adsabs/AstroCLIMB huggingface dataset:
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Comparison between our MP1 SfS DTM and MMDTM2024. (a) and (b) Colorized elevations underlain by shaded reliefs for (a) our DTM (same as Figure 9(e)) and (b) MMDTM2024 (malapert_massif-tile-0.tif; B. Boatwright 2024). (c) Signed difference (ours − MMDTM2024) with colorized intervals of 1 m. (d) and (e) Close-ups (red dashed boxes in panels (a) and (b)) of shaded relief for (d) our DTM and (e) MMDTM2024. The magenta polygon outlines the MP1’s ROI.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Differences in elevation between individual SfS DTMs and SPLDEM2021. (a) CR1 SfS DTM − SPLDEM2021 at Site01, (b) GR1 SfS DTM − SPLDEM2021 at Site11, (c) GR2 SfS DTM − SPLDEM2021 at SL3, (d) LP1 SfS DTM − SPLDEM2021 at Site20, (e) MP1 SfS DTM − SPLDEM2021 at Site23, (f) MP2 SfS DTM − SPLDEM2021 at Site23. NoData pixels are not rendered, allowing the black backgrounds to remain visible. Their statistics are listed in Table 7. The spatial extents and polygons are the same as those in Figure 9.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Log–log plots showing rms bidirectional slopes derived from each SfS DTM. Slopes are based on their elevation profiles in sample (left) and line (right) directions. The baseline lengths that we used to calculate slopes are 1, 2, 4, 8, 16, 32, 64, 128, 256, and 512 m for each SfS DTM and 5, 10, 20, 40, 80, 160, 320, 640, and 1280 m for a 5 m pixel−1 LDEM. As a reference to the slopes of CR1, we add those derived from both LDEM (LOLA GDR) and SPLDEM2021, two of which were clipped by the shape of CR1’s polygonal ROI.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Histogram of the difference in elevation between each DTM and LOLA RDR point. Each histogram corresponds to each of the ROI maps in Figure 16, including points outside its polygonal area. The width of each bin is 1.0 m.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Height-uncertainty maps of the SfS DTMs. Height-uncertainty pixels are colorized in a range from 0 to 0.50 m at intervals of 0.05 m. NoData pixels are not rendered, allowing the black backgrounds to remain visible. The spatial extents and white polygons are the same as those in Figure 9.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Histograms of height uncertainties of the SfS DTMs. All valid (non-NoData) pixels are counted from the individual DTMs (Figure 13; the pixels outside the white polygons are included in the histograms). Each of the major statistical values is summarized in Table 5. The count axis is log scale. Histogram bins are shown at intervals of 0.1 m. The MP2 cumulative fraction of height-error values at [0.0, 0.1) is 88.04%.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Combinations of measurement relative precisions allowing us to measure the ocean thickness (do), the rock-to-ice ratio (rock/ice), and the ice shell thickness (ds) with a given uncertainty level when the satellites have an ocean of 20 km depth. The combinations shown are the ones that have the maximum L2-norm (loosest measurement requirements) and that achieve the desired level of uncertainty.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Ocean thickness dependence of required precision quadruplets (marked with gray frames) in Ariel's geodetic observables, relative to our do = 20 km nominal case. These uncertainties in the MoI, k2, gs, and ε are selected such that one can determine the ocean thickness itself (do) and the rock-to-ice ratio (rock/ice) at the 30% level and the ice shell thickness (ds) at the 5% level. For the case with no ocean (do = 0 km), the ﹩{\sigma }_{{\rm{MoI}}},{\sigma }_{{k}_{2}},{\sigma }_{{g}_{s}}﹩, and σε are selected such that do can be inferred with an uncertainty of 30 km, which makes this case not readily comparable to the others, but nonetheless quite instructive. The quadruplets are the ones with the maximum L2-norm among all possible combinations.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Alternative quadruplets allowing us to measure the ocean thickness (do) and the rock-to-ice mass ratio (rock/ice) with a 30% uncertainty level, and the ice shell thickness (ds) at 5% when the satellites have an ocean of 20 km depth. These combinations all have one or more geodetic parameters with 100% uncertainty. Each colored dotted line represents a quadruplet. The red solid lines indicate the solutions presented in Figure 1 for the nominal case.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Alternative measurement combinations to determine together the three internal parameters (ocean thickness (do), rock-to-ice ratio (rock/ice), and ice shell thickness (ds)) with a specified degree of uncertainty for a satellite with an ocean depth of 20 km. These combinations are characterized by one observable having the loosest possible requirement, whereas the others have a requirement greater than 10−3. The absence of lines indicates that no combination has been identified.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Required relative precisions on MoI, k2, gs, and ε to determine all three interior parameters (do, rock/ice, and ds) with a specified degree of uncertainty for a satellite with an ocean depth of 20 km. The relative precisions are set to be equal for each interior parameter. The combination shown is the one with the maximum L2-norm among all possible combinations.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: UOP flybys of Ariel (±30 minutes around C/A). Colors show the altitude with respect to the moons’ surface, whereas the crosses show the point of C/A. Only flybys with a C/A distance less than three body radii are shown.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Total coverage map, overlaid on Cassini ISS imaging of Titan (NASA/JPL-Caltech/Univ. Arizona). Each objective corresponds to a specific-colored polygon on the map, indicating total minimum coverage required for that objective across instruments. Several regions of interest are annotated on the map.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Two possible scenarios of Titan’s liquid coverage at roughly 1 Gya. Black is liquid coverage, and color shows exposed ice shell and its relative elevation, where dark red indicates higher elevation and dark blue indicates lower elevation. On the left-hand side is the scenario wherein Titan was covered by a global hydrocarbon ocean in the past, and has since lost liquid coverage to reveal the surface seen today. Alternatively, if the body has not been losing surface liquids, the coverage would have been stable for the past 1 Ga (Adapted from R. Larsson & C. P. McKay 2013).
