adsabs/AstroCLIMB huggingface dataset:
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: The four images selected, with the ellipses computed after the thresholding process by VADER. Cyan ellipses are computed with incidence angle threshold set at 90°; yellow ones are computed using an incidence angle threshold set at 100°. (a) Image 4241; (b) image 4242; (c) image 4243; (d) image 4244 (see Table 1 for definitions of images).
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: The (p; q) plots for (a) the sub-S/C point changed by −2° in both latitude and longitude and (b) the sub-S/C point changed by +2° in both latitude and longitude. The results of all the images are merged together: where the green is darker, more than one image has solutions. The black cross represents the DART Dimorphos shape with uncertainties.
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: The (p; q) plots showing the comparison between VADER results and DART Dimorphos shape (indicated, together with uncertainties, by the black cross): (a) image 4241; (b) image 4242; (c) image 4243; (d) image 4244.
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Zoom-in of the liciacube_luke_l2_1664234241_00417_01 green channel image showing the nightside hemisphere of Dimorphos after the impact (highlighted by the red circle).
Paper: VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE
Authors: Angelo Zinzi, P. H. A. Hasselmann, V. Della Corte, J. D. P. Deshapriya, I. Gai, A. Lucchetti, M. Pajola, A. Rossi, E. Dotto, E. Mazzotta Epifani, R. T. Daly, M. Hirabayashi, T. Farnham, C. M. Ernst, S. L. Ivanovski, J.-Y. Li, L. M. Parro, M. Amoroso, J. Beccarelli, I. Bertini, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, M. Dall'Ora, L. Gomez Casajus, E. Gramigna, S. Ieva, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, B. Negri, P. Palumbo, D. Perna, S. Pirrotta, G. Poggiali, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: The (p; q) plots for all the images taking into consideration the threshold for the incidence angle at 90°. The results of all the images are merged together: where the green is darker, more than one image has solutions. The black cross represents the DART Dimorphos shape with uncertainties.
Paper: Detection of Close Kuiper Belt Binaries with HST WFC3
Authors: Simon B. Porter, Susan D. Benecchi, Anne J. Verbiscer, W. M. Grundy, Keith S. Noll, Alex H. Parker
Figure caption: Cumulative distributions of the brightnesses and physical separations of the SSOLS binaries in Table 1 (blue, solid) in comparison with the known KBO binaries (orange, dashed) listed at http://www2.lowell.edu/users/grundy/tnbs/status.html. The semimajor axes of the SSOLS binaries are estimated as their apparent separation times ﹩\sqrt{2}﹩. The SSOLS binaries are both fainter and tighter than the known binary KBOs. The only binary KBOs that are tighter than the SSOLS blended binaries are the two detected by New Horizons (2011 JY31 and 2014 OS393; Weaver et al. 2022) and the third by a stellar occultation (2014 WC510; Leiva et al. 2020).
Paper: Detection of Close Kuiper Belt Binaries with HST WFC3
Authors: Simon B. Porter, Susan D. Benecchi, Anne J. Verbiscer, W. M. Grundy, Keith S. Noll, Alex H. Parker
Figure caption: Recovery efficiency of simulated binary KBOs with SSOLS-style synthetic data, assuming jitter of 0.1 pixels and F606W–F814W color of 0.72. Each panel corresponds to 1000 simulations with a different primary/secondary flux ratio. The synthetic data was processed in the same way as the actual SSOLS data. The separations of the synthetic binaries were varied uniformly from 0 to 3 pixels but binned and averaged here for clarity. Recovery efficiency was as expected better for brighter satellites farther away, with very few (but still some) 10:1 flux ratio binaries detectable. None of the synthetic single-PSF cases were detected as a false-positive binary at 95% confidence.
Paper: Detection of Close Kuiper Belt Binaries with HST WFC3
Authors: Simon B. Porter, Susan D. Benecchi, Anne J. Verbiscer, W. M. Grundy, Keith S. Noll, Alex H. Parker
Figure caption: Examples of (top) a well-separated binary KBO, (middle) a blended-binary KBO, and (bottom) a KBO that appears to be single. The top separated binary case accounted for 11.6% of the KBOs in the SSOLS data set. For the middle case, the single-PSF solution only subtracts the primary, leaving behind a significant residual that is not there for the double-PSF solution, strongly indicating that this KBO is a blended binary. The residuals for the bottom case are almost identical for the single-PSF and double-PSF solutions, indicating that it is not binary to the resolution of HST/WFC3. All of these images are the F606W stacks for these objects; we performed the same analysis for the F814W stacks and enforced consistency between them for objects that we identified as blended binaries.
