adsabs/AstroCLIMB huggingface dataset:
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: The change in Apophis’s spin period due to its 2029 Earth tidal encounter is shown as a function of the angle between the Apophis-COM-to-Earth vector and the asteroid’s long axis, ϕ, at perigee and for different asteroid internal structures: homogeneous with ρ head = 2.2 g cm−3 (blue disks), heterogeneous with ρ head = 2.8 g cm−3 (orange crosses), and heterogeneous with ρ head = 3.3 g cm−3 (green squares).
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: (a) A map of the mean slope over a tumbling period for each facet of the Apophis shape model for Case 15 projected onto an equatorial map. The downslope direction is indicated by arrows whose length scales with the slope magnitude. (b) A map of the amplitude of the slope change, δθ, across Apophis for Case 15. (c) A map of the excavation depth due to the volume flux of centimeter-sized particles over the course of 10 kyr due to periodic surface slope changes caused by the asteroid’s tumbling state. This map is constructed using the granular mass flow prescription discussed in Section 5.1.
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: The radial acceleration for the surface particles highlighted in Figure 3(d) (top panel), Figure 3(e) (middle panel), and Figure 3(f) (bottom panel) for −1 to 1 hr since perigee. The top and bottom panels show that the axes that are originally in compression (negative values of acceleration), due to tidal stresses, begin to relax as the asteroid moves past Earth. The surface particle along the orthogonal axis (middle panel) is initially in tension (positive values). This latter surface particle is aligned with the vector that points from Apophis to Earth in that simulation. As Apophis flies by Earth, the alignment of different body axes with the tidal force flips. Axes that were once in tension become compressed, and vice versa.
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: (a) Mass movement results from periodic bed-tilting simulations of a granular bed (R.-L. Ballouz et al. 2019a) are used to construct a new formulation based on the geophysical process of dry ravel (Equation (2)). (b) The fraction of the Apophis surface “excavated” after a given time for three different cases (see Table A3). The horizontal dotted line denotes when 50% of the Apophis surface has been excavated to a depth >10 cm. The 50% excavation horizontal line crosses Case 15 (solid curve), Case 52 (dashed curve), and Case 37 (dotted–dashed curve) at times of 24, 50, and 223 kyr, respectively.
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: (a) Self-noise of the Silicon Audio SP (green curve) and InSight SEIS SP (yellow curve) and VBB (red curve) seismometers compared to the power spectral density computed from the motion of a particle on the surface of Apophis that is aligned with its major axis (x-axis; blue curve). The time series used to compute the ground motion (Figure 3(a)) was from 16 hr surrounding its close approach with Earth (∼6.0 R ⊕) on 2029 April 13. For reference, the new high-noise model and new low-noise model for Earth (J. R. Peterson 1993) are shown (black dashed lines). (b) Same as (a), but the blue curve now shows the predicted motion on the surface on the asteroid’s intermediate axis (y-axis) that is aligned with the Apophis–Earth vector at perigee. In both panels, the cutoff at larger frequencies is artificial, representing the simulation output Nyquist frequency. The true response of the asteroid to tidal forces may continue to rise at higher frequencies.
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: A series of snapshots of the surface radial acceleration across the surface of a simulated rubble-pile Apophis during a discrete shaking event triggered by its close encounter with Earth (magenta shaded region in Figure 3). The radial accelerations of discrete surface particles are projected onto an equatorial map. The bluer colors on the edges of each panel do not represent any particles and are an artifact of the projection of 3D data onto these 2D maps. (a) The beginning of the event, t = –1.12 hr before perigee, where a region near the equator and longitude ∼60°W exhibits strong vertical motion that begins propagating radially outward. (b)–(d) Surface acceleration maps show a seismic surface wave expanding radially outward at ∼100 m s−1. (e) Peak ground motion as Apophis experiences global shaking. Simulations show the possibility for antipodal focusing and ringing as strong shaking (|a/g| > 0.1|) continues for tens of seconds. (f)–(h) Global shaking decays over the next ∼2 minutes.
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: Close-ups of the simulated ground motion on Apophis shown in Figure 3 for the events in the cyan shaded region (a), the magenta shaded region (b), and the yellow shaded region (c).
