adsabs/AstroCLIMB huggingface dataset:
Paper: Could the Magnetic Star HD 135348 Possess a Rigidly Rotating Magnetosphere?
Authors: Rahul Jayaraman, Swetlana Hubrig, Daniel L. Holdsworth, Markus Schöller, Silva Järvinen, Donald W. Kurtz, and George R. Ricker
Figure caption: Archival XSHOOTER spectra showing “double-horned” Brackett line emission for HR 5907 (top panel), compared with the lack of a similar profile in HD 135348 (bottom panel). A similar plot of the Brackett series, albeit for HD 23478 and HD 345439, can be found in Figure 1 of Eikenberry et al. (2014). The dotted vertical lines mark the wavelengths of the corresponding Brackett series line (Br14: 15876.3 Å, Br12: 16402.8 Å, Br11: 16802 Å).
Paper: The Appearance of a “Fresh” Surface on 596 Scheila as a Consequence of the 2010 Impact Event
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Schelte J. Bus, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Josef Hanuš, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Comparison of 596's NIR spectra before and after the 2010 impact event. The dotted and solid lines show the spectra before and after the impact event, respectively. The figure shows spectra of 596 in the 0.4–2.5 μm wavelength region, normalized to 1 at 0.55 μm. The black and blue arrows in the figure indicate the slope uncertainty from Marsset et al. (2020), and the dispersion range of the spectra obtained by Licandro et al. (2011), centered at the reflectance value of the spectra at 2.35 μm as shown by the black dashed lines.(The data used to create this figure are available.)
Paper: The Appearance of a “Fresh” Surface on 596 Scheila as a Consequence of the 2010 Impact Event
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Schelte J. Bus, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Josef Hanuš, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Comparison of the 3 μm spectra of 596 before and after the 2010 impact event. The dotted and solid lines show the spectra before and after the impact event, respectively. The figure shows the spectra in the 1.8–4.0 μm wavelength regions, normalized to 1 at 2.2 μm.
Paper: The Appearance of a “Fresh” Surface on 596 Scheila as a Consequence of the 2010 Impact Event
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Schelte J. Bus, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Josef Hanuš, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Spectra of the Tagish Lake meteorite. Yellow and cyan areas indicate regions where the slope of the spectrum did not change and regions where it did change after minimum irradiation, respectively.
Paper: The Appearance of a “Fresh” Surface on 596 Scheila as a Consequence of the 2010 Impact Event
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Schelte J. Bus, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Josef Hanuš, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Orbit diagrams of 596 at the time of preimpact NIR observation (left panel) and the 2010 impact event (right panel). Assuming an impact angle of 45°, which is the highest impact probability, the small asteroid would have collided with 596 from the direction (α, δ) = (60°, −40°) (Ishiguro et al. 2011b). The values in blue and red fonts are the values of the two pole solutions of 596 (Hanuš et al. 2021).
Paper: The Appearance of a “Fresh” Surface on 596 Scheila as a Consequence of the 2010 Impact Event
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Schelte J. Bus, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Josef Hanuš, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Spectra of 57 Mnemosyne.
Paper: Parker Solar Probe Evidence for the Absence of Whistlers Close to the Sun to Scatter Strahl and to Regulate Heat Flux
Authors: C. Cattell, A. Breneman, J. Dombeck, E. Hanson, M. Johnson, J. Halekas, S. D. Bale, T. Dudok de Wit, K. Goetz, K. Goodrich, D. Malaspina, M. Pulupa, T. Case, J. C. Kasper, D. Larson, M. Stevens, P. Whittlesey
Figure caption: Comparison of electron parameters when whistlers were not identified within 15 s of the electron measurement (left) and when at least one whistler identified within 15 s (right). (a) and (b): the normalized heat flux, Qnorm, and (c) and (d) β  e,∣∣, plotted vs. radial distance and color-coded by encounter number; (e)–(h) are plotted vs. β  e,∣∣ and color-coded by radial distance; (e) and (f) Qnorm vs. β  e,∣∣ with the Vasko et al. (2019) heat flux fan instability threshold overplotted; (g) and (h) core temperature anisotropy vs. β  e,∣∣ with the temperature anisotropy and firehose instability limits overplotted. The upper dotted line is the temperature anisotropy threshold, and the lower lines are arbitrary firehose resonant (dotted–dashed) and nonresonant (dash) instability (Lacombe et al. 2014, based on Gary and Karimabadi 2006). Note that the right-hand plots in (c) and (d) are for a restricted range of beta.
