adsabs/AstroCLIMB huggingface dataset:
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: An example of the O2 cross sections and their associated k-tables, shown here for a single point in the temperature-pressure grid (200 K and 100 hPa; near tropopause). The blue curve shows the wavenumber-dependent cross sections; black curves show the k-table distributions. Vertical gray lines indicate the boundaries of the k-table bins. The gray shading indicates bins that are included only in the n84equiv configuration. Cross sections at higher wavenumbers than shown here are zero.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Comparison of ExoRT (1D mode), RRTMG, and SMART for the Control case (with O2 and O3). The top row shows the upward and downward beams in the SW and LW. The second row shows the difference between the correlated-k models and SMART for the upward and downward beams. The third row shows the net fluxes and heating rates in the SW and LW. Finally, the bottom row shows the difference between the correlated-k models and SMART for the net fluxes and heating rates.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: An example of the O3 cross sections and k-tables, shown here for a single point in the temperature-pressure grid (200 K and 100 hPa; near tropopause). The blue curve shows the wavenumber-dependent cross sections; black curves show the k-table distributions. Vertical gray lines indicate the boundaries of the k-table bins. The gray shading indicates bins that are included only in the n84equiv configuration. Cross sections at higher wavenumbers than shown here are zero.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Top-of-atmosphere spectra for our 1D Control case and Case A, from SMART and ExoRT. The full high-resolution output from SMART is shown in gray; blue points are binned to the resolution of ExoRT's n68equiv configuration. The top row shows the absorbed solar radiance, i.e., the downward SW beam—the upward SW beam. The second row shows the difference between ExoRT and SMART after binning. The third row shows the LW outgoing radiance, and the fourth shows the difference between ExoRT and SMART in the LW.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Input temperatures, humidities, and O3 and CH4 mixing ratios for our 1D comparison of ExoRT, RRTMG, and SMART. Gas abundances in the right panel are shown as mass mixing ratios.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: An example of the O2 CIA cross sections and band-averaged values, shown here at a temperature of roughly 295 K, for the three CIA interactions. Blue curves indicate the measured cross sections as a function of wavenumber; black indicates the band-averaged values used in ExoRT.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Same as Figure 5 but for Case A (no O2 or O3).
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Net SW and LW fluxes at the surface and the outgoing LW flux (top of atmosphere) for our four 1D calculations with ExoRT, RRTMG, and SMART.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Comparison of the SW radiation in SMART and ExoRT with varying wavelength limits for the SW. The first and second columns correspond to SMART output, with a 0.24 μm and a 0.1 μm cutoff. The third and fourth columns correspond to ExoRT output, with a ∼0.24 μm cutoff (n68equiv) and a 0.008 μm cutoff (n84equiv). Panels are arranged similar to Figure 5, with upward and downward beams in the top row, net fluxes and heating rates in the third, and differences in the second and fourth.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Zonal mean temperature, specific humidity, zonal wind speed, and relative humidity from ExoCAM and standard CAM4 simulations. The top row shows the ExoCAM PAL O2 and O3 simulation; the second row shows the corresponding CAM4 simulation. The third row shows the zero O2 and low O3 simulations in ExoCAM; the fourth shows the corresponding low O3 simulation in CAM4.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Same as Figure 11; zonal mean cloud fraction, ice cloud density, and liquid cloud density zoomed-in on the troposphere and lower stratosphere. Cloud densities below 10−12 kg m−3 are nulled.
Paper: Oxidizing ExoCAM: Introducing the Radiative Effects of Oxygen and Ozone into the ExoCAM General Circulation Model
Authors: Russell Deitrick, Colin Goldblatt, Eric T. Wolf, Tyler D. Robinson
Figure caption: Globally and temporally averaged properties from ExoCAM and CAM4 simulations. The temperature, cloud fraction, specific humidity (or MMR of water vapor), ice cloud density, relative humidity, and liquid water density are shown as a function of pressure.
