adsabs/AstroCLIMB huggingface dataset:
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: Comparison of asteroid spectral slopes measured using the SDSS MOC (x-axis) and LDT (y-axis). Error bars in the x-direction represent the full range of slopes measured in the SDSS MOC for asteroids with multiple slope measurements. Error bars in the y-direction represent errors in slope corresponding to measurement uncertainty associated with the LDT spectra. The dotted line represents the location of the 1:1 line, where SDSS MOC and LDT slope measurements would be equal. Those asteroids plotted with a large marker show an overlap in measured slope ranges in the SDSS MOC and LDT data, and those asteroids plotted with a small marker do not show an overlap in measured slope ranges between the two data sets.
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: The 0.85 − J and J − K color indices of all asteroids observed with the NASA IRTF. Asteroids with spectral slopes steeper than the average R-group Trojan are plotted in red, and those with shallower slopes are plotted in black. Asteroids classified as D types are plotted with larger markers than those classified as all other types. The color indices of the LR (lower left cluster; gray) and R (upper left cluster; gray) groups from Emery et al. (2011) are plotted for comparison. We draw attention to the asteroids that have higher J − K color values than would be predicted based on their 0.85 − J color if this population was Trojan-like that plot above the main cluster of R-group Trojans.
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: VNIR spectra of all asteroids observed with both the LDT and IRTF in this survey. All spectra are normalized to 1 at 0.55 μm and displayed at the same scale to enable direct visual comparison. Each spectrum is plotted alongside the average R- and LR-group Trojan reflectance spectrum from Emery et al. (2011).
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: Visible reflectance spectra of all objects observed with the LDT. Spectra from the 2021 and 2022 apparitions of (1947) Iso-Heikila are plotted separately. All spectra are normalized to 1 at 0.55 μm and displayed at the same scale to enable direct visual comparison. Each spectrum is plotted alongside the average R- and LR-group Trojan reflectance spectrum from Emery et al. (2011).
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: Near-infrared reflectance spectra of all objects observed with the IRTF. All spectra are normalized to 1 at 1 μm and displayed at the same scale to enable direct visual comparison. Each spectrum is plotted alongside the average R- and LR-group Trojan reflectance spectrum from Emery et al. (2011).
Paper: The Distribution of Highly Red-sloped Asteroids in the Middle and Outer Main Belt
Authors: Oriel A. Humes, Cristina A. Thomas, Lauren E. McGraw
Figure caption: Comparison of the VNIR spectra of objects throughout the solar system with steeply red spectral slopes. The VNIR spectrum of steep-sloped red object (81819) 2000 KS35 from this work is plotted alongside examples from the literature for comparison purposes. The mean colors of the RR TNOs and accompanying 1σ color ranges are sourced from Fulchignoni et al. (2008). The spectrum of large, steeply sloped main-belt asteroid 269 Justitia originates from Hasegawa et al. (2021). The mean R Trojan spectra is reproduced from Emery et al. (2011). The Apollo 11 sample measurements are taken from the RELAB database (Milliken 2020) and were originally measured by Carle M. Pieters. The D-type average spectrum and 1σ ranges are sourced from DeMeo et al. (2009). All spectra are normalized to 1 at 0.55 μm for ease of comparison.
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: Combination of regions in the (x,k)-space that produce either ﹩{P}_{\max }﹩ (blue) or ﹩{\rm{\Delta }}{P}_{\max }﹩ (orange) values in our simulations that match the observed values in Didymos system observations. The dashed vertical and horizontal lines indicate how the assumption of k = 0.0001 leads to a particle size parameter of ﹩{\mathrm{log}}_{10}(x)=3.1﹩ and a particle size of about 200 μm.
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: Density plots of simulated values of ﹩{P}_{\max }﹩ (left) and ﹩{{\rm{\Delta }}}_{c}={P}_{\max ,R}-{P}_{\max ,B}﹩ (right). The horizontal axis is the particle size parameter x, and the vertical axis is the imaginary part of the refractive index k, both in 10-based logarithmic scale.
