adsabs/AstroCLIMB huggingface dataset:
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: Two examples ((a), (b), (e) and (c), (d), (f)) show the extraction procedure of representative reflectance spectra of fresh ejecta deposits excavated by impact craters in the CE-6 landing area. The base images for (a) and (c) are LRO-NAC images, and those for (b) and (d) are M3 images. Image data IDs and available addresses are listed in Table A1. The M3 spectra displayed in (e) and (f) are available in machine-readable format. The spectra are not smoothed, except for the last three columns of data.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: The location of fresh craters, backgrounds, and the areas in the high-reflectance terrain. The light-blue circles and red circles represent the fresh crater locations in the W-mare and E-mare, respectively. The size of the circle refers to the relative diameter, not the actual diameter. Two blue areas in the W-mare and one red area in the E-mare are mare regolith backgrounds. Four areas marked P1, P2, P3, and P4 in the bright terrain are indicated by black and orange arrows. The light-green arrow points to the location of the second-largest crater selected in this work. Two fresh craters that will be shown in Figures 3(a) and (c) are indicated by white arrows. The red star represents the CE-6 landing location. The black dashed curve is a rough unit boundary between the W-mare and E-mare. The base map is from the OMAT mosaic (∼59 m pixel−1).
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: Mineral and composition abundances, and the OMAT value inferred from Kaguya MI global product maps. (a) OLV. (b) OPX. (c) CPX. (d) PLG. (e) FeO. (f) TiO2. (g) SMFe. (h) OMAT parameter. The light-blue and light-red horizontal boxes represent the range of background values in the W-mare and E-mare. The black vertical lines in (b) and (f) represent the crater diameter (1000 m) corresponding to the depth where significant material changes occur in the W-mare. The error bars are the statistical standard deviations of composition abundances.
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: (a) Topography of the wrinkle ridge. Blue, red, and orange circles represent fresh crater locations in the W-mare, E-mare, and the wrinkle ridge, respectively. Two red solid curves outline the main faults and the back thrust faults, and the red dashed curve represents the splay faults. The outline of the main faults is consistent with the boundary between the W-mare and the E-mare based on the spatial distribution of titanium content (Figure 1(c)). (b), (c) Features of the basaltic flow fronts. (d) Elevation of the profile line A-A′ and B-B′ in (c) based on SLDEM2015.
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: Compositional variations at different depths of the CE-6 landing mare. Data used in this plot are organized in Table 1. The light-blue and light-red boxes represent the range of background values in the W-mare and E-mare, respectively.
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: M3 spectra of materials at different depths in the W-mare. The Band I and Band II centers shift toward shorter wavelengths with increasing depth. P1, P2, P3, and P4 represent the craters in the high-reflectance terrain, as shown in Figure 2. The M3 spectra used in this work are available in machine-readable format from the online journal (see Figure 3).
Paper: The Composition and Stratigraphy of the Chang’e-6 Landing Mare
Authors: Pei Ma, Zhiyong Xiao, Yichen Wang, Yunhua Wu, Yizhen Ma, Fanglu Luo, Rui Xu, Qingyun Deng
Figure caption: Box plot of titanium contents of small fresh craters in the W-mare, E-mare, and the wrinkle ridge. The magenta short lines represent the median.
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Distributions of secular drift rate ∣k∣ as a function of a (left panel) and ω (right panel) for NEAs satisfying Equation (11). Objects with distinct MEI values (0.0–0.1 and 0.8–0.9) and eccentricity ranges (e ≥ 0.2 or e < 0.2) are highlighted with asterisks in the panels. The red dashed line in the left panel represents the empirical upper limit defined by Equation (12).