Paper: Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer
Authors: Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer
Figure caption: Views of Io. (a) Pioneer 11 image of Io captured on 1974 December 2 from a distance of 756,000 km (Credit: NASA/JPL). (b) Loki and Loki Patera shown in a Voyager 1 image mosaic (Credit: NASA/JPL/USGS). (c) Magnified view of part of a Galileo color image of Io (11.8 km pixel−1) captured on 1999 July 2. This image shows Pele, a small lava lake that has produced a large red ring that reaches as far as 600 km from the central vent, with overprinting by a recent dark tephra deposit from Pillan Patera (Credit: NASA/JPL/NOAO/Jason Perry). (d) Galileo view of Prometheus, which includes a large lava flow field and secondary plumes associated with lava–sulfur frost interactions along the flow’s margin (Credit: NASA/JPL). (e) Galileo view of Hiʻiaka Montes. The dark area near the center of this “pull-apart” mountain is a wide volcanic crater called a patera. (Credit NASA/JPL). (f) Galileo acquired its highest-resolution images of Jupiter’s moon Io on 1999 July 3 during its closest pass to Io since orbit insertion in late 1995. This color mosaic uses the near-infrared, green, and violet filters to approximate “true color” (i.e., what the human eye would see). Most of Io’s surface has pastel colors, punctuated by black, brown, green, orange, and red units near the active volcanic centers. (g) New Horizons image of Io, showing a large volcanic plume erupting from Tvashtar (Image: PIA09248; credit: NASA/APL). (h) Loki and Loki Patera shown in a Juno image captured during its 57th flyby of Jupiter, in 2023 December (Image: PJ57; credit: NASA/JPL-Caltech/SwRI/MSSS/Kevin M. Gill). Note that in panels (f) and (g), north is toward the top of the page, whereas the Juno image shown in panel (h) looks toward the north pole and the northern hemisphere.
Paper: Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer
Authors: Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer
Figure caption: Constraints on Io’s average lithospheric thickness and rigidity based on measurements of k2, magnetic induction, and libration amplitude. IVO would precisely determine average lithospheric thickness and rigidity, which—combined with new magnetic induction measurements—would provide the constraints necessary to assess whether or not Io has an internal magma ocean (J. T. Keane et al. 2022). Use of multiple independent constraints is one of the most powerful techniques in geophysics.
Paper: Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer
Authors: Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer
Figure caption: Conceptual models for the interior of Io, depending on where the bulk of tidal dissipation occurs (after K. de Kleer et al. 2019a; D. Breuer et al. 2022).
Paper: Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer
Authors: Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer
Figure caption: The normalized response of Io (i.e., ratio of the induced polar field at Io’s surface to the strength of the inducing field) for a range of magma-rich layer thicknesses for six periods ranging from 4.3 hr to 4 weeks.
Paper: Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer
Authors: Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer
Figure caption: Measurements of (a) tidal k2, (b) libration amplitude, and magnetic induction provide independent tests for a magma ocean (see Figure 3). Tidal k2 and the peak-to-peak libration amplitude of Io are calculated assuming an elastic lithosphere overlying a magma ocean (T. Van Hoolst et al. 2020). Io’s lithosphere is expected to be rigid (>30 GPa) and surprisingly thick (10–50 km) based on the volcanic heat-pipe model and to support mountains up to 17 km high. The peak-to-peak libration amplitude is 2 times the typically quoted value of displacement from the mean. Multifrequency magnetic sounding will measure the thickness of Io’s lithosphere and constrain models for the thickness and conductivity of the magma-rich layer.
Paper: Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer
Authors: Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer
Figure caption: Sources of enhanced thermal emission on Io. Io is an extremely active volcanic world with over 343 active thermal sources, nearly all of which are more energetic than the most active eruptions on Earth today. For example, Kīlauea Volcano, on the island of Hawaiʻi, has a mean energy output of <1 GW, which is less than nearly all volcanic systems on Io. (a) Global Voyager–Galileo global mosaic for Io, with the locations of key volcanic systems discussed in the text. (b) Thermal emission (i.e., heat flux) for volcanic systems on Io (A. G. Davies et al. 2024b, 2025).