Paper: Shaking and Tumbling: Short- and Long-timescale Mechanisms for Resurfacing of Near-Earth Asteroid Surfaces from Planetary Tides and Predictions for the 2029 Earth Encounter by (99942) Apophis
Authors: R.-L. Ballouz, H. Agrusa, O.S. Barnouin, K.J. Walsh, Y. Zhang, R.P. Binzel, V.J. Bray, D. N. DellaGiustina, E.R. Jawin, J.V. DeMartini, A. Marusiak, P. Michel, N. Murdoch, D.C. Richardson, E.G. Rivera-Valentín, A.S. Rivkin, Y. Tang
Figure caption: The radial acceleration for the surface particles highlighted in Figure 3(a) (top panel), Figure 3(b) (middle panel), and Figure 3(c) (bottom panel) after the initial settling period. Background vibration levels are on the order of 5–15 nm s−2, which is 3–4 orders of magnitude smaller than the seismic accelerations induced by the close encounter.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: Images of comet NEOWISE taken on (a) 2020 July 18 14:30 by Zixuan Lin and (b) 2020 July 3 03:19 by PSP/WISPR. Both images are aligned with north upward, and are plotted on R.A. and decl. axes (units in degrees). A scale bar of 107 km in the plane of the sky is provided in the bottom left-hand corner. The dust tail is clearly seen as the curved tail arcing to the right of the comet for each image. Image (a) shows extensive fine-scale structures being highly visible, while image (b) from PSP shows limited structural detail. In (a), the striae in the tail are the narrow, near-parallel streaks that point approximately northward. The tail is also clearly segmented into two curved bands for image (a), which analysis shows to be the syndynic bands of the tail.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: A Finson–Probstein modeled dust tail overlaid onto the image shown in Figure 2, taken on 2020 July 18 14:30 by Zixuan Lin. The blue line shows the comet’s orbital path, and the green line shows the Sun–comet vector, which is the direction of radiation pressure on the dust grains. The red lines denote syndynes, which are lines of constant dust β. The yellow lines denote synchrones: lines of constant dust age, labeled with the date of the respective dust ejection.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: Comet NEOWISE's trajectory with respect to the Sun–Earth line and ecliptic plane. Ecliptic plane gridlines are 0.1 au apart. Comet positions are shown every five days, with the approximate ion tail position shown as radial lines, for orientation.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: Graphs of the second derivative of the average syndyne brightness (y-axis) against dust β values (x-axis) using (a) amateur images only, (b) PSP images only, and (c) both data sets. The shaded blue area denotes the 96% confidence interval. The graphs clearly show a bimodal distribution of dust in the tail, with the peak β values of each peak displayed clearly in red. The dust-sparse region in the middle is bounded by the dotted green lines, showing the extent of this region as well as the peak β value associated with it.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: Temporal maps of images taken on (a) July 12, (b) July 17, and (c) July 18 (Figure 2), from top to bottom. Dust β is on the y-axis as a logarithmic axis, with the bottom of each image corresponding to a minimum β value of 0.01. The date and time of dust ejection is on the x-axis. Fine-scale structures such as striae and syndynic bands can be accurately tracked with ease using these temporal maps, enabling analysis of how these structures change over time. Images taken by Michael Jäger, Rutger Bus, and Zixuan Lin, respectively.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: Images (a) and (c) are images of comet NEOWISE in which an atomic sodium tail is visible (oriented so that north is upward). Image (a), taken by PSP WISPR on 2020 July 5, has no color information. However, a short featureless tail can be seen between the main bulk of the ion tail (pointing toward upper right) and the green antisunward vector line. Image (c), taken by Mustafa Aydin on 2020 July 12, clearly displays a bright red tail adjacent to the blue ion tail, a typical characteristic of atomic sodium tails. Images (b) and (d) show the modeled atomic sodium tail (red line) overlaid onto images (a) and (c), respectively. Images (b) and (d) show that there is good agreement between the modeled and the observed tails, as well as providing evidence that the short tail observed by PSP was indeed the atomic sodium tail.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: A graph showing the approximate points of origin in heliographic coordinates at the Sun of the solar wind that encountered the comet on a Mercator projection. The comet’s position was mapped back to the solar wind source surface at 2.5 solar radii from the center of the Sun using ballistic mapping. This takes into account the rotation rate of the Sun and is computed for two solar wind speeds: 800 km s−1 (orange), and 400 km s−1 (blue). The position of the neutral line at the source surface for Carrington rotation 2232, approximating that of the HCS further out in the heliosphere, is shown as the solid black line. This neutral line position is provided by the Wilcox Solar Observatory. The intersection of the source region tracks and the neutral line suggest that the comet’s only HCS crossing occurred around 2020 June 28.
Paper: Characterization of the Dust and Sodium Tails of Comet C/2020 F3 (NEOWISE) from Parker Solar Probe and Amateur Observations
Authors: Qasim Afghan, Geraint H. Jones, Karl Battams, Oliver Price, Andrew J. Coates
Figure caption: Temporal maps of images taken on July 12 (a), July 17 (b), and July 18 (Figure 2) (c), from top to bottom. This is similar to Figure 4, but with a smaller date range and β range to focus on the striae region. Images taken by Michael Jäger, Rutger Bus, and Zixuan Lin, respectively.
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: The spatial distribution of the model 5–2 resonant objects in the OSSOS++ model realized on Julian Date 2459874.5. The position of Neptune is shown by the blue square. Only those objects with r < 27 are shown. The realization is ∼8× oversampled. Objects seen by the New Horizons and DEEP pointings are shown in blue and red, respectively, with color-matched histograms of each sample shown in the inset. As well, the inset also shows an example of a radial distribution of discoveries that would be discovered from an annulus model in the New Horizons (orange) and DEEP (green) pointings. The example is of an annulus centered at 70 au. The annuli histograms have been rescaled for clarity. Annuli centered at other distances merely move the histogram of simulated detections inward or outward accordingly. This figure demonstrates how strongly survey pointing can influence the density and distribution of detectable resonant objects, an effect that is not present in distributions that are longitudinally symmetric.