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: (a) Comparison of the elevation and composition gradients for the Truckee River System spanning California and Nevada, USA on Earth. (b) Elevation and composition gradients for a scenario in which Titan’s lakes and mare experience material exchange through a subsurface alkanifer, with ethane-methane clathrate substitution occurring analogous to subsurface chemical processing resulting in enhanced pCO2 levels downstream in Earth rivers. (c) Elevation and composition gradients for a scenario in which Titan’s lakes and mare are not connected by a subsurface reservoir.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Data sufficiency by objective. Each objective, described above, will be fully answerable by THUNDER’s proposed mission. This figure summarizes the necessary instrumentation, coverage, and data volume. Schematic figures of each physical parameter are shown in the bottom row, indicating end-member cases that can be differentiated using THUNDER’s results.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Comparison of the SAR resolution achieved by Cassini RADAR over a subset of Titan's surface (left-hand side) and the SAR resolution THUNDER will achieve (right-hand side). Figure modified from J. W. Miller et al. (2021), where full Cassini resolution is mapped over the entire globe. THUNDER will achieve a ≤125 m px−1 resolution over the entire surface.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Payload Accommodation Requirements Imposed by Instrumentation
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: THUNDER ConOps: Spacecraft pointing directions and day/night side measurement capabilities for operational modes 1–4 (top); example duty cycle for a 6-orbit ConOps cycle (bottom).
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Planned THUNDER Cruise Phase trajectory from launch to Saturn orbital insertion. Dates of flybys are listed, and planets are marked by numbers.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Instrument Capabilities Compared to Mission Science Requirements. All are shown at 1300 km altitude and with time binning on ground.
Paper: A Case Study of Interstellar Material Delivery: α Centauri
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The heliocentric equatorial radiant for the 350 close approaches at the time of their closest solar approach (“Arrival Time”), with the current heliocentric equatorial coordinates of α Cen plotted as a black star, and the “effective radiant” corresponding to α Cen’s apparent velocity is plotted as a red star. The purple shaded region is the combined projection of the effective cross section of the solar system (solid angle size as seen from α Cen), from the start of the simulation up to the current time (t ≈ 0 yr). The left figure views the entire CA population while the right figure zooms into the region surrounding α Cen’s effective radiant.
Paper: A Case Study of Interstellar Material Delivery: α Centauri
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The relative travel distance (the distance a particle travels with respect to α Cen) vs. travel time of the α Cen material that enter our Oort cloud. The left figure shows the total distribution while the right zooms into the most common times.
Paper: A Case Study of Interstellar Material Delivery: α Centauri
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The ejection velocities vs. time of ejection of the α Cen material that enter our Oort cloud. The left figure shows the total distribution while the right zooms into the most common times.