Paper: Parker Solar Probe Evidence for the Absence of Whistlers Close to the Sun to Scatter Strahl and to Regulate Heat Flux
Authors: C. Cattell, A. Breneman, J. Dombeck, E. Hanson, M. Johnson, J. Halekas, S. D. Bale, T. Dudok de Wit, K. Goetz, K. Goodrich, D. Malaspina, M. Pulupa, T. Case, J. C. Kasper, D. Larson, M. Stevens, P. Whittlesey
Figure caption: Statistics of whistler-mode waves identified in bandpass-filter data. (a) Number of BBF samples in E1 through E9 vs. radial distance, (b) number of BBF samples identified as whistler-mode wave vs. radial distances, and (c) whistler-mode wave occurrence rate vs. radial distance. The red line shows the location where whistler occurrence drops (∼28 R s or ∼0.13 au). (d) Spacecraft frame frequency, f. (e) f/fce. (f) Electric-field amplitude, dE, mV m−1. (g) dE/dB. (h) Magnetic-field amplitude, dB, nT. (i) Ratio of wave magnetic field to background magnetic field, dB/B.
Paper: Parker Solar Probe Evidence for the Absence of Whistlers Close to the Sun to Scatter Strahl and to Regulate Heat Flux
Authors: C. Cattell, A. Breneman, J. Dombeck, E. Hanson, M. Johnson, J. Halekas, S. D. Bale, T. Dudok de Wit, K. Goetz, K. Goodrich, D. Malaspina, M. Pulupa, T. Case, J. C. Kasper, D. Larson, M. Stevens, P. Whittlesey
Figure caption: Encounter 7 comparison of whistler identification. From top to bottom: the radial distance in astronomical units (orange dots indicate BPF data; green are identified as whistlers); wave electric-field amplitude; relevant frequencies, the wave frequency in green, the electron cyclotron frequency, f ce, in blue, 0.3 f ce in yellow, and the lower hybrid frequency, f lh, in red; magnetic field in RTN coordinates, proton speed from SPAN-I, DC-coupled spectra of magnetic field, and electric field 30–5000 Hz, electron energy spectrum and 314 eV pitch angle spectrum.
Paper: Parker Solar Probe Evidence for the Absence of Whistlers Close to the Sun to Scatter Strahl and to Regulate Heat Flux
Authors: C. Cattell, A. Breneman, J. Dombeck, E. Hanson, M. Johnson, J. Halekas, S. D. Bale, T. Dudok de Wit, K. Goetz, K. Goodrich, D. Malaspina, M. Pulupa, T. Case, J. C. Kasper, D. Larson, M. Stevens, P. Whittlesey
Figure caption: Comparison of whistlers auto-identified and the original electric and magnetic field bandpass-filter data for 10 minutes on 2018 November 3. (a) Electric field amplitude, (b) BPF wave magnetic-field amplitude, (c) wave propagation angle, identified whistler wave event frequency overplotted in black on the (d) BPF electric field, (e) electric field spectrum, and (f) BPF magnetic field. White lines represent f lh and 0.2 f ce.
