adsabs/AstroCLIMB huggingface dataset:
Paper: Postperihelion Cometary Activity on the Outer Main-belt Asteroid 2005 XR132 
Authors: Yu-Chi Cheng, 宇棋 鄭, Bryce T. Bolin, Michael S. P. Kelley, D. Bodewits, Quanzhi Ye, 泉志 葉, Christoffer Fremling, Zhong-Yi Lin, 忠義 林, Ya-Lin Wu, 亞霖 吳, Reed L. Riddle, Wing-Huen Ip, 永烜 葉, Steven L. Groom, Russ R. Laher, 嶺亞 良主
Figure caption: The visible spectrum obtained with the LRIS instrument on Keck I and the g′, r′, z′ broadband reflectance normalized at 550 nm, indicated by an orange cross. The error bars of the spectrum correspond to 1σ uncertainty. The Bus–DeMeo D- and BR-type reflectances are shown as gray and red shading, respectively. No clear features of cometary gas emissions, such as CN and C2, were detected.(The data used to create this figure are available.)
Paper: Postperihelion Cometary Activity on the Outer Main-belt Asteroid 2005 XR132 
Authors: Yu-Chi Cheng, 宇棋 鄭, Bryce T. Bolin, Michael S. P. Kelley, D. Bodewits, Quanzhi Ye, 泉志 葉, Christoffer Fremling, Zhong-Yi Lin, 忠義 林, Ya-Lin Wu, 亞霖 吳, Reed L. Riddle, Wing-Huen Ip, 永烜 葉, Steven L. Groom, Russ R. Laher, 嶺亞 良主
Figure caption: Stacked images of XR132 in linear scale. The field of view of each image stamp is 20″ and oriented with north up. The observational details are shown in Table 1.
Paper: Postperihelion Cometary Activity on the Outer Main-belt Asteroid 2005 XR132 
Authors: Yu-Chi Cheng, 宇棋 鄭, Bryce T. Bolin, Michael S. P. Kelley, D. Bodewits, Quanzhi Ye, 泉志 葉, Christoffer Fremling, Zhong-Yi Lin, 忠義 林, Ya-Lin Wu, 亞霖 吳, Reed L. Riddle, Wing-Huen Ip, 永烜 葉, Steven L. Groom, Russ R. Laher, 嶺亞 良主
Figure caption: The daily R-band (LOT) and r-band (P200) light curve on six individual nights.
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: (a) Tracer particles of the impactor’s metallic core (shown for the y = 0 km slice only) colored by the reservoirs that they are determined to accrete to at the end of the simulation; a white arrow is used to depict the impactor’s velocity vector. (b) Locations of all impactor core tracer particles (y > 0 km also) at the end of the simulation (t = 3 hr), overlaid on top of the target mantle and core yield strengths (0 MPa for fully fluid material). Impact parameters: M  i  = 3.60 × 1022 kg, v  i  ∼ 1.5 v esc, θ  i  = 45°.
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: An Earth-like target and a M  i  = 3.604 × 1022 kg (M  i /M  t  = 0.0063) impactor at the time of contact between the impactor and the target, with (a) the locations of tracer particles within the target and impactor. (b) Geotherms under standard and warm mantle conditions (see Appendix A.3), as well as the solidus for our mantle and core materials. (c) The pre-impact pressure and temperature profiles within the y = 0 km slice of both bodies.
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Mass fraction of the impactor core material as a function of the modified specific energy of impact (Equation (4)), that (a) accretes to the target core, (b) dynamically escapes and is not accreted to the target on short timescales, and (c) accretes to the target mantle, from iSALE simulations. Parameterized fits are shown by the solid and dashed lines, corresponding to different accretion modes, with a 1σ error contained by the shaded region around each line. Filled-in data points are those included in the parameterized fits, with white dots indicating those points included in the “None to Target Core” fit. Unfilled data points are those not included in the parameterized fits (either impacts that are head-on or that exhibit secondary impacts). Data from Genda et al. (2017) and Citron & Stewart (2022) are shown only in (b) as no method of distinguishing between impactor core accreting to the planet mantle and planet core is implemented. Data from Marchi et al. (2018), conversely, are shown in all panels. Appendix B contains an alternative version of this figure with additional information on the impact parameters of Marchi et al. (2018) and Citron & Stewart (2022).