Paper: Classifying and Characterizing the Evolution of the Minimum Orbit Intersection Distance for Near-Earth Asteroids
Authors: Shoucun Hu, Yuanyuan Chen, Xinran Li, Xiuhai Wang, Xuefeng Wang
Figure caption: Distributions of ε and η as a function of the semimajor axis a. Objects that experience close encounters with different planets are represented by different colors. The locations of several MMRs are also illustrated for reference.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: The effect of equatorial electrodynamics on the SMITE Model 4 baseline run (Table 2) is shown. A pair of electron density profiles from Cassini radio occultation S133 is shown in panels (a)–(c) at 6 hr local time (dawn) and panels (d)–(e) at 18 hr (dusk) local time. Panels (a)–(f) show the SMITE Model 4 baseline run using a solid black line, and the solid colored lines show electrodynamic iterations of the SMITE Model 4 baseline run that best matched the data. Model runs using Drifts 1, 2, and 3 (previously shown in Figure 4) are shown by green, purple, and yellow lines, respectively. The “up” and “down” iteration of each electrodynamic model is shown by solid and dashed lines, respectively. The peak dayside field-perpendicular plasma drift velocity, vD, associated with each model is indicated. The latitudinal TEC distribution from all SMITE Model 4 iterations (color/line style the same as (a)–(f)) and the measured TEC from Cassini occultation S133 (hollow brown circle marker with error bars) are shown at (g) dawn and (h) dusk.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: A contour map of the normalized TEC distribution from SMITE is shown for three different Saturnian seasons: (a) southern (hemisphere) summer (Model 2 baseline), (b) near equinox (Model 1 baseline), and (c) northern (hemisphere) summer (Model 3 baseline). For each season, the normalized TEC latitudinal distribution at dawn (blue solid line) and dusk (red solid line) is also shown. The dashed blue and red lines in these panels correspond to analogous models which exclude the ring shadow from the baseline. Panel (d) shows the unscaled TEC at 18 hr local time (dusk) for the southern summer (dotted), near-equinox (solid), and northern summer (dashed) models, and the TEC derived from Cassini dusk radio occultations between 2005 and 2013 with error bars, which span approximately half a Saturn year corresponding to subsolar latitudes from −23° to 17°.
Paper: A New Saturn Model of Ionospheric Transport and Electrodynamics (SMITE)
Authors: Omakshi Agiwal, Luke Moore, Carlos Martinis, Ingo Mueller-Wodarg, J.D. Huba
Figure caption: Model–data comparisons of the electron density altitude profiles are shown for Cassini RSS occultation S125 at (a) 6 hr local time (dawn), and (b) 18 hr local time (dusk). The data are shown using solid gray lines, and the latitude, local time, and subsolar latitude of the measurements are indicated on the figure. The SMITE baseline model is shown using a solid black line and assumes the same solar conditions, latitude, and local time as the data. The TEC measured by Cassini RSS during occultation S125 with error bars and the latitudinal distribution of TEC from the SMITE baseline model are also shown using a hollow brown circle and solid black line, respectively, at (c) dawn, and (d) dusk. The dawn and dusk measurements were taken ∼4 hr apart, with the dusk profile measured first. The occultation points vary by 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1 latitude in the altitude range shown.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Model-derived properties of the water band observed in comet C/2017 K2 (PanSTARRS) vs. projected distance from the photocenter. (a) The water production rate. (b) The rotational temperature. (c) The OPR as a function of cometocentric distance derived from model fits. Considered spectra are MRS Channel 1 MED (ν2 band from 5.66 to 6.63 μm; results with blue symbols) and NIRSpec (5 μm hot band; red symbols) spectra extracted over annuli of 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩13 (MRS) and 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩1 (NIRSpec) diameter. Results from model fits to unblended ortho and para lines are shown with green and orange symbols, respectively. In panel (a), Q(H2O) values derived from the 6.3 μm band were multiplied by 1.17 for consistency with NASA PSG models (see text), and those inferred from ortho and para lines assume OPR = 3. Panel (c) displays OPR values that provide consistent ortho- and para-derived Q(H2O) values (purple symbols).