Paper: Parker Solar Probe Evidence for the Absence of Whistlers Close to the Sun to Scatter Strahl and to Regulate Heat Flux
Authors: C. Cattell, A. Breneman, J. Dombeck, E. Hanson, M. Johnson, J. Halekas, S. D. Bale, T. Dudok de Wit, K. Goetz, K. Goodrich, D. Malaspina, M. Pulupa, T. Case, J. C. Kasper, D. Larson, M. Stevens, P. Whittlesey
Figure caption: Location of identified whistler-mode waves in Encounters 1–9. From top to bottom: Radial distance in astronomical unit (orange dots indicate BPF data, green identified as whistlers), wave electric-field amplitude, relevant frequencies, f BW/f EW, and f EW/f ce.
Paper: Parker Solar Probe Evidence for the Absence of Whistlers Close to the Sun to Scatter Strahl and to Regulate Heat Flux
Authors: C. Cattell, A. Breneman, J. Dombeck, E. Hanson, M. Johnson, J. Halekas, S. D. Bale, T. Dudok de Wit, K. Goetz, K. Goodrich, D. Malaspina, M. Pulupa, T. Case, J. C. Kasper, D. Larson, M. Stevens, P. Whittlesey
Figure caption: Wave amplitude vs. wave-propagation angle for Encounter 1 whistlers. From top to bottom: scatter plot of wave amplitude vs. angle, histogram of number of whistlers at a given angle, and average amplitude vs. angle.
Paper: Bursting Bubbles: Clustered Supernova Feedback in Local and High-redshift Galaxies
Authors: Matthew E. Orr, Drummond B. Fielding, Christopher C. Hayward, Blakesley Burkhart
Figure caption: Gas fraction—dynamical time phase space of remnant outcomes, following Equations (9), (12), (13), and (15) from O21. Low-redshift observations are compiled from McKee et al. (2015, Solar Circle estimate), Gallagher et al. (2018, radial gas fractions for NGCs), Leroy et al. (2015, for NGC 253 circumnuclear clump surface densities), Sorai et al. (2000, for molecular gas data in the NGC 253 disk), and rotation curves from Sofue et al. (1999), Chemin et al. (2006), and Dicaire et al. (2008). Intermediate-redshift SMG observational estimates are inferred from Tacconi et al. (2013) and Genzel et al. (2020). Bold NGC points denote detected outflows. Solid orange and light blue regions denote cases where remnants successfully break out of the disk and light-gray and blue-gray regions correspond to cases where the remnant stalls/fragments in the ISM. We also compare with superbubble simulations from Fielding et al. (2018), which overlap in their initial disk and star cluster properties with this model. Insets at right: these simulations are in good agreement with our model, hosting dramatic breakouts in PBO case parameter space and churning stalled bubbles in the PS case parameter space (images are of projected gas density for the simulations from Fielding et al. 2018, adapted from their paper).
Paper: Bursting Bubbles: Clustered Supernova Feedback in Local and High-redshift Galaxies
Authors: Matthew E. Orr, Drummond B. Fielding, Christopher C. Hayward, Blakesley Burkhart
Figure caption: Case boundaries with constant star cluster formation efficiency (per Toomre-mass) assumed for the superbubble model, in the style of Figure 1, in inverse disk surface density–dynamical time phase space, following required adjustments to Equations (9), (12), (13), and (15). In replacing Σcrit → Σ g /ϵ cl, the adjustment to the case boundaries is found by substituting ﹩{\tilde{f}}_{g}\to {\tilde{f}}_{g}/{{\rm{\Sigma }}}_{g}﹩ (i.e., 1/Σdisk). With a constant star cluster formation efficiency, CBO/CF cases remain unlikely to occur given the long dynamical times required (unchanged from fiducial model predictions). In this case, our fiducial model parameters and ϵ cl = 0.01 predict that breakout occurs at lower disk surface densities (almost always <130 M ⊙ pc−2), implying that breakout, i.e., outflows/fountains never occur in the inner disk, contrary to observations. In spite of the outflow detection in NGC 4321 by Castillo-Morales et al. (2007), and the well-known superwind of NGC 253, we would not predict the centers of either NGC 253 or 4321 to host a SN-driven outflow. Instead, this constant efficiency model predicts outflows from solar circle (and more diffuse) disk conditions. Moreover, we would also expect the surface densities in high-redshift SMGs to be such that there are no predicted outflows, contrary to observations from z ∼ 1–3.