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Regimes in the M  i –θ  i  parameter space for which different accretion modes can be predicted to occur, where accretion modes correspond to the parameterizations we construct as a function of Q  L  (Section 4.2). Data points indicate iSALE simulations or SPH simulations of other studies. Data points with multiple colors indicate simulations at the same M  i  – θ  i  but with different v  i  that belong to different impact regimes. Note that regimes are not prescriptive, with both overlapping regions and boundaries between regions meant to indicate where the accretion of impactor core material is sensitive to impact parameters. In these regions, either of the numerical evaluations of Equation (5) could be valid, or somewhere in between.
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Evolution of the impactor core material, including (a), (b) formation of a linear geometry of molten impactor iron through deceleration and pancaking; (c), (d) disruption of the linear geometry, leading to material escape and formation of molten iron blobs and ligaments; (e), (f) sinking of large molten iron blobs to the target core or residency in the mantle. Grid cells containing impactor iron are shown in white (cell mass fraction is ignored for simplicity, but it should be noted that cells often contain ≪100% iron). Yellow dashed line shows the initial location of the surface of the planet and the outer edges of the impactor mantle and core. Impact parameters: M  i  = 3.60 × 1022 kg, v  i  = 1.5 v esc, θ  i  = 45°. The final time step for this impact (300, t = 3 hr) is shown in Figure 3(b).
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Alternative version of Figure 6, with additional detail given for Marchi et al. (2018) and Citron & Stewart (2022) impact parameters to assist in direct comparison between iSALE simulations and their SPH equivalents with similar impact parameters. Impacts with M  i /M  t  ≥ 0.010 0 are also shown, which belong to the giant impacts accretion mode and show distinctly different impactor core material distribution as a function of Q  L .
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Density profiles at the final time step of the simulations for iSALE2D simulations under central (left) and self- (center) gravity, as well as an iSALE3D simulation under central gravity (right). Lagrangian tracer particles representing impactor core material are shown as white dots, visible almost exclusively at the CMB (see text for more details). Impact parameters are M  i  = 1.93 × 1022 kg, v  i  ∼ 1.5 v esc, θ  i  = 0°. Because of the symmetry of 2D simulations, iSALE models only one hemisphere of the planet slice along y = 0 km to reduce computation time. iSALE3D models one hemisphere of the full planet for similar reasons of symmetry, but because of the head-on nature of the impact in this specific scenario, the impact is additionally symmetrical in the x-axis, hence we show only one half of the simulated space (right).
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Mass fractions of impactor core material accreted to each of our defined accretion reservoirs for a selection of iSALE simulations, demonstrating the wide variety of distributions possible across the parameter space of large impacts. Numerical values are provided in Table 5 in Appendix B, alongside a much wider range of impact parameters.
Paper: The Distribution of Impactor Core Material During Large Impacts on Earth-like Planets
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Thomas M. Davison, Gareth S. Collins, Oliver Shorttle
Figure caption: Evolution of models run for 24 hr with and without material strength in iSALE3D with impact parameters M  i  = 1.93 × 1022 kg, v  i  ∼ 1.5 v esc, θ  i  = 45°. Frames are selected to show key stages of the accretion pathways of impactor core material (see text). The Eulerian grid property of cell-averaged material density is shown for the y = 0 km slice, with tracer particles of the impactor core at all depths (i.e., y > 0 km also) overlaid on top (white dots).