Paper: Modeling Linear Polarization of the Didymos–Dimorphos System before and after the DART Impact
Authors: Antti Penttilä, Karri Muinonen, Mikael Granvik, Zuri Gray, Stefano Bagnulo, Ludmilla Kolokolova, Fernando Moreno
Figure caption: Plots showing how the observed Δ t  on the vertical axis are inverted back to change in particle diameter (left) or k (right) using simulated data with the B filter and R filter.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Same as Figure 1 for the reflectance spectrum of Ch-class asteroid 19 Fortuna (Paper I). The spectral characteristics of 19 Fortuna serve as a marker for the 0.7 and 0.43 μm features in C-complex asteroids; all C-complex asteroids show similar spectral widths (see Vilas et al. 1993b, 1994).
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Reflectance spectra divided by a linear continuum calculated across a spectral range of 0.55–0.85 μm of Jovian irregular satellites in the JVIII Pasiphae retrograde (i = 149°) cluster: JVIII Pasiphae, JXII Ananke (in 2006), JXII Ananke (in 2010), and JXVII Callirrhoe. Spectra are scaled to 1.0 across a 100 Å spectral width around 0.55 μm. Spectra are offset by 0.5 in reflectance for clarity. The binned, lower-resolution spectrum of JXVII is plotted with larger symbols for ease of visibility.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Same as Figure 1 for reflectance spectra of Jovian irregular satellites in the JVIII Pasiphae retrograde (i = 149°) cluster: JVIII Pasiphae, JXII Ananke (in 2006), JXII Ananke (in 2010), and JXVII Callirrhoe.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Mixing modeling fits to three members of the prograde (i = 28°) cluster: JVI Himalia, JVII Elara (in 2006), JXII Elara (in 2009), and JX Lysithea. Satellite spectra are plotted in blue. Model fits are plotted in red.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: JVI Himalia spectrum (blue dots) compared with JVI Himalia from Jarvis et al. (2000; red open squares), demonstrating the consistency of the lower edge of the 0.7 μm feature between observations.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Reflectance spectra of end-members used for compositional modeling: (a) aC (Rouleau & Martin 1991), (b) lizardite (http://speclib.rsl.wustl.edu/), (c) “Himalia Phyllosilicate“ simulating Fe-bearing serpentine and saponite combined, and (d) a kerogen-like spectrum derived from Sinope.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Same as Figure 1 for the reflectance spectra of Jovian irregular satellites JIX Sinope (in 2006) and JIX Sinope (in 2009).
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Notional drawing of the Himalia cluster parent body, demonstrating where the satellites JVI Himalia, JVII Elara, and JX Lysithea (delineated by different shadings in the drawing) could reside in their parent body based on the changes in composition. The sizes are taken from the NEOWISE tabulation (see Table 3; Grav et al. 2015; Mainzer et al. 2016).
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Same as Figure 1 for the reflectance spectrum of Jovian irregular satellite JXI Carme in the retrograde (i = 165°) cluster.