Paper: Bursting Bubbles: Clustered Supernova Feedback in Local and High-redshift Galaxies
Authors: Matthew E. Orr, Drummond B. Fielding, Christopher C. Hayward, Blakesley Burkhart
Figure caption: Fragmentation radius as a fraction of disk scale height (for CF/PS cases), and ratio of “effective” to fiducial feedback strength of superbubbles that break out of the disk before t SNe (PBO case) in gas fraction—dynamical time phase space. We color the parameter space by predictions from Equations (17), (18), and (20) in O21, and include the same observational data and case boundary lines as in Figure 1. The light blue region denotes the CBO case where remnant coasts out of the disk but deposits all feedback momentum into the dense gas. Dashed cardinal line indicates division between the CF (coasting fragmentation) and PS (powered stall) cases. We find good agreement with the breakout time and fragmentation scale of the simulations by Fielding et al. (2018). Low-redshift observations suggest that superbubbles in the local universe fragment very near the gas disk scale height (i. e., R  b (t frag)/H ≳ 0.7) and that those which break out deposit as little as ∼10% of feedback momentum locally into dense gas. Whereas, z ∼ 2 galaxies (hatched gray patch) may deposit the majority of their feedback momentum into the ISM, suggesting that the effects of breakout may be significantly different in high-redshift hosts.
Paper: Bursting Bubbles: Clustered Supernova Feedback in Local and High-redshift Galaxies
Authors: Matthew E. Orr, Drummond B. Fielding, Christopher C. Hayward, Blakesley Burkhart
Figure caption: Observed properties of “intact” H I bubbles from (Bagetakos et al. 2011, using THINGS rotation curves from de Blok et al. 2008 to estimate H) in local star-forming galaxies, and their predicted outcomes. Orange and hatched gray regions denote parameter space where the bubbles are expected to have broken out of the ISM disk (R  b  > H) or fragmented within it (v  b  < σ), respectively. Bubble radii and velocities (Equations (7) and (8) O21, see also Section 2.1) are predicted to evolve in ﹩\mathrm{log}{v}_{b}/\sigma ﹩-﹩\mathrm{log}{R}_{b}/H﹩ along lines of constant slope ( − (2 + α)/(2 − α) in log–log space). The dashed line in the “evolving bubbles” portion of parameter space demarcates the superbubbles we predict will fragment within the ISM (PS case) from those that this model predicts will break out of the local gas disk (PBO case). Bolded points indicate superbubbles in regions with inverse dynamical times Ω > 50 Gyr−1 (or t dyn < 20 Myr = t SNe/2), showing that almost all of the “largest” bubbles (relative to local H) have short dynamical times (i.e., in the central regions of galaxies).
Paper: Impact of the SpaceX Starlink Satellites on the Zwicky Transient Facility Survey Observations
Authors: Przemek Mróz, Angel Otarola, Thomas A. Prince, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Michael S. Medford
Figure caption: Starlink streak brightness measurements in three filters used by ZTF, g, r, and i, as a function of the azimuth difference between the center of the trail and the Sun. Magnitudes are scaled to a common range of 550 km. Darker colors (green, red, purple) mark visor-type satellites, lighter colors (turquoise, orange, plum) mark (nonvisor) original design satellites. The mean magnitudes printed in each panel are also reported in Table 2.
Paper: Impact of the SpaceX Starlink Satellites on the Zwicky Transient Facility Survey Observations
Authors: Przemek Mróz, Angel Otarola, Thomas A. Prince, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Michael S. Medford
Figure caption: Fraction of ZTF images with at least one Starlink satellite trail. Black dots (blue squares) mark images taken when the solar elevation was greater than −18° (−30°). Currently, nearly 20% of images taken during twilight are affected.