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: The NIRSpec spectrum of comet C/2017 K2 (PanSTARRS) derived from the G395M IFU data cube in a 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter circular aperture centered on the comet photocenter. Emissions from CO2, 13CO2, CO, OCS (carbonyl sulfide), and H2O are present. The complex near 3.35 μm is composed of C2H6 and CH3OH (ethane and methanol) and the CH3OH Q-branch at 3.52 μm.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Spaxel-by-spaxel spatial distribution of H2O-related physical parameters deduced from MRS Channel 1 MED data. From left to right: band intensity in the range 5.66–6.63 μm, water production rate Q(H2O), and rotational temperature Trot (K) from model fits. A 3 × 3 boxcar spatial smoothing was applied to the original data cube. The inset white arrow indicates the sunward direction.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Model fits to H2O MRS spectra of C/2017 K2 (PanSTARRS). Measurements and model fits are shown in black and red, respectively. Residuals are in green. Top: extracted on-nucleus spectrum. Bottom: extracted off-nucleus spectrum at the (+1:+1) position (see Figure 1). A 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter circular aperture is used. Fitted parameters are given in the inset. Derived apparent production rates are (0.967 ± 0.005) × 1028 molecules s−1 and (2.64 ± 0.01) × 1028 molecules s−1 for the on-nucleus and off-nucleus spectra, respectively.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Apparent molecular production rates (Q) as a function of nucleocentric distance for CO, CH3OH, CO2, CH4, and C2H6 (top panel) and for OCS, H2CO, 13CO2, HCN, and CN (bottom panel) derived from NIRSpec observations of comet C/2017 K2 (PanSTARRS) and modeled with the NASA PSG.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Comet C/2017 K2 (PanSTARRS) rotational temperature profiles for H2O (ν2 band para lines measured with MRS) along with CO, CO2, 13CO2, CH4, and CH3OH (measured with NIRSpec).
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: (a–e) Maps of continuum-subtracted band intensity, apparent production rate, and rotational temperature for CO2, 13CO2, CO, CH4, and CH3OH. (f) Map of continuum-subtracted intensity for H2O, along with apparent production rate for H2O, CN, and OCS.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: The radial distribution of the 12CO2-to-13CO2 ratio in the inner coma of comet C/2017 K2 (PanSTARRS) as a function of nucleocentric distance.
Paper: Conditions for Accretion Favoring an Unmelted Callisto and a Differentiated Ganymede
Authors: Yannis Bennacer, Olivier Mousis, Marc Monnereau, Vincent Hue, Antoine Schneeberger
Figure caption: Simulation of the accretion of a protosatellite similar to Callisto and Ganymede, with parameters α = 4, τacc = 2 Myr, and tstart = 4 Myr. The body begins accreting material at t0 = tstart, starting with an initial radius R0 = 100 km. The simulation stops when the moon’s radius reaches that of Callisto (Rf = 2410 km) and Ganymede (Rf = 2630 km) at tend = tstart + τacc. Left panel: temperature profile radius (black line) within the protosatellite at the end of the accretion phase. The red line represents the melting curve ﹩{T}_{m}(P,{X{}_{{\rm{NH}}}}_{3})﹩ for water ice with 5% NH3. The layer where the temperature profile exceeds the melting curve undergoes melting, where the percentage of material above the melting point of water ice (in volume) is 2.2% and 10.4% for Callisto and Ganymede, respectively. Right panel: time evolution of the temperature distribution during the accretion phase.