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Overview of the best model for Scenario A and its ability to fit our constraints. Panels (A)–(D) show the semimajor axis (A), inclination (B), eccentricity (C), and hyperbolic excess velocity (D) as observed by CMOR (orange solid line) and as reproduced in our model (black solid line). The gray solid lines show the collisional grooming iterations, where the lighter gray tones show the early iterations and the darker show more final ones. The blue line represents the model residuals. Panel (E) shows the SFD of particles impacting Earth (black solid line), the broken power-law fit (orange dashed line), and Grun et al. (1985) interplanetary (pink dashed line) and lunar (blue dashed line) particle fluxes. The Grun et al. (1985) fluxes are multiplied by a factor of 3 to account for the gravitational focusing effect that Earth experiences with respect to the Moon and interplanetary space (Pokorný et al. 2018). The legend shows broken power-law fit parameters and the fitting function. All fluxes are cumulative. Panel (F) shows the distribution of particle density with heliocentric distance measured in the ecliptic plane for our model (black solid line) and the fitted exponential (orange dashed line). The fit parameters and fitting function are shown in the legend. Finally, the blue panel shows the value of ﹩{{ \mathcal M }}_{\dot{M}}﹩ and the goodness-of-fit function values. The red panel shows the model parameters ﹩{ \mathcal P }﹩.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Variations of the goodness-of-fit function ﹩{\chi }_{\mathrm{tot}}^{2}﹩ of our Scenario A JFC model for 216 different parameters value combinations (﹩{{ \mathcal P }}_{\alpha }﹩, ﹩{{ \mathcal P }}_{{A}_{{\rm{s}}}}﹩, ﹩{{ \mathcal P }}_{\gamma }﹩). The three symbols represent three different values of ﹩{{ \mathcal P }}_{\gamma }﹩: (×; 0.125), (•; 0.15), and (+; 0.175). For clarity, we offset the × and + symbols from • but all three symbols have the same values of (﹩{{ \mathcal P }}_{\alpha }﹩, ﹩{{ \mathcal P }}_{{A}_{{\rm{s}}}}﹩). Each of the model realizations is color-coded by the value ﹩{\chi }_{\mathrm{tot}}^{2}﹩ . The region of the best-fitting parameters is denoted by the black rectangle: ﹩4.325\leqslant {{ \mathcal P }}_{\alpha }\leqslant 4.425﹩ and ﹩1500\lt {{ \mathcal P }}_{{A}_{{\rm{s}}}}\lt 8500﹩. Panel (A) shows the full range of the total ﹩{\chi }_{\mathrm{tot}}^{2}﹩, where we recorded the minimum value ﹩{\chi }_{\mathrm{tot}}^{2}=1.13﹩ for (﹩{{ \mathcal P }}_{\alpha }﹩, ﹩{{ \mathcal P }}_{{A}_{{\rm{s}}}}﹩, ﹩{{ \mathcal P }}_{{B}_{{\rm{s}}}}﹩, ﹩{{ \mathcal P }}_{\gamma }﹩) = (4.40, 8000, −0.24, 0.125). Panel (B) contains the same information, but the color scale now spans those values of ﹩{\chi }_{\mathrm{tot}}^{2}﹩ within 10% of the minimum value (1.13). Panel (C) shows the variation in the goodness-of-fit for mass accretion at Earth, ﹩{\chi }_{\dot{M}}^{2}﹩, while panel (D) shows the variation in the goodness-of-fit for the SFD slope, ﹩{\chi }_{\alpha }^{2}﹩.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Goodness-of-fit function variations for different values of model parameters ﹩{ \mathcal P }﹩. Panel (A) shows the influence of ﹩{{ \mathcal P }}_{\alpha }﹩ on the goodness-of-fit functions for fixed ﹩{{ \mathcal P }}_{\gamma }=0.15,{{ \mathcal P }}_{{A}_{s}}=5500,{{ \mathcal P }}_{{B}_{s}}=-0.24﹩. Goodness-of-fit functions are color-coded: ﹩{\chi }_{R}^{2}﹩ is shown in yellow, ﹩{\chi }_{\dot{M}}^{2}﹩ in pink, ﹩{\chi }_{O}^{2}﹩ in blue, and ﹩{\chi }_{\alpha }^{2}﹩ in black. The gray region shows the parameter space we used for our focused fitting ﹩{{ \mathcal P }}_{\alpha }\in [4.2,4.6]﹩. Panels (B)–(D) show the same as panel (A) but for parameters ﹩{{ \mathcal P }}_{{A}_{s}},{{ \mathcal P }}_{\gamma },\,\text{and}\,{{ \mathcal P }}_{{B}_{s}}﹩, respectively. The focused fitting parameter space is (B) ﹩{{ \mathcal P }}_{{A}_{s}}\in [1000,8000]﹩, (C) ﹩{{ \mathcal P }}_{\gamma }\in [0.125,0.175]﹩, and (D) ﹩{{ \mathcal P }}_{{B}_{s}}=-0.24﹩.