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: Absolute reflectance of CI and CM simulant material before and during laser irradiation between 0.24 and 2.5 μm. Top: spectra of loose CI (red line) and CM (black line) simulant powder obtained under ambient conditions. Middle: CI spectra (from top to bottom at 0.3 μm) correspond to the spectrum after 0 (black), 1 (orange), 3 (magenta), and 5 (blue) pulses. Bottom: CM spectra (from top to bottom at 0.3 μm) correspond to the spectrum after 0 (black), 1 (orange), 3 (magenta), and 5 (blue) pulses. One laser pulse corresponds to one raster across the sample.(The data used to create this figure are available.)
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: Secondary electron (SE) SEM images of a CI ((a) and (c)) and CM ((b) and (d)) simulant pellet before and after irradiation. Panels (a) and (b) show images of the fresh material, while panels (c) and (d) are of representative laser-irradiated regions. The white scale bar at the lower left side of each panel corresponds to 2 μm in length.
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: Absolute and relative change of the normalized reflected intensity for the CI (empty red symbols) and CM (filled black symbols) sample during laser irradiation. Top: absolute reflectance at 0.55 μm (circles), 1.0 μm (inverted triangles), and 2.0 μm (crosses). Bottom: normalized reflected intensity at 0.55 μm (circles), 1.0 μm (inverted triangles), and 2.0 μm (crosses).
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: Changes in the average spectral slope for the CI (empty red symbols) and CM (filled black symbols) sample during laser irradiation. Top: average spectral slope between 0.3 and 0.7 μm. Bottom: average spectral slope between 0.8 and 2.4 μm.
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: SDSS g − r color of C-complex asteroid families as a function of their dynamical ages. The error bars of the family colors correspond to the standard deviation among the whole members. The horizontal dotted and dashed lines indicate the g − r colors of the CI and CM laboratory spectra, respectively. Each set of lines corresponds to laboratory spectra after 0, 1, and 5 laser pulses.
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: High-resolution XPS spectra of the fresh (black solid line) and weathered (red dashed line) CM sample. Bottom right: the ratio between the integrated area of the irradiated and the unirradiated surface for a given photoelectron transition.
Paper: Laser Irradiation of Carbonaceous Chondrite Simulants: Space-weathering Implications for C-complex Asteroids
Authors: Andy J. López-Oquendo, Mark J. Loeffler, David E. Trilling
Figure caption: Distribution of the SDSS griz visible spectral slope of C-complex asteroid families. The filled bars correspond to the percentage of blue (negatively sloped) asteroids in a given family, while the dashed bars correspond to the percentage of red (positively sloped) asteroids.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Bow shock and induced magnetospheric boundary terminator distances, calculated for all dayside crossings. All values are from 2007 May 1 to November 30. (a) Terminator distance R TD (see Equation (2)), values given from the center of Mars, (b) Mars–Sun distance during the study period in astronomical unit, (c) normalized terminator distance values. The dust storm phases are marked in the dashed lines: (i) dust loading begins, (ii) dust storm becomes global, and (iii) surface conditions return to normal. The solar longitude of Mars is included on the x-axis.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Mars Express ASPERA data from 2007 August 7. Shown here are the (a) electron counts, (b) proton counts, (c) heavy ion counts from the ELS and IMA instruments, and (d) altitude of the spacecraft traveling outbound in it is orbit around Mars. The vertical line (i) indicates an induced magnetospheric boundary (IMB) crossing from the planetary plasma region into the magnetosheath, and (ii) shows a bow shock crossing from the magnetosheath into the solar wind.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Mean terminator distance of the bow shock calculated per 10° × 10° bin across the Martian surface, for all dayside crossings of the bow shock from 2007 May 1 to November 30. Base map is the Martian topography for reference to surface features. Topography obtained by the digital elevation model of the Mars Global Surveyor’s Mars Orbiter Laser Altimeter (USG 2023).
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: All bow shock (BS, red) and induced magnetospheric boundary (IMB, turquoise) crossings from 2007 May 1 to November 30, as observed by Mars Express. Bow shock positions taken from Hall et al. (2019) and verified by eye. All IMB positions recorded by eye. Plotted in Mars Solar Orbital coordinates.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Terminator (a) and subsolar (b) distances, in Mars Solar Orbital Coordinates.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Differences between the Wang et al. (2020) model boundary location and the Mars Express crossing of the boundary. Gray line indicates that the Mars Express crossing matched where the model predicts the boundary to be, located using the solar wind conditions from the Tao model. Black dashed lines indicate different dust stages: (i) dust loading begins, (ii) dust storm becomes global, and (iii) surface conditions return to normal. Maroon and teal points represent the bow shock and induced magnetospheric boundary, respectively. The plot includes all dayside and nightside crossings of boundaries.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Bow shock surface in Mars Solar Orbital coordinates, produced by the Wang et al. (2020) model with solar wind input from the Tao model. Model produced for conditions at the time of the Mars Express crossing of the boundary at 20:49:24 on 2007 November 12. Blue cross is the point on the model boundary surface that is closest to the Mars Express crossing (orange cross). Points projected to each axis are represented by dots.