Paper: A Case Study of Interstellar Material Delivery: α Centauri
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The apparent velocities of the α Cen material that cross our Oort cloud. The left figure shows the total distribution while the right zooms into the most common speeds.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Top panels: Erigone family projected onto 2D planes in proper element space: (i) semimajor axis aP vs. eccentricity eP (top left), and (ii) semimajor axis aP vs. sine of inclination ﹩\sin {I}_{P}﹩ (top right). Black circles are for all 4925 members identified at the HCM cutoff velocity 32.5 m s−1. Color-coded symbols highlight special subgroups of the whole sample: blue circles are 834 low-albedo members (pV < 0.125), red triangles are 55 high-albedo members (pV > 0.125), and cyan circles are members in the z2 secular resonance (for which ∣z2∣ < 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩3 yr−1). The locations of Erigone and DJ are highlighted with black and green stars, respectively. The vertical gray line shows the location of exterior mean motion resonance 1/2 with Mars (M1/2), and the dashed gray curve in the top left panel locates orbits with perihelion q = 1.82 au (approximate limit where the population becomes efficiently depleted by Mars encounters). Bottom left panel: Erigone family members projected onto the plane defined by the proper semimajor axis aP (abscissa) and absolute magnitude H (ordinate). The same color-coding is used as in the top panels. The vertical dashed line shows the center of the family (ac = 2.3695 au), and the two solid gray curves show the limiting ∣C⋆∣ = 1.7 × 10−5 au lines defined by maximum conjoint contrast r(C⋆, ac; ΔC) (see Equations (1) and (A3)), while the dashed gray curves correspond to ∣Cfam∣ = 1.95 × 10−5 au, the limit used for Yarkovsky/YORP chronology modeling. Formal members with H smaller than H⋆ at the critical lines, for a given aP value, are deemed unrelated interlopers in the family. Bottom right: distribution of H ≤ 17.5 mag Erigone members dN(C) with ∣C∣ ≤ Cfam values binned with ΔC = 1.5 × 10−6 au intervals; only WISE-identified dark asteroids are used in this data set. The black symbols, with formally adopted ﹩\sigma (C)=\sqrt{dN(C)}﹩ uncertainty, are raw data. The gray symbols at C ≥ 0 values mirror the C ≤ 0 distribution.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Top left: geometric albedo values pV, with formal uncertainties, determined for 889 Erigone family members by analysis of WISE observations. The sample is dominated by 834 dark objects (pV < 0.125) shown by black symbols. The albedo values for a bright group (55 objects with pV > 0.125) are shown using gray symbols (some would fall even beyond the upper limit 0.25 of the plot). DJ’s value is shown in green. The horizontal gray line at ﹩\bar{{p}_{V}}=0.054﹩ indicates the median value of the dark sample. Note that the largest objects (D > 10 km) have systematically ﹩{p}_{V}\lt \bar{{p}_{V}}﹩. Bottom left: cumulative size distribution of Erigone family members; the red curve is for all 4925 members assigning to all median WISE albedo ﹩\bar{{p}_{V}}=0.054﹩ for the dark sample and adopting their absolute magnitudes, and the blue curve is for the distribution of size for 834 members with WISE dark albedo. DJ's location is marked by the green symbol. The gray lines are approximations with power-law distribution N( > D) ∝ D−α in the 4–10 km range, with α ≃ 3.63 for the whole population (red) and α ≃ 3.50 for the WISE subsample (blue). The horizontal dashed lines correspond to the H = 17.5 mag limit. This is unique for the whole sample in red (where sizes are computed from magnitudes using a fixed albedo value), while H = 17.5 asteroids are in a certain range in the WISE sample, because individual objects have slightly different pV values. Right panel: distribution of dN(C) binned with ΔC = 1.5 × 10−6 au intervals for H ≤ 17.5 mag Erigone members (formal ﹩\sqrt{dN(C)}﹩ uncertainties shown by the vertical bar); the blue symbols are for the subsample of asteroids with WISE-determined pV < 0.125 albedo values and ∣C∣ ≤ Cfam (the same as the black symbols in the bottom right panel of Figure 2), and the red symbols are for all Erigone members. The black line is simply the blue distribution multiplied by a factor 1.9. A good match to the total population suggests (i) a small fraction of bright interlopers in the Erigone family up to the H = 17.5 mag limit and (ii) that there is a 1.9 incompleteness factor of the WISE-observed sample. The mismatch for C < −20 × 10−5 au is likely due to contamination by bright objects transported along the z2 secular resonance.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Top panel: distribution of the Erigone family age T from a set of simulations in which all parameters p2 = (ρ, Γ, τ0) uniformly sampled the following interval of values (gray histogram with black outline): (i) ρ ∈ (1.2, 1.7) g cm−3, (ii) Γ ∈ (115, 710) SI, and (iii) τ0 ∈ (0.5, 100) Myr (the last two in log-measure). The median age is 186 Myr. The color-coded distributions are for subsamples characterized by distinct bulk densities: (i) ρ ∈ (1.2, 1.275) g cm−3 (red), (ii) ρ ∈ (1.275, 1.355) g cm−3 (green), (iii) ρ ∈ (1.355, 1.44) g cm−3 (blue), (iv) ρ ∈ (1.44, 1.52) g cm−3 (cyan), (v) ρ ∈ (1.52, 1.61) g cm−3 (magenta), and (vi) ρ ∈ (1.61, 1.7) g cm−3 (yellow). All distributions are normalized by the maximum of the total distribution. The lower-density solutions imply a smaller family age. Bottom panel: distribution of the Erigone family age T from a set of simulations in which bulk density was fixed to 1.3 g cm−3, but with the remaining two parameters p2 = (1.3, Γ, τ0) sampling the following interval of values (gray histogram with black outline): (i) Γ ∈ (118, 650) SI, and (ii) τ0 ∈ (0.5, 100) Myr (both in log-measure). The color-coded distributions are for subsamples characterized by distinct values of the thermal inertia (all in SI units): (i) Γ ∈ (115, 150) (red), (ii) Γ ∈ (150, 200) (green), (iii) Γ ∈ (200, 268) (blue), (iv) Γ ∈ (268, 350) (cyan), (v) Γ ∈ (350, 470) (magenta), and (vi) Γ ∈ (470, 650) (yellow). The lower-inertia solutions imply a smaller family age. As demonstrated by the two panels, the family age becomes more constrained if one or more parameters are determined.