Paper: Impact of the SpaceX Starlink Satellites on the Zwicky Transient Facility Survey Observations
Authors: Przemek Mróz, Angel Otarola, Thomas A. Prince, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Michael S. Medford
Figure caption: Number of ZTF images with at least one Starlink satellite trail in 10 day bins. The thick red line presents the cumulative number of deployed satellites.
Paper: Turbulence and Particle Acceleration in a Relativistic Plasma
Authors: Cristian Vega, Stanislav Boldyrev, Vadim Roytershteyn, Mikhail Medvedev
Figure caption: The magnetic and electric spectra in the 2D runs with different magnetizations (runs III & IV). The spectrum of the electric field approaches that of the magnetic field at small scales as the plasma magnetization increases. The lines indicating power laws are given for reference.
Paper: Turbulence and Particle Acceleration in a Relativistic Plasma
Authors: Cristian Vega, Stanislav Boldyrev, Vadim Roytershteyn, Mikhail Medvedev
Figure caption: The magnetic-field strength distribution functions and the corresponding magnetic compressibilities κ. The distribution is independent of the magnetization parameter, but depends on the relative strength of the applied magnetic field.
Paper: Turbulence and Particle Acceleration in a Relativistic Plasma
Authors: Cristian Vega, Stanislav Boldyrev, Vadim Roytershteyn, Mikhail Medvedev
Figure caption: The particle energy distribution functions in runs I, II (top), III, IV (middle), and V, VI (bottom panel). The lines indicating power-law slopes are given for reference.
Paper: Predicting the Water Content of Interstellar Objects from Galactic Star Formation Histories
Authors: Chris Lintott, Michele T. Bannister, J. Ted Mackereth
Figure caption: Water-rich (﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}\gt 0.4﹩) ISO fraction as a function of galaxy median age for 2039 galaxies with 1010 < M ⋆ < 1011 M ⊙ from the Ref-L100N1504 EAGLE volume. Points are colored by the mean stellar iron abundance relative to hydrogen, [Fe/H], as a proxy for the overall metallicity; as expected, this quantity is linked to the star formation history. There is a clear trend between median stellar age and water-rich ISO fraction such that galaxies with older stellar populations harbor more water-rich ISOs.
Paper: Predicting the Water Content of Interstellar Objects from Galactic Star Formation Histories
Authors: Chris Lintott, Michele T. Bannister, J. Ted Mackereth
Figure caption: Top: star formation histories of two example galaxies (at fixed stellar mass) selected from EAGLE to demonstrate the ISO population predicted in a galaxy with recent star formation (blue) vs. one with earlier star formation (yellow). Bottom: predicted water mass fractions of ISO populations predicted for the galaxies shown above. The histograms are normalized such that p(H2O mass fraction) is the probability density for finding an ISO in a given mass fraction bin or equivalently the fraction of the predicted ISO population in each bin.
Paper: Predicting the Water Content of Interstellar Objects from Galactic Star Formation Histories
Authors: Chris Lintott, Michele T. Bannister, J. Ted Mackereth
Figure caption: Top: predicted distribution of ISO objects by water-mass fraction. As before, the histograms are normalized such that p(H2O mass fraction) is the probability density for finding an ISO in a given mass fraction bin or equivalently, the fraction of the predicted ISO population in each bin. The gray regions lie outside the formal limits of the BB20 model; here we assume that predicted ISOs have the minimum or maximum possible water mass fraction. Bottom: as above, but split by age of population. The low water-mass fraction population is dominated by the youngest objects, while the population with high water-mass fraction is from older systems.
