adsabs/AstroCLIMB huggingface dataset:
Paper: Revealing the Interior Structure of Icy Moons with a Bayesian Approach to Magnetic Induction Measurements
Authors: John B. Biersteker, Benjamin P. Weiss, Corey J. Cochrane, Camilla D. K. Harris, Xianzhe Jia, Krishan K. Khurana, Jiang Liu, Neil Murphy, Carol A. Raymond
Figure caption: Sensitivity of the induction response to ocean parameters. Shown is the complex norm of the derivative of the induction amplitude (Ae  i ϕ ) at the synodic frequency with respect to fractional change in ocean thickness as a function of ocean conductivity and thickness. Scenarios are indicated by blue squares. Contours of constant induction amplitude (A) intersecting Scenarios A, B, and F are shown for the synodic, its second harmonic, and the orbital frequency. Scenarios B, D, and F occupy a region where the synodic induction response is saturated, such that changes in ocean thickness produce negligible changes in the induction response.
Paper: Revealing the Interior Structure of Icy Moons with a Bayesian Approach to Magnetic Induction Measurements
Authors: John B. Biersteker, Benjamin P. Weiss, Corey J. Cochrane, Camilla D. K. Harris, Xianzhe Jia, Krishan K. Khurana, Jiang Liu, Neil Murphy, Carol A. Raymond
Figure caption: Example retrieval of Europan interior for Scenario B with 1D and 2D posterior distributions for the three ocean parameters and parameter pairings. 2D posteriors are illustrated by contours of constant probability density drawn enclosing 5%, 50%, 68%, 95%, and 99.7% of the probability mass. Blue lines and squares indicate the input values. Above each contour plot, a histogram displays the posterior for the ocean parameter on the x-axis. In these plots, the horizontal black line indicates the 99.7% interval, the black diamonds indicate the bounds of the 95% interval, and the blue shaded region indicates the Metric II accuracy interval.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Top three rows: Vertical profiles of dayside mean air temperature, vertical wind, and zonal wind over time for the moist atmosphere Control TRAP-1e and the dry atmosphere Dry TRAP-1e. The vertical range of (a) and (b) is 0–5 km, to better show the temperature oscillation near the surface. Due to the relatively low resolution of our simulations, this close-in view results in discontinuities between vertical levels. The discontinuities are not visible in (c)–(f), because the vertical range shown is 0–35 km. Bottom row: Time series of the dayside mean net downward shortwave flux close to the planet’s surface (black), shown with the power spectral density of the zonal wavenumber 1 Rossby wave (red) and the sum of the power spectral density of the waves with zonal and meridional wavenumbers 1–1, 2–1, 2–2, and 3–2 (blue). The different limits of the y-axis should be noted.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Comparative climatology of the five simulations, showing (from left to right) the vertical temperature profile at the substellar and antistellar point, the zonal mean zonal wind, the vertical water vapor profile at the substellar and antistellar point, and the surface temperature. From top row to bottom row: Control ProxB, Warm ProxB, Control TRAP-1e, Warm TRAP-1e, Dry TRAP-1e. All values are 300 day means.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Top: Time series of Rossby wave phase velocity at 71N for Control and Dry TRAP-1e simulations. Bottom: Time series of Rossby wave phase velocity at 71N overlaid with the longitudinal position of the northeast Rossby gyre for Control TRAP-1e. A 3 day rolling mean has been applied to all curves.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Long-term mean of the general circulation for Control TRAP-1e and Dry TRAP-1e, as well as daily snapshots of days 0, 10, and 20 and days 0, 30, and 60, respectively. The differing quiver scale in (c) should be noted.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Vertical profile of dayside mean total cloud cover (sum of ice and liquid) over time for the Control TRAP-1e simulation. As in Figures 5(a) and (b), the short vertical range of 0–5 km results in discontinuities between vertical levels due to the low resolution of the simulation.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Time–longitude diagrams of the mid-latitude (55–85N) averaged meridional wind at an altitude of 2.96 km above the surface. Subplot (f) also shows the low latitudes for Dry TRAP-1e. Positive values correspond to northward flow, while negative values represent southward flow.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Mean cloud condensate (mixing ratio, kg kg−1) over time at the planetary limb for each of the four moist atmosphere simulations. Liquid and ice cloud are shown separately. Each type of cloud is averaged over all latitudes and all heights on the eastern and western terminator. The data have been filtered to remove cycles with periods shorter than 10 days. The different limits of the y-axis should be noted.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Longitudinal and latitudinal cross sections of the dayside cloud layer for the four moist atmosphere simulations. The total cloud level is the sum of ice and liquid cloud condensate. The images depict 120 day means.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Time series of the 1.4 μm water absorption feature and 2.7 μm CO2 absorption feature for the Control ProxB, Warm ProxB, Control TRAP-1e, and Warm TRAP-1e simulations. A sample of 300 days is taken to cover the 157.5 and 120 day oscillation periods in the Control and Warm Proxima Centauri b simulations, respectively.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Latitude–time diagrams of Rossby wave phase velocity for each simulation at h = 2.96 km height. Positive values correspond to eastward flow, while negative values represent westward flow. The phase velocity is calculated via subtraction of the mean zonal wind as in Figure 4.