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: A diagram of the ResNet structure we have adopted. A master network consists of ensembles of the deceptively simple network. Each branch of the ensemble consists of two residual layers, with each layer consisting of two standard convolutional layers (3 × 3 kernels, 16 and 32 filters for first pair and second pair of convolutional layers, respectively) with surrounding skip connection and max-pooling between residual layers. The two residual layers are followed by two fully connected layers with 64 nodes each, and finally a sigmoid output. The outputs of the three branches, each with identical structure but independent training runs, are averaged for the classification probability of this ensemble. The final probability we adopted is the ensemble of three separate master ensemble networks like that shown above, but with each ensemble trained using an independent training data set. We direct the reader to K. He et al. (2016) for an understanding of the operations of a ResNet.
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: Results of orbit fitting to simulated ephemerides of objects in the 5:2 resonance model that fell within the New Horizons discovery field. Top left: barycentric inclination vs. heliocentric distance. Fitted data are shown in circles, with true values in red open squares. Simulated arcs of lengths of 2, 4, and 26 days are shown in blue, orange, and green, respectively. The fitted and true values of each object are connected by black dashed lines. Top right: fitted vs. simulated barycentric inclinations for the objects shown in the top left panel. The 1–1 line is shown by the dashed line. Bottom left: simulated vs. fitted heliocentric distances for the objects shown in the top left panel. The 1–1 line is shown by the dashed line.
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: The barycentric inclination and distance of the discoveries we report here. A histogram of the heliocentric distances is shown in the bottom panel, with bin width of 5 au chosen to be similar to the typical uncertainty of the objects with best-fit heliocentric distance R > 70 au. Uncertainties are 1σ values from the best-fit orbit clouds (see Section 3.4).
Paper: Candidate Distant Trans-Neptunian Objects Detected by the New Horizons Subaru TNO Survey
Authors: Wesley C. Fraser, Simon B. Porter, Lowell Peltier, JJ Kavelaars, Anne J. Verbiscer, Marc W. Buie, S. Alan Stern, John R. Spencer, Susan D. Benecchi, Tsuyoshi Terai, Takashi Ito, Fumi Yoshida, David W. Gerdes, Kevin J. Napier, Hsing Wen Lin, Stephen D. J. Gwyn, Hayden Smotherman, Sebastien Fabbro, Kelsi N. Singer, Amanda M. Alexander, Ko Arimatsu, Maria E. Banks, Veronica J. Bray, Mohamed Ramy El-Maarry, Chelsea L. Ferrell, Tetsuharu Fuse, Florian Glass, Timothy R. Holt, Peng Hong, Ryo Ishimaru, Perianne E. Johnson, Tod R. Lauer, Rodrigo Leiva, Patryk S. Lykawka, Raphael Marschall, Jorge I. Núñez, Marc Postman, Eric Quirico, Alyssa R. Rhoden, Anna M. Simpson, Paul Schenk, Michael F. Skrutskie, Andrew J. Steffl, Henry Throop
Figure caption: Estimated color terms for the HSC EB-gri filter for the SDSS and PS systems. The bottom panel shows the difference between the modeled colors and the third-degree polynomial fit to the colors shown by the red curve.
Paper: Radar Circular Polarization Ratio of Near-Earth Asteroids: Links to Spectral Taxonomy and Surface Processes
Authors: Edgard G. Rivera-Valentín, Betzaida Aponte-Hernández, Patrick A. Taylor, Michael C. Nolan, Ellen S. Howell, Dany Waller, Luisa F. Zambrano-Marín, Anne K. Virkki, Ronald-Louis Ballouz, Angela M. Stickle
Figure caption: The resultant PDF for (a) X-complex, (b) V-type, (c) C-complex, (d) L-type, (e) S-complex, and (f) Q-type NEAs, scaled by their maximum value, along with the bootstrap estimate for 1σ (dashed lines) and 2σ uncertainty (solid lines). The taxonomic classes are denoted by color following the legend in the figures, within which N is the total number of objects in the taxonomic class. Note that the x-axis for the X complex extends to CPR = 2, while for the others, it extends to CPR = 1.5.
Paper: Radar Circular Polarization Ratio of Near-Earth Asteroids: Links to Spectral Taxonomy and Surface Processes
Authors: Edgard G. Rivera-Valentín, Betzaida Aponte-Hernández, Patrick A. Taylor, Michael C. Nolan, Ellen S. Howell, Dany Waller, Luisa F. Zambrano-Marín, Anne K. Virkki, Ronald-Louis Ballouz, Angela M. Stickle
Figure caption: Box plot illustrating the summary statistics for the combined Arecibo S-band CPR radar and MITHNEOS spectral taxonomic database. The number of objects in each class, N, is listed below the taxonomic label. Unclassified objects are represented by a question mark. The red line represents the median value for the class, the blue box encapsulates the interquartile range, the black dashed lines represent a distance of 1.5 times above/below the upper and lower quartiles, and the black dots are data beyond these limits.