Paper: A Convolutional Neural Network–Based Approach for Detecting Solar System Objects in Wide-field Imaging
Authors: Aram Lee, J. J. Kavelaars, Hossen Teimoorinia, Wesley Fraser, Edward Ashton
Figure caption: Right Panel: Points show the 500 random sky locations of subimages used for training and testing (differs for each CCD). Left Panel: Points show the grid of subimage centers used for the search.
Paper: A Convolutional Neural Network–Based Approach for Detecting Solar System Objects in Wide-field Imaging
Authors: Aram Lee, J. J. Kavelaars, Hossen Teimoorinia, Wesley Fraser, Edward Ashton
Figure caption: A labeled image pair with positives on each side. This pair represents a simple case, as no stars overlap with the TNO, and the noise level is low. The orange circles indicate the positions of the synthetic TNOs.
Paper: Unoccupied Aircraft Systems Sampling for Earth and Mars
Authors: Colin Chen, Christopher W. Hamilton, Christian Sipe, Kathryn Bywaters, Justin Lawrence, Paul Creekmore, Nicklaus Traeden, Kris Zacny
Figure caption: Drill (a) and scoop (b) UAS sampling systems.
Paper: From Colors to Spectra and Back Again: First Near-IR Spectroscopic Survey of Neptunian Trojans
Authors: Larissa Markwardt, Hsing Wen Lin, 省文 林, Bryan J. Holler, David W. Gerdes, Fred C. Adams, Renu Malhotra, Kevin J. Napier
Figure caption: PC1 versus optical (S′) and near-IR slope (SIR1). Each NT is depicted with a unique color marker in the plots. The dashed lines in panel (a) demark S′ = 17 and 24%/1000 Å, our proposed borders to separate the three major spectral groups. The dashed line in panel (b) demarks SIR1 = 3.5%/1000 Å, our proposed border to separate the shallow NIR and steep NIR slope subtypes of bowl-type objects.
Paper: From Colors to Spectra and Back Again: First Near-IR Spectroscopic Survey of Neptunian Trojans
Authors: Larissa Markwardt, Hsing Wen Lin, 省文 林, Bryan J. Holler, David W. Gerdes, Fred C. Adams, Renu Malhotra, Kevin J. Napier
Figure caption: The joint optical photometry and NIRSpec spectra of eight NTs. Each plot color corresponds to a different NT, while the circular markers correspond to the central wavelengths of different optical bands (from short to long wavelength: g, r, i, z or B, V, R for 2011 WG157). The error bars and shaded regions represent the 1σ uncertainties on the optical photometry and NIR spectra, respectively. References for the optical photometry data: 2011 WG157 from D. Jewitt (2018), 2011 HM102 from A. H. Parker et al. (2013), 2008 LC18 from B. T. Bolin et al. (2023), and others from L. Markwardt et al. (2023).
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The (a) time evolution and (b) cohesion dependence of the simulated momentum enhancement, β, from impacts on a curved asteroid with a homogeneous interior. (c, d) Same as panel (a) and (b), but for the diameter of the impact crater. Colored solid lines show different cohesive strengths for the target asteroid. The gray shading and black solid line indicate the reference DART impact β range and its mean value from A. F. Cheng et al. (2023). The circles in panels (b) and (d) correspond to the values of β and crater diameter at the final simulated time step in panels (a) and (c), respectively. While craters continue to grow in panel (d), as indicated by the increasing trends in panel (c), the β trends demonstrate an approaching convergence.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The time evolution of the simulated (a) momentum enhancement efficiency, β, and (b) crater diameter, from impacts on a curved asteroid with a homogeneous interior. Colored solid lines depict different internal friction values for the target asteroid, Dimorphos. The gray shading and black solid line indicate the reference DART impact β range and its mean value from A. F. Cheng et al. (2023). Note that as the β factor continues to grow, the case with the internal friction of f = 0.5 is shown up to t = 60 s after impact in Figure 2.