C3D6O+H]+), whereas EI (bottom) produces molecular cations at the exact mass of the acetone-D6 molecule at m/z 64 from [C3D6O)]+. The x-axis represents m/z values, and the y-axis shows normalized relative intensity (arbitrary units). For the full spectrum, see Appendix Figure A1(b).
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Different types of ionization reactions during the EI process (adapted from Smith 2004). The left side represents a molecule (A-B-C) exposed to an electron (e−) beam of 70 eV, and the right side shows the production of different ionic and neutral species. (a) Excitation of a molecule that remains undetected, (b) formation of negative ions not detected by positive EI MS, (c) formation of a positive molecular ion, (d) formation of fragment cations, (e) formation of fragment cations with rearrangements, and (f) multiple ionization processes to form singly and doubly charged ionic species.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Composition and formation pathways of molecular and fragment cations of (a) acetone and (b) propanal-isomeric carbonyl compounds as produced by EI and LILBID. Organic fragment clusters with water are not shown.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Composition and formation pathways of molecular and fragment cations of a sample of aldehydes and ketones with a carbon number of four. Comparisons of EI and LILBID fragmentation and ionization of (a) 2-butanone and (b) butanal are given.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: Steady-state solutions of (a) separation velocity (cm yr-1), (b) melt fraction, (c) solid overpressure (MPa), and (d) forces (N) in Equation (6) under η  l  = 10 Pa s and 160 TW of tidal dissipation within the layer. Colors indicate different solid viscosities η  s , corresponding to 1019 (red), 1020 (orange), and 1021 Pa s (green). (b) The thickness of a high-melt-fraction layer (ϕ > 0.2) exceeds 50 km only when η  s  is larger than 1021 Pa s. (d) Buoyancy (gray) is plotted positive upward, whereas the resistance of solid matrix to compaction (colored) is shown positive downward.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: Characteristic melt fraction of the partial-melt layer as a function of rheological parameters. Black lines show values calculated using scaling laws, whereas colored ones are results from Figures 2–4. A surface volcanic flux of 1.5 cm yr−1 is assumed here, which corresponds to a surface heat flow of 100 TW. (a) The scaling relation of Equation (11) is plotted as a function of melt viscosity, whereas modeled values are taken from the porosity profiles of η  s  = 1019 (red) and 1020 Pa s (orange). The average melt fraction at the top 20% of the partial-melt layer is adopted as characteristic values. (b) The scaling relation of Equation (13) is plotted as a function of solid viscosity, whereas the modeled values are adopted from a case for η  l  = 1 Pa s. It is noted that Equation (13) predicts the average melt fraction of the partial-melt layer, and the maximum melt fraction (dotted) is higher than the value indicated by the scaling law.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: (a) Average melt fraction and (b) the thickness of high-melt-fraction layer (ϕ > 0.2) as a function of total tidal dissipation within the partial-melt layer. Colors indicate different solid viscosities η  s , corresponding to 1019 (red), 1020 (orange), and 1021 Pa s (green), and dotted, solid, and dashed lines describe melt viscosities η  l  of 1, 10, and 100 Pa s, respectively. (c)–(d) Contours of the maximum melt fraction as a function of melt and solid viscosities. For a predicted rate of tidal dissipation (100–200 TW), a high-melt-fraction layer consistent with the observation of Khurana et al. (2011) is only stable when η  l  ≥ 100 Pa s or η  s  ≥ 1021 Pa s.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: (a)–(b) Steady-state solutions of (a) separation velocity (cm yr-1) and (b) melt fraction under η  s  = 1020 Pa s and 100 TW of tidal dissipation within the layer. Colors indicate different melt viscosities, corresponding to 1 (red), 10 (orange), and 100 Pa s (green). The thickness of a high-melt-fraction layer (ϕ > 0.2) exceeds 50 km only when η  l  is larger than 100 Pa s. (c) Forces (N) described in Equation (2) for a case with η  l  = 10 Pa s. Buoyancy (gray solid) is plotted as positive upward, whereas viscous drag (orange) and the resistance of solid matrix to compaction (gray dashed) are positive downward.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: (a) The profile of melt fraction under the tidal dissipation rate of 160 TW. Three different layer thicknesses are assumed: 200 (red), 400 (orange), and 700 km (green), and the degree of melt increases when tidal dissipation is concentrated within a narrow depth range. (b) Maximum (solid) and average (dashed) melt fraction. Results are plotted as a function of total tidal dissipation within a partially molten layer.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: The profiles of (a) solid overpressure (MPa) and (b) melt fraction for a case with η  l  = 10 and η  s  = 1020 Pa s. Colors indicate pressure difference imposed at the top boundary, corresponding to liquid overpressures of 3 (red), 1 (orange), and −1 MPa (green). The profile of the melt fraction changes little with boundary conditions.