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Highest-resolution unobstructed view of the two rocks that were moved and possibly modified by the TAG event—“plate rock” (left outline) and “tagged rock” (right outline). Arrows point to stones described in the main text. The upper arrow points to a stone that is ∼1 cm in length. The lower-right arrow indicates a stone ∼3 cm in length. The lower-left arrow points to a longer, flat stone ∼7 cm in length. As in Figure 5, the larger circle indicates the outer extent of the TAGSAM head (32 cm diameter). The smaller circle indicates the extent of the opening in TAGSAM through which regolith particles may have been ingested. North is approximately toward the right in the image. SamCam image 20201020T214934S275_sam_iofL2pan5.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Top: thermal inertia values for OTES spots near the TAGSAM contact point (white circle, 32 cm diameter) observed during the TAG pass. The dotted lines indicate the approximate extents of the larger plate rock and smaller tagged rock. The OTES spots obtained during the TAG approach are very tightly spaced and have significant overlap. This figure only shows every third spot to avoid clutter. The basemap is a PolyCam Recon C mosaic. Bottom: thermal inertia of the OTES spots in the top figure. The results from running the ATPM model with each of the two DTMs (OLA v20 and v21) are shown for comparison. The approximate extent of the plate rock and the tagged rock are indicated in light gray and dark gray, respectively. Representative error bars (all the same) have been added to some points but not all to avoid clutter. The spot center position error bars indicate the extent of the OTES spot (±7.6 cm based on the OTES spot diameter).
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Modeled apparent thermal inertia of a rock covered with a continuous monolayer of spherical particles. The unlayered thermal model was fit to the 3D model radiance at local hour 14:40, the approximate time that OTES observed the eventual TAG point as the spacecraft approached the surface for sample collection. Particle sizes are 1 mm, 5 mm, 1 cm, 2 cm, and 5 cm. The thermal inertia of the individual particles, the rock substrate, or in some cases both sets of materials are indicated in the legend (units of J m−2 K−1 s−1/2).
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: SamCam image taken approximately 30 s before TAGSAM contact with the surface. The front edge of TAGSAM can be seen at the bottom of the frame. The lateral extent of the OTES data swath that was collected during the TAG approach is shown as dashed lines, with arrows indicating the direction of data collection (compare to Figure 4, top). The larger white circle indicates approximately where the 32 cm diameter TAGSAM touched the surface. The smaller white circle indicates the extent of the TAGSAM opening. Regolith within the inner circle may have been sampled in bulk. Smaller particles from within the annular area between the two circles may have been sampled by the contact pads. North is approximately toward the right. SamCam image 20201020T214918S448_sam_iofL2pan5.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: (a) Elevated thermal inertia values in Matchpoint and TAG data correspond spatially with higher-reflectance boulders that are tens of centimeters in size. (b) Low thermal inertia values in Checkpoint data on fine regolith and a dark-toned boulder. In both figure frames, OTES spots are colorized by thermal inertia. We omit two out of every three sequential spots in this figure to improve clarity. The basemap is a PolyCam Recon C mosaic.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Diurnal brightness temperature results from (top) the 3D sphere-coated model as a function of sphere diameter, where both sphere and substrate thermal inertia is fixed 860 J m−2 K−1 s−1/2, and (bottom) the simple 1D unlayered model as a function of thermal inertia (TI, units J m−2 K−1 s−1/2).
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Geometry and example temperature result for the 3D thermal model of particle monolayers on a rock substrate. In this example, the spheres are 5 cm in diameter, the thermal inertia of both materials is 860  J m−2 K−1 s−1/2, and the time of observation is local noon.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Scatter plot comparison between v20 and v21 thermal inertia results. Some random Gaussian noise was added to the thermal inertia values (±5 standard units) to reduce the number of overlapping points for ease of data visualization. Blue line is 1:1 for comparison.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Comparison of v20 and v21 DTM model results, shown through time (observation number).