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: The “AO50” Case C modeling of the scattered light, removal of water lines, and NASA PSG contributions from volatiles and extraction of residual from the SEDs in comet C/2017 K2 (PanSTARRS) from beam position 0:0 (a 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter beam centered on the photocenter of the comet). Top panel: the observed JWST NIRSPEC (gray line) + MRS (black line) and the “AO50” Case C model with the components of the model shown and extrapolated to NIRSpec wavelengths, and the scattered light (slope) assessed for NIRSpec and extrapolated to MRS. Middle panel: the observed JWST NIRSPEC (gray line) + MRS (black line) and the “AO50” Case C “F(total)” and the scattered light (slope) extrapolated to MRS wavelengths. The MRS residual is shown by the medium turquoise line and the residual median-filtered result plotted with the navy-colored line on top of the medium turquoise line. Bottom panel: same as the middle panel, but in reflectance. The MRS medium turquoise “hash” arises from imperfect modeling of the H2O lines, and the NIRSpec “hash” is not poor signal-to-noise ratio, but rather arises from imperfect molecular modeling of the lines (likely due to optical depth effects in regions of CO2 and HCN emission).
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: Top panel: the “AP50” thermal model fitted to the JWST MRS IR SED in a 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0-diameter aperture centered on the photocenter (position 0:0) of comet C/2017 K2 (PanSTARRS). The models fitted to the observed 7.0–27 μm SED constrain the dust mineralogy, assuming that the coma refractory dust species have optical constants similar to those of amorphous carbon (orange line), amorphous olivine (Mg:Fe = 50:50; cyan line), amorphous pyroxene (Mg:Fe = 50:50; blue line), Mg-crystalline olivine (forsterite; green line), and, when present, Mg-crystalline orthopyroxene (enstatite; pink line). At position 0:0 enstatite was excluded from the best-fit model. The solid red line is the best-fit model composite spectra, superposed on the observed data (black solid curve) that were modeled (λ ≥7.0 μm) and the observed data that were omitted from the thermal models (purple solid line) where strong water emission is dominant. Bottom panel: the model residual (observed data – best-fit thermal model) is in the bottom panel. The spectral region containing the ν2 water emission bands (purple, bottom panel) was not included in the model fit, and the gray vertical regions illustrated the point–point uncertainties (discussed in Section 7.3). Uncertainties were multiplied by 40 in wavelength regions spanning 12.5–16.5 μm (gray vertical lines). AP50 overshoots wavelengths ≲7.0 μm.
Paper: Conditions for Accretion Favoring an Unmelted Callisto and a Differentiated Ganymede
Authors: Yannis Bennacer, Olivier Mousis, Marc Monnereau, Vincent Hue, Antoine Schneeberger
Figure caption: Final states of Callisto and Ganymede as functions of tstart, τacc, and α. The white region indicates where Ganymede undergoes melting, while Callisto remains undifferentiated. From left to right, the panels display increasing values of α, ranging from 3 to 5, with a total of 100 simulations per panel. Values equal to 6 are not shown, as the mass fraction distribution remains unchanged between α = 5 and α = 6, with ∼100 wt% for small impactors (﹩{x}_{m}^{\mathrm{si}})﹩ in both cases. To prevent melting during formation, Callisto must accrete a minimum amount of large impactors (α ≳ 4), namely less than 30% of its final mass. For α = 4 (or α ≳ 5) Callisto’s accretion likely occurred slowly, with τacc ≳ 2 Myr (or τacc ≳ 0.6 Myr), and started no earlier than tstart = 3.5 (or tstart = 3 Myr) after CAIs. Using the same parameters that prevented Callisto from melting, Ganymede could have differentiated early if α = 4, suggesting that the observed dichotomy may be primordial.
Paper: Conditions for Accretion Favoring an Unmelted Callisto and a Differentiated Ganymede
Authors: Yannis Bennacer, Olivier Mousis, Marc Monnereau, Vincent Hue, Antoine Schneeberger
Figure caption: Stokes sinking and overturn timescales vs. typical mantle temperature (150–273 K). Both timescales are inferred using the viscosity of the ice–rock mixture ηmix = ηice/f(ϕ) and an Arrhenius-type relation for ice viscosity ηice = ηrefexp(A(Tref/T − 1). Timescales for Stokes sinking are displayed for different sizes of rock particles (100 m–1 km).