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: (Left) Two NSTs and Ryugu. The spectrum of Ryugu is from Kitazato et al. (2019), provided by Yada et al. (2021). All three of these objects share similar NST reflectance spectra despite their range in semimajor axis (1.18, 2.47, and 3.43 au for Ryugu, Svea, and Cybele, respectively) and size (1, 81, and 237 km in the same order). Svea is offset from Cybele and Ryugu for clarity. (Right) Polana and Bennu. While the available spectrum of Polana, a putative parent body for low-albedo NEOs, is relatively low-quality, it is consistent with the average spectrum of Bennu from Zou et al. (2021).
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: Same as Figure 4 but with a linear 2.9–3.6 μm continuum removed and focusing on that wavelength region. Also added is Antiope, with its continuum adjusted to better fit 67P. Most of the NST spectra are qualitatively similar to 67P, though spectra with larger observational uncertainties are obviously less compelling matches.
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: Cybele, 67P, and two residues of irradiated ice mixtures from Urso et al. (2020). The Urso et al. experiments involved mixtures of different amounts of water ice, methanol, and ammonia, irradiated and then heated to 300 K. The spectra of the residues were presented by Urso et al. in optical depth; they have been converted to transmission and their contrast has been stretched for this plot. Cybele, 67P, and the residues have qualitatively similar spectra in this wavelength region.
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: Average NST and ST spectra, both as calculated from the average Gaussian parameters for those groups and as calculated from the actual spectra. While the Gaussian fits are not adequate for detailed compositional studies, they do allow the basic differences between groups to be studied.
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 NST groups. The distinction between Ceres and Themis types is difficult to make in most of the new measurements, though most seem more akin to Themis in BD and BC. Also presented is Winchester, which has a shallow but definite band that seems to represent a distinct group separate from either Themis or Ceres types.
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: Adapted from Rivkin et al. (2019). Observations of Interamnia, including a rereduced 2007 spectrum and the new 2015 spectrum, show relatively consistent behavior at a global scale, though details differ, including behavior near 3.3 μm and the specific location of the BC.
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: Cumulative distributions of BC for different Bus taxonomic classes. As shown by Rivkin et al. (2015b), the Ch/Cgh class is dominated by ST objects. However, all of the other groupings have significant NST populations, with the majority of the objects being >3 μm.
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: Cumulative distributions of BC for different asteroidal locations. Steep increases shortward of 3 μm in the inner and middle belt show that ST objects dominate there, though NST objects are also present. The bulk of objects have BC > 3 μm in the outer belt and Cybele–Hilda regions, indicating that NST objects are much more common.
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 four objects presented here are interpreted as NB. They cover a range of sizes, solar distances, and spectral types, but NB spectra are rare in the spectral sample. These 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: Though data quality varies, additional objects with bands like Winchester (Figure 13) are present in the sample. Because Bamberga is the largest such object, we refer to these as Bamberga types. Further study is necessary to determine how robust this grouping is.
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: Continuum-removed reflectance spectra for new objects. The asteroid number and date of observation are included in each panel, and each panel shares the same x- and y-axis bounds and tick marks.
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: PCA of 710 NEAs with the “α-line” boundary from DeMeo et al. (2009), which separates the S- and C/X-complexes. Space weathering and shock-darkening trends are shown as adapted from Binzel et al. (2019) and Reddy et al. (2014). Ordinary chondrite grain size trends are also shown for El Hammami (H), Viñales (L), and Chelyabinsk (LL) meteorites at 45–90 μm, 90–150 μm, 150–300 μm, 300–500 μm, and 500–1000 μm grain sizes with increasing plot marker size. 1998 OR2 is shown at the end of the shock-darkening trend, within the C/X-complex, despite having H-chondrite-like mineralogy. PC values for the dark lithology of meteorite analog Chergach are shown for <45 μm and 150–300 μm grain sizes.
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: Left: molar content of fayalite (Fa) vs. ferrosilite (Fs) derived for 1998 OR2 showing a mineralogy consistent with H-chondrites. The error bars in the upper right corner correspond to the uncertainties derived by Sanchez et al. (2020), 2.0 mol% for Fa and 1.4 mol% for Fs. Figure adapted from Nakamura et al. (2011). Right: molar content of fayalite (Fa) versus ol/(ol+px) ratio derived for 1998 OR2. Black dashed boxes represent the range of values for each ordinary chondrite subgroup, and gray solid boxes represent the uncertainty in those measurements. Figure adapted from Dunn et al. (2010). Both panels indicate an H-chondrite-like mineralogy.
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 NEA (52768) 1998 OR2. Visible data (0.45–0.93 μm) were taken with the RAPTORS I telescope from Tucson, Arizona, on 2020 April 16 UTC. NIR data (0.78–2.49 μm) were obtained using the NASA IRTF on 2020 February 28 UTC and retrieved from the MITHNEOS survey archives. All data were normalized to 0.8 μm to provide overlap between visible and NIR data and then renormalized to 1.5 μm.
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: Band I center vs. BAR with select S-type asteroid subgroups from Gaffey et al. (1993). 1998 OR2 falls between the S(IV) OC “boot” and the S(VI) region. Error bars are on the order of the marker size.