Paper: Effects of the 2007 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Richard P. Haythornthwaite, Dikshita Meggi, Rudy A. Frahm, Mats Holmström
Figure caption: Comparison of the ENLIL and Tao solar wind models to the ASPERA solar wind data at Mars.
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: Band I center vs. BAR from Gaffey et al. (1993) for NEOs whose spectra exhibit absorption bands centered at ∼1 and 2 μm due to the presence of olivine and pyroxene. The polygonal region corresponds to the S(IV) subtype associated with ordinary chondrites (OC). The horizontal lines represent the approximate boundaries for ordinary chondrites found by Sanchez et al. (2020). The rectangular zone overlapping the S(IV) subtype represents the spectral zone for acapulcoite–lodranite clan meteorites found by Lucas et al. (2019). The rectangular zone (BA) includes the pyroxene-dominated basaltic achondrite assemblages (Gaffey et al. 1993). The dashed curve indicates the location of the olivine–orthopyroxene mixing line (Cloutis et al. 1986).
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 fayalite (Fa) and ferrosilite (Fs) and ol/(ol+px) ratio for NEOs with an ordinary chondrite-like composition (red squares). The synthetic data set corresponding to the three ordinary chondrite subtypes (H, L, LL) created to train the machine-learning classifier is also shown. The error bars correspond to the uncertainties derived by Sanchez et al. (2020), 2.0 mol% for Fa, 1.4 mol% for Fs, and 0.04 for the ol/(ol+px) ratio.
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: Distribution of absolute magnitudes (H) and diameters for the NEOs included in the spectroscopic study. Diameters were calculated from the absolute magnitudes and the mean geometric albedo of the sample (P  V  = 0.22).
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: Approximate fractions of the main taxonomic types and ordinary chondrites. In this figure, asteroids in the S-complex include Q-types and a new subclass of objects introduced in the present study called Sx-types. Asteroids in the C/X-complex include those with ambiguous C- or X-complex classification plus asteroids classified as Xk-, Xn-, and B-types. The fraction corresponding to “others” includes K-types and objects whose taxonomic classification is indeterminate.
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: Distribution of taxonomic types found in the present study. The label C/X corresponds to objects with ambiguous C- or X-complex classification. The label IND is assigned to objects whose taxonomic classification is indeterminate. The Sx-types are a new subclass of objects introduced in the present study. The source regions of the NEOs are indicated with different colors.
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 content of fayalite (Fa) vs. ferrosilite (Fs) for NEOs with an ordinary chondrite-like composition whose spectra do not show the 2 μm band. Measured values for H- (green), L- (orange), and LL- (blue) ordinary chondrites from Nakamura et al. (2011) are also included. The error bars 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).
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 asteroids 163348 (2002 NN4), 2015 AP43, 2015 LK24, 2015 TF, 2016 EB1, 2017 FU64, and 2017 OP68. Modeled albedo curves that encompass the observed thermal fluxes and thermally corrected spectra are shown.
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: Probability of NEOs belonging to the three ordinary chondrite subtypes (H, L, LL). Each row represents an NEO, and each column represents an ordinary chondrite subtype.
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: Normalized confusion matrix resulting from the multinomial logistic regression model. Labels correspond to the three ordinary chondrite subtypes (H, L, LL).
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: Amplitude vs. spin rate for the NEOs included in the photometric study. Taxonomic types are indicated with different colors. Objects whose amplitudes and spin rates were determined in this study (or previous work) are depicted with circles. Objects for which only a lower limit for the amplitude and spin rate was calculated are depicted with triangles. The curves represent the critical spin rate for bulk densities (ρ) of 1.0, 2.0, and 3.0 g cm−3. Figure adapted from Pravec & Harris (2000).
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: Rotational periods vs. absolute magnitudes for all NEOs with published lightcurves (black dots). NEOs with a full lightcurve presented in this study are depicted with red circles (Apollos), green squares (Amors), and blue diamonds (Atens). NEOs with partial lightcurves (i.e., a lower limit for their periods) are indicated with triangles and the same color code as mentioned before. The red dashed line is the spin barrier at 2.2 hr.