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: The same as Figure 5 but now for Scenario B using the Gaidos (1999) total Zodiacal Cloud cross section ΣZC = 1.12 × 1017 m2 for our JFC model. The three symbols represent three different values of ﹩{{ \mathcal P }}_{\gamma }﹩: (×; 0.175), (•; 0.20), and (+;0.225). For clarity, we offset the × and + symbols from • but all three symbols have the same values of (﹩{{ \mathcal P }}_{\alpha }﹩, ﹩{{ \mathcal P }}_{{A}_{{\rm{s}}}}﹩). Each of the model realizations is color-coded by the value ﹩{\chi }_{\mathrm{tot}}^{2}﹩. The region of the best-fitting parameters is denoted by the black rectangle: ﹩4.1725\leqslant {{ \mathcal P }}_{\alpha }\leqslant 4.225﹩ and ﹩1500\lt {{ \mathcal P }}_{{A}_{{\rm{s}}}}\lt 8500﹩. Panel (A) shows the full range of the total ﹩{\chi }_{\mathrm{tot}}^{2}﹩, where we recorded the minimum value ﹩{\chi }_{\mathrm{tot}}^{2}=0.299﹩ for (﹩{{ \mathcal P }}_{\alpha }﹩, ﹩{{ \mathcal P }}_{{A}_{{\rm{s}}}}﹩, ﹩{{ \mathcal P }}_{{B}_{{\rm{s}}}}﹩, ﹩{{ \mathcal P }}_{\gamma }﹩) = (4.20, 5000, −0.24, 0.20). Panel (B) shows the values within 10% of the minimum value ﹩{\chi }_{\mathrm{tot}}^{2}=0.292﹩. Panel (C) shows the variations of the goodness-of-fit for mass accretion at Earth ﹩{\chi }_{\dot{M}}^{2}﹩, while panel (D) shows the same for the goodness-of-fit ﹩{\chi }_{\alpha }^{2}﹩ for SFD slope α.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Initial conditions for JFCs in our numerical models. Panel (A) shows the cumulative distributions of semimajor axis a for 10 different values of critical perihelion distance q ⋆ (color-coded solid and dashed lines) and the currently observed distribution of JFCs with comet total magnitude parameter M 1 ≤ 12. Panels (B)–(D) are the same as panel (A) but show instead the inclination (panel (B)), eccentricity (panel (C)), and perihelion distance (panel (D)) cumulative distributions. The legend also shows the total number of bodies for each perihelion distance set, N. The data for currently observed JFCs were obtained on 2021 May 20 from https://ssd.jpl.nasa.gov/sbdb_query.cgi. An ASCII version of the cumulative plots is available at the project's GitHub.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Normalized surface density Σ/Σ10au of the steady-state solution as a function of heliocentric distance for our simple test scenario of dust migrating from a heliocentric distance of 10 au via PR drag with no planets included (gray solid line). All collisions between particles are destructive in this case and the collision products are omitted. The analytic solution given by Equation (13) is represented by a black dashed line. We ran our collisional grooming code for five different values of η 0, which is linearly proportional to the collisionless cloud mass, surface area, or the total number of particles. The analytic solution agrees with the solutions of our code for all five values shown here.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: Maximum target and impactor size ratio for destructive collisions ﹩{{ \mathcal R }}_{\max }﹩. If the target is larger than ﹩{{ \mathcal R }}_{\max }﹩, then the target is not destroyed during the collision. This figure shows values of ﹩{{ \mathcal R }}_{\max }﹩ for four different values of A  s . In Panel (A) we show A  s  = 102 J kg−1, which is equal to the A  s  = 3.02 × 106 erg g−1 used in Krivov et al. (2005). Panels (B)–(D) show ﹩{{ \mathcal R }}_{\max }﹩ for A  s  = 3 × 104, 3 × 105,  and 106 J kg−1, which are cases of interest in this manuscript.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: The same as Figure 6 but now for the best model for Scenario B.
