adsabs/AstroCLIMB huggingface dataset:
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: PAH model fitted to ﹩{F}_{{\rm{Residual}}}^{{\rm{PAHextract}}}﹩ for comet C/2017 K2 (PanSTARRS). (a) Model fit to 3.2–3.6 μm and 5.5–8.62 μm (black solid) spectral regions, and model predicted outside of that range (black short dashed), shown with a breakdown into seven categories of PAHs in the model: small (NC ≤ 40) neutral PAHs with CH2 groups (﹩{N}_{{{\rm{CH}}}_{2}}﹩ > 0) (pink); small cations (﹩{N}_{{{\rm{CH}}}_{2}}﹩ = 0) (purple), small cations with CH2 groups (﹩{N}_{{{\rm{CH}}}_{2}}﹩ > 0) (blue), and small cations with metylene side groups (﹩{N}_{{{\rm{CH}}}_{3}}﹩ > 0) (green); large neutrals (yellow); large cations (﹩{N}_{{{\rm{CH}}}_{2}}﹩ = 0) (red); and large cations with CH2 groups (﹩{N}_{{{\rm{CH}}}_{2}}﹩ > 0) (brown). (b) Model fit of the 3.42 μm region where primarily three small neutrals with CH2 groups generate the observed peak, with fully hydrogenated C18H24 (pink dotted) dominating the flux density compared to heavily hydrogenated C10H12 (pink dashed–dotted) and fully hydrogenated C24H24 (pink dashed). (c) Model components of small cations and large neutrals with their sum (black long-dashed line) that dominate the 6.85–8.62 μm emission: small cations (﹩{N}_{{{\rm{CH}}}_{2}}﹩ = 0) (purple), and large neutrals (﹩{N}_{{{\rm{CH}}}_{2}}﹩ = 0) (yellow). Small cations with groups (﹩{N}_{{{\rm{CH}}}_{2}}﹩ > 0, ﹩{N}_{{{\rm{CH}}}_{3}}﹩ > 1) (blue, green) contribute near 6.85 μm, and (﹩{N}_{{{\rm{CH}}}_{3}}﹩ > 1) to the 8.25 μm feature. Small cations and large neutrals contribute to the 6.3 μm feature. (d) Model breakdown into functional groups: ﹩{N}_{{{\rm{CH}}}_{2}}﹩ = 0, ﹩{N}_{{{\rm{CH}}}_{2}}﹩ > 0, ﹩{N}_{{{\rm{CH}}}_{3}}﹩ > 0 (brown, blue, cyan). (e) Model breakdown into neutrals (chartreuse) and cations (deep purple). (f) Model breakdown into small (orange) and large PAHs (NC > 40) (dark teal).
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 14 μm residual feature in comet C/2017 K2 (PanSTARRS) compared to other comets observed with Spitzer (D. E. Harker et al. 2023) that span this spectral range in the SED. The blue dotted vertical line in the middle panel is at 14.0 μm. The SEDs in the middle panel are taken from the model compilations of Spitzer-observed comets (D. E. Harker et al. 2023), where the fluxes are relative, scaled to that of comet C/2017 K2 (PanSTARRS) for comparison. The bottom panel shows the residual (observed SED – model SED) to highlight residual features present at 9.3 and ≃14.7 μm. The top residual plot is that of comet C/2017 K2 (PanSTARRS). Immediately below that black solid line (which is the residual) are four curves of various oxides (see Section 7.6) scaled to 0.5 at their peak of a blackbody function (Fbb) of Fbb[TBB] × Qabs, where TBB is the derived blackbody temperature of the model fit at position “0:0” and Qabs are the absorption efficiencies of common characteristic minerals commonly found in CAIs (A. Greshake et al. 1996). The plum-colored dashed–dotted line shows that dust with a crystalline pyroxene composition cannot produce the observed ≃14 μm residual or the features in the residual near 9.3 and 10.0 μm because the other resonances of CP are absent from the residual at the contrast predicted by the thermal model for CP for C/2017 K2 (PanSTARRS) (scaled from the position +1:+1 “AO50” model Case A).
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 3.0–5.0 μm spectral region of comet C/2017 K2 (PanSTARRS) derived from NIRSpec data of the central coma (position 0:0; see Figure 6). Top spectrum: the spectra decomposed using a NASA Planetary Spectrum Generator (NASA PSG; G. L. Villanueva et al. 2018) model that incorporates CH3OH adopting a temperature of 40 K. The black solid line is the observed spectrum, while the NASA PSG model is given by the blue solid line, both scaled up by factor of 2 for offset clarity. Bottom spectrum: the lower purple line is the result of median filtering (medfilt) of the residual (observed – model). The lower chartreuse and lower green lines are the continuum derived by more complex steps than just medfilt as described in the text (Appendix D). The magenta line is the residual emission centered near 3.42 μm that cannot be accounted for by the PSG model. This residual emission is fitted by models with small, heavily hydrogenated PAHs fluorescing in the solar radiation field (see Section 8.2).