Paper: A JWST Study of the Remarkable Oort Cloud Comet C/2017 K2 (PanSTARRS)
Authors: Charles E. Woodward, Dominique Bockélee-Morvan, David E. Harker, Michael S. P. Kelley, Nathan X. Roth, Diane H. Wooden, Stefanie N. Milam
Figure caption: HDI vs. Natoms. PAH molecules in the PAH model for comet C/2017 K2 (PanSTARRS) with NC ≤ 54 are plotted here (red; symbol size is 10 times the number fraction in the PAH model) in the HDI vs. Natoms relation to set PAHs in comet C/2017 K2 (PanSTARRS) into the context of complex organic molecules assessed for comet 67P/Churyumov-Gerasimeko (yellow, gray), for the ISM (purple), and for nondetections in the Taurus Molecular Cloud 1 (TMC-1; blue), where symbol size represents the number of molecules sharing the HDI value and number of atoms, with the smallest circles representing one molecule. Organic molecules identified by ROSINA in 67P/Churyumov-Gerasimeko include linear, heterocyclic, and aromatic molecules of NC  ≥  4. PAHs in comet C/2017 K2 (PanSTARRS) are more hydrogenated than the trend for the ISM and less hydrogenated than 67P/Churyumov-Gerasimeko. Adapted from N. Hänni et al. (2022), using their data and their data compilations from K. Altwegg et al. (2019), B. A. McGuire (2021), and T. J. Barnum et al. (2022).
Paper: Conditions for Accretion Favoring an Unmelted Callisto and a Differentiated Ganymede
Authors: Yannis Bennacer, Olivier Mousis, Marc Monnereau, Vincent Hue, Antoine Schneeberger
Figure caption: Evolution of the midplane effective temperature Te(t) in the Jovian CPD at the current orbits of Ganymede (solid line) and Callisto (dashed line). The CPD model assumes a metallicity Z/H = 2.45 × 10−2, a disk viscosity parameter of 10−3, a centrifugal radius of 50RJ, an ambient temperature Tneb = 40 K, and a planetary temperature Tp = 2000 K.
Paper: On Error Estimates for Hapke Photometric Model Parameters from Disk-integrated Phase Curves of Airless Planetary Bodies
Authors: Paul Helfenstein, Anne J. Verbiscer
Figure caption: Left: histogram of all valid residuals from the full suite of stepwise grid searches for the nominal fit to 2002 KX14’s phase-curve data after exclusion rules have been applied. The abscissa is the absolute difference between grid-searched χ2 values and ﹩{\chi }_{{\rm{\min }}}^{2}﹩, the χ2 that corresponds to the nominal parameter solution found on the unweighted magnitude scale. N is the number of grid-searched parameter sets remaining after filtering the entire collection through the exclusion rules. ﹩\Delta {\chi }_{0}^{2}=| {\chi }_{{\rm{nom}}}^{2}-{\chi }_{{\rm{\min }}}^{2}| \geqslant 0﹩, where ﹩\Delta {\chi }_{{\rm{nom}}}^{2}﹩ is the nominal solution for the best-fit parameters independently found on the weighted reflectance scale. The finite width of the histogram increments for Δχ2 is adjusted to ensure that the computed cumulative distribution converges on zero when ﹩\Delta {\chi }_{0}^{2}﹩ is very small compared to the total histogram width. Total area of the discrete distribution is normalized to unity. Histogram mean Δχ2 and its corresponding deviation ﹩{\boldsymbol{\pm }}1{\sigma }_{\Delta {\chi }^{2}}﹩ are shown as long-dashed and short-dashed vertical lines, respectively. Right: cumulative distribution corresponding to the histogram on the left with the corresponding CEG scale on the right ordinate. Filled circles are the CEG∣j values determined for each labeled jth Hapke parameter. Vertical dashed lines extending downward from the circles identify the corresponding values of each Δχ2∣j correction for missing phase angle coverage (Table C3) to be used in defining the parameter waterlines (Appendix B.3). Figure B1 contains the complete set of 12 plot pairs.