Paper: How Long-lived Grains Dominate the Shape of the Zodiacal Cloud
Authors: Petr Pokorný, Althea V. Moorhead, Marc J. Kuchner, Jamey R. Szalay, David M. Malaspina
Figure caption: The same as Figure 4 but now using the Gaidos (1999) total Zodiacal Cloud cross section ΣZC = 1.12 × 1017 m2 for our JFC model. The focused fitting parameter space for Scenario B is (A) ﹩{{ \mathcal P }}_{\alpha }\in [4.0,4.4]﹩, (B) ﹩{{ \mathcal P }}_{{A}_{s}}\in [1000,8000]﹩, (C) ﹩{{ \mathcal P }}_{\gamma }\in [0.125,0.225]﹩, and (D) ﹩{{ \mathcal P }}_{{B}_{s}}=-0.24﹩.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Left: space-weathering parameter Δη vs. grain size for the LL-chondrite Chelyabinsk. Black squares represent the Δη values calculated for different grain sizes of Chelyabinsk obtained by Bowen et al. (2023). Red squares represent the Δη values of Chelyabinsk plus space weathering (SW) after being offset to match the Δη calculated for asteroid Itokawa (blue diamond) from the spectrum obtained by Binzel et al. (2001). Right: space-weathering parameter Δη vs. date for the Didymos system. Δη has been calculated from the PC values reported by Polishook et al. (2023). The location in the x-axis of the Didymos system corresponds to the observation dates carried out before (September 26) and after (September 27–October 2) the impact of the DART mission. For both figures, regions corresponding to the different regimes of space weathering (fresh, intermediate, and saturated) from Binzel et al. (2019) are indicated.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: NIR spectra of NEOs 163348, 2006 XY, 2012 ER14, 2014 WN4, 2015 TB25, 2017 BW, and 2017 FU64. Also shown are the spectra of the CM2 carbonaceous chondrite Mighei (RELAB sample IDs cmms01 and ccms01), the CM2 carbonaceous chondrite Murchison (RELAB sample ID cnms02), troilite from the Canyon Diablo iron meteorite (RELAB sample ID cae01), the enstatite achondrite (aubrite) Khor Temiki (RELAB sample ID latb48), CAIs from Allende (RELAB sample ID c1tm05), and the CM2 carbonaceous chondrite ALH84033 (RELAB sample ID c1mp14).
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: PC2′ vs. PC1′ diagram from DeMeo et al. (2009). PC values calculated for 2013 CW32, 2016 CM194, 2017 WX12, 2019 SH6, and the metal-rich chondrite NWA 12273 (Reddy et al. 2019) are depicted with different colors. PC values for intimate mixtures of the L-chondrite Viñales and the iron meteorite Gibeon and intimate mixtures of Chelyabinsk and shock-darkened (SD) material from (Reddy et al. 2014) are also shown. Arrows indicate the direction in which the grain size or the content of metal and shock darkening increases. The first data point for the mixture of Viñales and Gibeon (lower right corner) corresponds to a mixture of 40 wt% Gibeon and 60 wt% Viñales. The following data points represent increments of 20 wt% Gibeon. The space-weathering vector from Binzel et al. (2019) is also indicated.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Molar contents of wollastonite (Wo) vs. ferrosilite (Fs) for NEOs 85990, 2015 BC, 2015 WF13, 2015 XC, 2016 EF28, 2017 RR15, and 2020 RO6. The error bars correspond to the values determined by Burbine et al. (2009), 3 mol% for Fs and 1 mol% for Wo. The approximate range of pyroxene chemistries for howardites, noncumulate eucrites, cumulate eucrites, and diogenites from Sanchez et al. (2013) are indicated as dashed boxes.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Spectra of intimate mixtures of the L-chondrite Viñales and the iron meteorite Gibeon. All spectra are normalized to unity at 0.55.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Left: spectra of the LL-chondrite Chelyabinsk corresponding to five different grain sizes plus a slab from Bowen et al. (2023). All spectra are normalized to unity at 0.55 μm. Right: Band I and II depths as a function of grain size measured from the Chelyabinsk spectra. Uncertainties are smaller than the symbols.
Paper: The Population of Small Near-Earth Objects: Composition, Source Regions, and Rotational Properties
Authors: Juan A. Sanchez, Vishnu Reddy, Audrey Thirouin, William F. Bottke, Theodore Kareta, Mario De Florio, Benjamin N. L. Sharkey, Adam Battle, David C. Cantillo, Neil Pearson
Figure caption: Space-weathering parameter Δη as a function of the perihelion distance for S-, Sq-, and Q-types. Regions corresponding to the different regimes of space weathering (fresh, intermediate, and saturated) from Binzel et al. (2019) are indicated. Figure adapted from Binzel et al. (2019).