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 ternary diagram of comets showing the three-dimensional dependence along the axes of amorphous carbon (AC), amorphous silicates (AC), and crystalline silicate (CS) dust composition. The filled black symbols represent the dust composition of the seven JWST MRS beam-tile positions derived from Case A treatment of the JWST SEDs (see Section 7.3). Filled symbols are OCCs, and open symbols are JFCs. The purple filled star is that of OCC comet C/1995 O1 (Hale-Bopp; D. E. Harker et al. 2002; C. E. Woodward et al. 2021). The circles are values derived from thermal models of OCCs and JFCs from the Spitzer-observed full-wavelength-coverage SEDs (D. E. Harker et al. 2023). The filled cyan squares are values derived from SOFIA SEDs of OCCs (C. E. Woodward et al. 2021).
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 ternary diagram for the “AO50” model dust composition in the coma of comet C/2017 K2 (PanSTARRS). The black plus sign is the dust composition derived for Case A, the orange plus sign is the dust composition derived for Case B, and the blue plus sign designates the dust composition derived from Case C. The filled black symbols represent the dust composition of the seven MRS beam-tile positions derived from Case A treatment.
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 three “AO50” models for Case A, Case B, and Case C thermal model fits (Section 7.3). Top panel: the top curve is Case A, the middle curve is Case B, and the bottom curve is Case C. The inset explains the details of each case, and the red curve in each instance is the best model fit. Purple denotes regions where water emission bands are present. Bottom panel: the residuals (fit data – the best-fit thermal model).
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: Number fraction of PAH molecules in the PAH model for comet C/2017 K2 (PanSTARRS) vs. number of carbon atoms (NC) and colored by number of CH2 groups (NCH2). The number fractions are grouped by (NC, NCH2) and summed.
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: Comparison of the two methods for defining phase coverage partitions from which the parameter-dependent value of CEG is determined. The axes labeled “Normalized Sensitivity” identify plots of ﹩{\dot{R}}^{2}(\alpha ,{\varpi }_{o})﹩ (see Section 5.1.3). The examples shown compare ϖo parameter sensitivity plots for α coverage of Triton (Table 8). Both curves are computed from our nominal fit of the Hapke model to Triton. The CEG value represents the fractional area of the hatched regions relative to the total area under the curve. Each filled circle on the abscissa identifies the α of an observation. Open circles mark the full α range. (a) Discrete partitions used in Verb22 are shown by hatched columns. (b) The hatched contours represent the cumulative statistical phase modulation function (see Equation (26)) developed in this study. This method models how the distribution of observations with α and the separation of each data point from its nearest neighbors contributes to the Hapke parameter’s overall sensitivity to available data.
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: Phase curves of BCB(α) and BSH(α) for different assumed values of the opposition effect angular widths (i.e., HWHM, αhw). At the same values of αhw, SHOE diminishes at a slower rate than CBOE (B. Hapke 2012b). For αhw = 0.1°, hCB = 0.00264, hSH = 0.000873; for αhw = 1°, hCB = 0.0264, hSH = 0.00873; for αhw = 10°, hCB = 0.264, hSH = 0.0873. The value of αhw = 59.82° corresponds to the upper physical limit of hSH = 0.522 (B. Hapke 2008). For CBOE curves B0SH = 0 and B0CB = 1, and conversely, for SHOE curves B0SH = 1 and B0CB = 0. The other parameters were fixed at ﹩\bar{\theta }=0^\circ ﹩, ϖo = 0.01, Henyey−Greenstein g = 0.
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: Behavior of our adaptation (Equations (10) and (11)) of B. Hapke (2012b) ﹩{\bar{\theta }}_{p}﹩ albedo correction to ﹩\bar{\theta }﹩. Top row: Each solid curve models the effect of decreasing the value of ϖo, given different assumed values of ﹩\bar{\theta }﹩. Separate plots are shown for backward-scattering particles (left), isotropic particles (middle), and forward-scattering particles (right). Dashed curves show the inverse case in which the predicted ﹩\bar{\theta }﹩ increases with ϖo for given different assumed values of ﹩{\bar{\theta }}_{p}﹩. For isotropically scattering grains (geff = 0), the behavior simplifies to that of the B. Hapke (2012b) original approximation. Bottom row (left and right): same as the top row, but for backward-scattering (left) and forward-scattering (right) grains with more extreme narrow peaks in the SPPF. Bottom middle: values of ϖo at which ﹩{\bar{\theta }}_{p}﹩ exceeds physically meaningful limits, assumed here to be 55°. Separate curves show values of geff assumed in the other panels: geff = 0, isotropic case (solid line); geff < 0, backward-scattering case; and geff > 0, forward-scattering case.