Paper: Traveling Planetary-scale Waves Cause Cloud Variability on Tidally Locked Aquaplanets
Authors: Maureen Cohen, Massimo A. Bollasina, Denis E. Sergeev, Paul I. Palmer, Nathan J. Mayne
Figure caption: Wind vectors overlaid on the total cloud condensate (sum of ice and liquid) at the given height for Warm ProxB and Control TRAP-1e simulations. The images are daily snapshots chosen to illustrate the eastmost and westmost phases of the Rossby gyre migration for each planet.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Distance at which an object of 100 m is deformed by 30%, vs. dynamic viscosity (in poise) and interaction timescale (in hours). Results are presented for cases in which the Sun, the Earth, and Jupiter are the primary orbital bodies.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Optimized fit (red line) for a random parameter choice. The true (blue line) and noise-added data (gray points) are also plotted for comparison.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Synthetic light curves of a body rotating with an arbitrary period for a range of phase angles (A) and aspect ratios (B).
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Evolution of ‘Oumuamua’s aspect ratios due to tidal deformation. The primary aspect ratio (left column) is the ratio of the largest to the smallest axis, while the secondary (right column) is the ratio of the intermediate to the smallest axis. At t = 0, both aspect ratios are 6. The time of discovery is plotted as a vertical dashed line.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Evolution of ‘Oumuamua’s spin period due to modulation in the moment of inertia. The period is initialized at p = 7.3906, ensuring that p = 7.3975 hr at discovery (vertical dashed line) for the optimal fit. Rows represent different initial sizes.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Synthetic light curves of ‘Oumuamua, which incorporate simulated changes in period and aspect ratio from tidal deformation. Rows correspond to the initial sizes and colors correspond to the dynamic viscosities of the body in the simulations. The time of discovery is indicated with a vertical dashed line.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Best-fit χ 2 values between synthetic and photometric data. Empty spaces indicate parameter choices for simulations that were not run. Fits for both October and November are computed and the χ 2 values are added together.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Flowchart showing the structure of the simulation runs used to model ‘Oumuamua.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Synthetic light curve using the ML15 model (red line) alongside photometric observations of ‘Oumuamua (gray points, data from Belton et al. 2018). The period, initial rotation state, and average magnitude are optimized for the first six nights.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Simulated change of ‘Oumuamua’s moment of inertia from 2017 May 4 to 2018 January 16. Red X’s indicate simulations that were halted because of disintegration or numerical divergence. Empty squares indicate parameters for simulations that were not run, as convergence was achieved for lower dynamic viscosity values.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Order-of-magnitude area change of Apophis for a range of dynamic viscosities, in square meters.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: The distribution of χ 2 for 104 synthetic light curves. The histogram marginalizes over all selected parameters, which were randomly chosen.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Left: the (g − r) and (r − J) colors of Col-OSSOS targets. Repeat measurements for targets (10 objects) have been connected by dashed lines. The reddening curve is shown by the solid black curve. Right: the projection values PC1 and PC2 of the (g − r) and (r − J) colors. In this projection, the reddening curve is a horizontal line with PC2 = 0. Gray hashes show lines of constant (g − r) or (r − J) color. The blue dashed–dotted curve in both panels marks PC2 = −0.13, the value we have adopted to distinguish the FaintIR (below) and BrightIR classes. The bottom and side panels show histograms of the full data set (black) and of the objects in the BrightIR (blue, bottom panel) and FaintIR classes (orange, bottom panel). In both panels, red points are CCKBOs defined by their i free < 4°, yellow and red points together are CCKBOs by the historical definition based on i (see Section 3), and black points are all those excited objects outside the CC region. Objects identified as belonging to the class of blue binary KBOs (Fraser et al. 2021) are outlined with cyan halos.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Left: the optical colors of KBOs and Centaurs reported in Peixinho et al. (2015). The data points generally scatter around and follow the reddening curve, which is shown by the solid line. Right: the projection values PC1 and PC2 of the (V − R) and (R − I) colors shown in the left panel. Only the colors of objects with color uncertainty Δ(V − R) < 0.1, Δ(R − I), and H  R  > 4 are plotted. The limit on absolute magnitude is made to avoid the few dwarf planets that have surfaces dominated by their own rheologies and therefore have colors that are outliers on this plot. Red points are CCKBOs defined by their i free, yellow and red points together are CCKBOs by the historical definition based on i, and black points are all those excited KBOs outside the CC region.