Paper: Col-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations
Authors: Laura E. Buchanan, Megan E. Schwamb, Wesley C. Fraser, Michele T. Bannister, Michaël Marsset, Rosemary E. Pike, David Nesvorný, J.J. Kavelaars, Susan D. Benecchi, Matthew J. Lehner, Shiang-Yu Wang, Nuno Peixinho, Kathryn Volk, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Stephen Gwyn, and Jean-Marc Petit
Figure caption: Optical and NIR colors of the Col-OSSOS E, H, and L observing blocks. The object 2013 UQ15 (orange circle) is dynamically consistent with the Haumea collisional family. The green circles represent the hot classical KBOs, the pale gray crosses are the cold classicals, the purple triangles are the MMR objects, the red pentagrams are the scattering disk KBOs, the black diamond is a detached TNO, and the yellow square is a Centaur. The solar colors, with g − r = 0.45 and r − J = 0.97, are shown by the yellow star. The vertical red dashed line shows the split between red and neutral surface colors at (g − r) = 0.75.
Paper: Col-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations
Authors: Laura E. Buchanan, Megan E. Schwamb, Wesley C. Fraser, Michele T. Bannister, Michaël Marsset, Rosemary E. Pike, David Nesvorný, J.J. Kavelaars, Susan D. Benecchi, Matthew J. Lehner, Shiang-Yu Wang, Nuno Peixinho, Kathryn Volk, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Stephen Gwyn, and Jean-Marc Petit
Figure caption: Schematic of the primordial outer solar system before giant planet migration. It consists of two gas giant and three ice giant planets as in the dynamical model of Nesvorný & Vokrouhlický (2016), with Neptune being the outermost planet. The primordial planetesimal disk from which the dynamically hot population originated is represented by the gray boxes and ranges from 24 to 30 au. It is split into the inner and outer primordial disk.
Paper: Col-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations
Authors: Laura E. Buchanan, Megan E. Schwamb, Wesley C. Fraser, Michele T. Bannister, Michaël Marsset, Rosemary E. Pike, David Nesvorný, J.J. Kavelaars, Susan D. Benecchi, Matthew J. Lehner, Shiang-Yu Wang, Nuno Peixinho, Kathryn Volk, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Stephen Gwyn, and Jean-Marc Petit
Figure caption: Barycentric orbital parameters, derived from Bannister et al. (2018), of TNOs with Col-OSSOS surface colors presented in this paper. One TNO at a = 150 au in H block is omitted for better resolution. The 1σ uncertainties are smaller than the size of the plot symbol. The colors of the points represent the object’s surface colors (as defined in Section 2), with red indicating red surfaces and blue indicating neutral surfaces.
Paper: Col-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations
Authors: Laura E. Buchanan, Megan E. Schwamb, Wesley C. Fraser, Michele T. Bannister, Michaël Marsset, Rosemary E. Pike, David Nesvorný, J.J. Kavelaars, Susan D. Benecchi, Matthew J. Lehner, Shiang-Yu Wang, Nuno Peixinho, Kathryn Volk, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Stephen Gwyn, and Jean-Marc Petit
Figure caption: Col-OSSOS photometry of observed nonresonant, non-Centaur, dynamically excited objects in the E, H, and L observing blocks. The red/neutral color split is placed at a (g − r) magnitude of 0.75. The color distribution of the objects before these cuts in the E, H, and L blocks is shown in Figure 1. The star shows solar colors.
Paper: Col-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations
Authors: Laura E. Buchanan, Megan E. Schwamb, Wesley C. Fraser, Michele T. Bannister, Michaël Marsset, Rosemary E. Pike, David Nesvorný, J.J. Kavelaars, Susan D. Benecchi, Matthew J. Lehner, Shiang-Yu Wang, Nuno Peixinho, Kathryn Volk, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Stephen Gwyn, and Jean-Marc Petit
Figure caption: Barycentric orbital parameters, derived from Bannister et al. (2018), of observed nonresonant, non-Centaur, dynamically excited objects in the E, H, and L observing blocks. Blue circles represent those objects with neutral-colored surfaces ((g − r) < 0.75), red triangles are the objects with red surfaces ((g − r) ≥ 0.75), and the gray square represents the KBO within the sample with no Col-OSSOS observations.