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: Sensitivity of our model-fitting approach to different first guesses of model parameter values and to two different model-fitting options for our 2002 KX14 example. (a) Fitting observations on a magnitude scale and without statistical weighting (Equation (19)) using two different first-guess models from Table 4 to bracket the observations: 2014 OE394 and Ixion. All of the model fits converge on the same solution, represented by the solid curve. Error bars are omitted from the data points since they were not used in the fitting algorithm. Here the solution best fits the implied shape of the phase curve at the expense of ignoring the differences in predicted reliability among the observations. (b) Fitting observations on an I/F scale with statistical weighting (Equation (18)). Error bars shown on the data points were used in weighting factors. First-guess models are the same as in panel (a). Fits from the two first guesses converge on different solutions that do not match our nominal solution from panel (a). Here the solutions are dominated by the cluster of the most reliable data at small α at the expense of fitting the one observation that would define the shape of the phase curve at much larger α.
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: B. Hapke (2012b) model curves of the normalized reflectance ratio vs. phase angle computed for backward-scattering Henyey−Greenstein functions relative to the isotropic model (g = 0). Separate labeled curves correspond to values of g ranging from −0.1 to −0.975. The reflectance ratio at each phase angle is the predicted Hapke model whole-disk reflectance for an assumed value of g relative to the same Hapke model parameters but with g = 0 to model isotropically scattering particles. Each curve is normalized to unity at α = 0°. The plot shows how the predicted behavior of the SPPF progressively mimics an opposition effect as g approaches −1.0. All model parameters except g were fixed at ϖo = 0.01, B0SH = B0CB = 0, hSH = 0.522, hCB = 0.0001, ﹩\bar{\theta }=0^\circ .﹩
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: Normalized disk-integrated reflectance ratio as a function of phase angle. Separate labeled curves correspond to values of ﹩\bar{\theta }﹩ from 0° to 80° (see Table 6). The reflectance ratio at each phase angle is the predicted Hapke model whole-disk reflectance for an assumed value of ﹩\bar{\theta }﹩ relative to the same Hapke model parameters but with ﹩\bar{\theta }=0^\circ ﹩ to model a smooth surface minus 1, or (Rrough − Rsmooth)/Rsmooth. Each curve has been normalized to unity at α = 0°. The plot shows how the predicted behavior of macroscopic roughness progressively mimics an opposition effect as ﹩\bar{\theta }﹩ approaches 90°. All model parameters except ﹩\bar{\theta }﹩ were fixed at ϖo = 0.01, B0SH = B0CB = b = 0, c = 1.0, hSH = 0.522, hCB = 0.0001.
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: Parameter sensitivity plots for each parameter of our B. Hapke (2012b) model preliminary fit to 2002 KX14. Filled circles on the abscissa identify the α of each observation. Open circles mark the full α range. Filled curves show the cumulative statistical phase modulation function (see Equation (26)) that controls how the distribution of observations with α and the separation of each data point from its nearest neighbors contribute to the Hapke parameter’s overall sensitivity to available data (i.e., its CEG value, reported in each plot).