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Left: the (g − r) and (r − z) colors of Col-OSSOS targets. Repeat measurements for targets o3l63 and o3l79 have been connected by dashed lines. Right: the projection values PC1 and PC2 of the (g − r) and (r − z) colors shown in the left panel. Red points are CCKBOs defined by their i free, yellow and red points together are CCKBOs by the historical definition based on i, and black points are all those excited KBOs outside the CC region. The blue dashed–dotted line in both panels is the curve of PC 2 = −0.13 below which all FaintIR objects are found. These mainly consist of CCKBOs. The color scheme follows that of Figure 1.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Synthetic light curves for ‘Oumuamua, which incorporate simulated aspect ratio changes and constant period. Colored lines indicate the dynamic viscosity and photometric data are shown in gray points. These curves use optimized values of β 0 and ΔV. Note that the rotation state is entirely fixed in these curves, with no evolution in the rotation period or axis. This allows for comparison to the photometric data and the original composite light curve, since the evolution of the rotation will require a more complex and physically accurate model.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: The optical colors of Jupiter Trojans reported in the Sloan Digital Sky Survey Moving Object Catalog v4 (Ivezić et al. 2001) with Δ(g − r) < 0.04 and Δ(r − i) < 0.04. The data points generally scatter around and follow the reddening curve, which is shown by the solid line. Error bars are omitted for clarity. Semitransparent points are used to show overlapping table values. The shading is a kernel density estimate to highlight the densest regions of the data.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: Diagram of the cross-sectional ellipse. Unprimed coordinates are fixed in the reference frame of the solar system, while primed coordinates are fixed in the reference frame of the object. The angle β defines the rotation state of the body with respect to the Sun.
Paper: Numerical Simulations of Tidal Deformation and Resulting Light Curves of Small Bodies: Material Constraints of 99942 Apophis and 1I/‘Oumuamua
Authors: Aster G. Taylor, Darryl Z. Seligman, Douglas R. MacAyeal, Olivier R. Hainaut, Karen J. Meech
Figure caption: The best-fit synthetic light curve (red line) and photometric data (gray points). This model incorporates the simulated changes in aspect ratio. Here, μ = 109 g cm−1 s−1 and the body is initially 75 m.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Histograms of (r − z) and (g − r) color samples from our mixing model. Orange and blue points represent FaintIR and BrightIR objects, respectively, with the black curve showing the overall sample histograms. The histograms were weighted to have an equal number of objects in each class, which is approximately true of the observed sample. The absolute values in this figure are meaningless. The (r − z) histogram is only of optically red KBOs with (g − r) > 0.85, which show a bimodality in (r − z) that is apparent in both the simulations and the observations. Neither the simulated nor the observed (r − z) distribution is bimodal for objects with (g − r) < 0.85.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Left: the (F606W − F814W) and (F814W − F139M) colors of KBOs and Centaurs reported in Fraser & Brown (2012). The reddening curve is shown by the solid curve. The curve of PC2 = −0.13 is shown by the blue dotted–dashed curve. Colors are in the STMAG system. The left and bottom panels show histograms of the colors. Right: the projection values PC1 and PC2 of the (F606W − F814W) and (F814W − F139M) colors shown in the left panel.  The left and bottom panels show histograms of PC1 and PC2. The horizontal blue dotted–dashed line at PC2 = −0.13 marks the value below which all FaintIR objects are found. These mainly consist of CCKBOs. The color scheme follows that of Figure 1; red points are CCKBOs defined by i free, yellow and red points are those based on i, and black points are KBOs outside the CC region. The blue binary 2003 HG57 is outlined with a cyan halo. All histograms show only objects that have uncertainties less than 0.1 mag in both colors to avoid inclusion of uncertain measurements that may mask the presence of the bifurcation in PC2.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: The Col-OSSOS data set plotted with the mixing model representation (red dashed curves in the top panel). Simulated spectra were those randomly drawn that were consistent with the (g − r) and (r − J) colors of the mixing models. Other colors were evaluated from those spectra. The resultant colors for mixing model classes 1 and 2 are shown by the orange and blue points, respectively. Point transparency of 50% is used to show where simulated colors clump.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Visual demonstration of the reddening curve projection. The dashed grid shows curves of constant PC1 and PC2 in intervals of 0.1. Objects with positive and negative values of PC2 have convex and concave spectra and are found above and below the reddening curve, respectively. The point values show the extremal projection values.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Left: the (u − g) and (g − r) colors of Col-OSSOS targets. Right: the projection values PC1 and PC2 of the (g − r) and (u − g) colors shown in the left panel. The color scheme follows that of Figure 1; red points are CCKBOs defined by i free, and black points are KBOs outside the CC region. In these colors, CCKBOs cannot be differentiated from excited KBOs, to the S/N limits of the data set.