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The time evolution of the momentum enhancement β from impacts on a curved asteroid with a homogeneous interior (assuming Y0 = 1 Pa and the internal friction of f = 0.50) as a function of porosity, ϕ: (a) 10%, (b) 20%, (c) 30%, (d) 40%. (e) Same as panels (a)–(d), but for the impact crater diameter. (f) Simulated β values at t = 45 s as a function of the bulk density of Dimorphos, as displayed by downward-pointing triangles and connected with a purple dashed line, illustrate the relative effects of the target porosity. The gray shading and black solid line indicate the reference range and its mean value from the DART impact β reconstructions (A. F. Cheng et al. 2023). The circle and upward-pointing triangle mark the converged β values of Y0 = 50 Pa and Y0 = 500 Pa (case 07 and case 08, respectively) from Figure 2(a). The blue dashed line depicts the relative effects of the cohesion Y0 for f = 0.50 and ϕ = 30%.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Vertical positioning of a single boulder before impact (t = 0 s) for (a) a half-buried (z/rb = +1.0) boulder and (b) a subsurface (z/rb = −0.5) boulder located along the symmetry axis of a 2D axisymmetric spheroidal target. The resulting crater morphology at t = 15 s post-impact is displayed for (c) the half-buried and (d) the subsurface boulder cases. The color bar indicates the density map in units of kg m−3. The light-blue sphere above the asteroid at r = 0 m represents the DART projectile before the impact (t = 0 s). The boulder in dark blue corresponds to the low (10%) porosity. The regolith strength is set to a low cohesion (Y0 = 1 Pa), 30% porosity, and an internal friction of f = 0.5, similar to case 02 in Table 2. The time evolution of the simulated (e) momentum enhancement factor, β, and (f) crater diameter for different burial depths of a central boulder, for DART-scale impacts. The gray shading and black solid line indicate the reference range of β and its mean value from A. F. Cheng et al. (2023).
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The normalized ejecta mass, velocity, and launch-position profiles for DART-scale impacts on a single boulder with varying burial depths (cases 11–15 in Table 3) relative to the no-boulder setup (case 02 in Table 2) at t = 15 s. The variation of the cumulative ejecta mass normalized by the projectile mass along with (a) the total ejecta velocity, v, normalized by the impact velocity, U, and (b) the radial position normalized by the impactor radius. The black solid line shows the ejecta profiles for the no-boulder homogeneous setup, while the shades of blue depict the heterogeneous setup involving a single central boulder located along the symmetry axis of a 2D axisymmetric spheroidal target.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: (a) The vertical component of the ejecta velocity normalized by the impact speed (panels (a), (c), (e), (g), (i), (k)) and the ejecta angle (panels (b), (d), (f), (h), (j), (l)), along with the radial position normalized by the impactor radius for the cases of Figure 5 at t = 15 s, as specified in the respective legends.
Paper: Determinations of Asteroid Masses Using Mutual Encounters Observed in the Legacy Survey of Space and Time
Authors: Gary M. Bernstein, Negin Najafi, Daniel C. H. Gomes
Figure caption: The results of the search for useful deflector-tracer encounters among MBAs in a simulated LSST are plotted vs. the absolute magnitude H of the deflector. The left plot gives the number of encounters producing impulses I > 2 × 10−6 m s−1 for each unique deflector. This number is well above unity for H ≲ 10.5, if we assume the high-M/L value of M10. This is despite the fact that we retain only encounters with impact parameter b < 0.1 au. The right plot’s blue histogram shows, in bins of 0.5 mag in H, the total number of known MBAs at a < 5 au. In orange (dashed green) is the histogram of those MBAs that perturb at least one tracer with an impulse >2 × 10−6 m s−1, assuming the high (low) M/L value for M10. As expected from the left plot, all of the 725 MBAs at H ≲ 10 generate an impulse above this threshold on a known tracer during the LSST. Among the fainter/smaller bodies at H > 10, not all generate an above-threshold impulse, but some fraction of them is “lucky” in that they encounter a tracer with small enough impact parameter and velocity. In this way, an incomplete but random selection of MBAs at H > 10 are candidates for mass measurement, outnumbering the complete sample at H < 10. Assuming the lower-M/L value for all MBAs shifts the completeness curve to brighter H, as expected.