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: the equivalent amplitudes of the topographic roughness pseudo-opposition effect behavior as a function of the corresponding value of ﹩\bar{\theta }﹩ (Table 6). The amplitudes increase almost linearly up to 50°, above which they increase radically. Right: equivalent angular width parameters of SHOE and CBOE as functions of the assumed value of ﹩\bar{\theta }﹩. Variations in the angular widths over the range from 10° to 80° are relatively small, with a slight trend toward narrowing with increasing ﹩\bar{\theta }﹩.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Enlarged spectrum between 3500 and 1000 cm−1 (2.5–10 μm) of the 5% CH4 (top) and 5% CO (bottom) atmosphere generated hazes as a function of wavelength in reflectance with major spectral features labeled. Between pre- and postirradiation, there are larger changes in the 5% CH4-derived haze spectrum in comparison to the 5% CO-derived haze spectrum, where the differences are not obvious.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Top: UV–VIS (46,000–18,000 cm−1, 0.22–0.54 μm) spectrum for the 5% CH4 atmosphere haze sample across the 350 nm filter, corrected for interference fringe effects. The pre- and postirradiation uncorrected spectra have been offset vertically by 0.065 for clarity. The corrected and smoothed data during the irradiation process are plotted as is. Bottom: the total integrated reflectance of the fringe-corrected smoothed data spanning the plotted wavelength range over the duration of the irradiation process. The gray solid line is the best-fit flat line, with a reduced χ2 of 1.1. The gray dashed line is the best-fit sloped line, with a reduced χ2 of 0.77. The error bars for the integrated reflectance are derived from propagating errors throughout the instrument, fringe interference equation, smoothing, and integration.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Top: UV–VIS (46,000–18,000 cm−1, 0.22–0.54 μm) spectrum for the 5% CH4 atmosphere haze sample across the 228 nm filter. The pre- and postirradiation uncorrected spectra have been offset vertically by 0.065 for clarity. The corrected and smoothed data during the irradiation process are plotted as is. Bottom: the total integrated reflectance of the fringe-corrected and smoothed data spanning the plotted wavelength range over the duration of the irradiation process. The gray solid line is the best-fit flat line, with a reduced χ2 of 4.4. The gray dashed line is the best-fit sloped line, with a reduced χ2 of 2.9. The error bars for the integrated reflectance are derived from propagating errors throughout the instrument, fringe interference equation, smoothing, and integration.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Top: UV–VIS (46,000–18,000 cm−1, 0.22–0.54 μm) smoothed spectrum for the 5% CO atmosphere haze sample across both the 228 nm and 350 nm filters pre- and postirradiation. Due to the apparent thinness of the haze film, there is not enough fringing seen to be corrected. Bottom: the total integrated reflectance of the smoothed data spanning the plotted wavelength range over the duration of the irradiation process. The blue solid line is the best-fit flat line for the 350 nm filter, with a reduced χ2 of 0.22. The purple dashed line is the best-fit flat line for the 228 nm filter, with a reduced χ2 of 0.36. The error bars for the integrated reflectance are derived from propagating errors throughout the instrument, fringe interference equation, smoothing, and integration. There are no changes within the error bars in the integrated film reflectance between pre- and postirradiation in this wavelength range.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Top: the C–O stretching features of the 5% CH4-derived haze sample evident of a primary alcohol seen pre- and postirradiation in reflectance. The irradiation process made the spectral features less pronounced in relation to the preirradiation spectra across both filters. Bottom: the relative change between preirradiation and postirradiation of each filter, respectively.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Top: the C–H stretching mode of an alkane spectral feature of the 5% CH4-atmosphere-derived sample pre- and post-UV irradiation in transmittance. The postirradiation through the 350 nm filter had larger increases in transmittance and created “bumps” in the spectra. Bottom: the relative change between the preirradiation and postirradiation spectrum of each filter respectively due to the UV bombardment.
Paper: Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes through Laboratory Experiments
Authors: Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton
Figure caption: Reflectance spectra of our 5% CH4-derived haze sample (top) and 5% CO-derived haze sample (bottom) in the visible to mid-IR wavelength region (26,000–1000 cm−1, 0.4–9 μm). The black line represents the samples before the irradiation process began, and the teal and red lines represent the postirradiation spectrum across the 350 nm and 228 nm filters, 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: The CE-6 landing site (red stars) and the southern mare in the Apollo basin. The yellow dashed curve in (a) and black dashed curves in (b–d) are rough boundaries that divide the landing mare as the western and eastern units. White dashed curves are approximate boundaries of prominent impact rays formed by the Chaffee S crater, which have changed the reflectance spectra at the northwestern area of the landing mare so that derived surface compositions are different. (a) Normalized albedo based on the Chang’e-2 global orthophoto map (50 m pixel−1). (b) Red, green, and blue false color composition derived by the Kaguya Multiband Imager data (20 m pixel−1). Red = 750 nm/415 nm, green = 750 nm/950 nm, blue = 415 nm/750 nm. (c) TiO2 content derived from reflectance spectra obtained by the Kaguya Multiband Imager (∼59 m pixel−1). (d) Topography map from the SLDEM2015 (∼59 m pixel−1) appended to the Kaguya Terrain Camera morning mosaic, respectively. The boundary of the southern mare is from D. M. Nelson et al. (2014).
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 spectral analysis results. (a) The plot of the Band I position and crater diameter. (b) The plot of the Band II center position and crater diameter. The light-red (800 m) and light-blue (1300 m) vertical lines are the crater diameters corresponding to the depths where significant material changes occur in the E-mare and W-mare, respectively. (c) and (d) Band centers of fresh craters inside the southern mare. The band centers of synthetic pyroxene and the dashed line locations are from R. L. Klima et al. (2007, 2011). The error bars are the statistical standard deviation of the fitted band centers. The M3 spectra used to generate these plots are available in machine-readable format from the online journal (see Figure 3).