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: (A) LROC NAC image (NAC M1197583152; 1.2 m pixel−1) of a wrinkle ridge in East Mare Serenitatis showing boulder fields on the east-facing scarp (yellow arrows). The blue inset box shows the density of meter-scale boulders present over one small area of the wrinkle ridge scarp. (B) LOLA/Kaguya ∼60 m pixel−1 slope map over the wrinkle ridge from Figure 1(A).
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: Apparent thermal inertia of a rock covered with a dense monolayer of spherical particles. The unlayered thermal model was fit to the 3D model radiance at (top) local hour 3:20 AM and (bottom) to seven times of day corresponding to the OSIRIS-REx Detailed Survey stations. Particle sizes are 1 mm, 5 mm, 1 cm, 2 cm, and 5 cm. The thermal inertia of the individual particles, the rock substrate, or in some cases both sets of materials are indicated in the legend assuming standard units (J m−2 K−1 s−1/2). Compare to Figure 7 (daytime fit) in the main text.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: TAG site stereo-pair images. Top version can be viewed with a stereoscope, bottom version can be viewed cross-eyed. Figure adapted from Lauretta et al. (2023b).
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: 3D particle-coated model brightness temperature (10 μm, orange) solutions where the thermal inertia of particles and the substrate is 860 J m−2 K−1  s−1/2, as a function of particle size indicated in each plot. Best-fit thermal inertia solutions from the 1D model (fit to the local solar time of the TAG site observations, 14:40) are shown in blue. The small drop in temperature near noon for the cases with 1 mm and 5 mm sphere coatings is simply due to the ordered arrangement of the spheres. At that time, the direction of the Sun is aligned with the square pattern of the spheres such that they all briefly partially shadow each other, causing a temporary drop in temperature. This is not observed for the larger spheres because they have a larger volumetric heat capacity and thus do not respond as rapidly to shadowing.
Paper: Lunar Boulder Fields as Indicators of Recent Tectonic Activity
Authors: Cole Nypaver, Thomas Watters, Bradley Thomson, Ali Bramson, Joshua Cahill, Jaclyn Clark, Catherine Elder, Caleb Fassett, Gareth Morgan, Santa Lucía Pérez Cortés, Tyler Powell
Figure caption: (A) NT2022 recently active wrinkle ridges colorized by median rock abundance (RA) value overlaid onto the LROC WAC global mosaic (∼100 m pixel−1). The highest 5% RA wrinkle ridges are primarily located in S. Mare Cognitum, Mare Procellarum, Mare Humorum, and Mare Serenitatis. Ridges with the lowest 5% RA are concentrated in Mare Imbrium and central Mare Procellarum. (B) The overall distribution of wrinkle ridge RA median values for every ridge in the NT2022 database.
Paper: Rocks with Extremely Low Thermal Inertia at the OSIRIS-REx Sample Site on Asteroid Bennu
Authors: Andrew J. Ryan, Benjamin Rozitis, Daniel Pino Munoz, Kris J. Becker, Joshua P. Emery, Michael C. Nolan, Marc Bernacki, Marco Delbo, Catherine M. Elder, Matthew Siegler, Erica R. Jawin, Dathon R. Golish, Kevin J. Walsh, Christopher W. Haberle, Carina A. Bennett, Kenneth L. Edmundson, Victoria E. Hamilton, Phillip R. Christensen, Michael G. Daly, Dante S. Lauretta
Figure caption: rms error for TAG spots exclusively inside (left) and outside (right) of the central 7 m of the crater (which includes the TAG observations). The black asterisk on both plots indicates the best-fit location when all spots are considered (Figure B3, Frame D). The red asterisk on the left figure indicates a second local minimum solution. However, fits to the full radiance spectrum using this minimum were much worse than when using the global minimum. The analysis of the spots outside of the sampleability region (right) revealed only one global minimum (red asterisk) which was within 3.5 cm of the global solution (black asterisk).