adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Value of ﹩f+\overline{\zeta }﹩ normalized (each line is normalized by its maximum) using Equation (5) for the zonal mean zonal wind for different vortex strengths (panel (a): U 0 = 10, black; U 0 = 30, blue; U 0 = 60, red), latitude (panel (b): ϕ 0 = 35°, black; ϕ 0 = 50°, blue; ϕ 0 = 65°, red), width (panel (c): ϕ  w  = 20°, black; ϕ  w  = 10°, blue; ϕ  w  = 3°, red), and rotation rates (panel (d): Ω = 1, black; Ω = 1/4, blue; Ω = 1/16, red). The default parameter values are U 0 = 30, ϕ 0 = 35°, ϕ  w  = 10°, and Ω = 1.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Top row: zonal mean zonal wind (ms−1) seasonal cycle around southern hemisphere winter for ω = 1, γ = 70°, and Ω = 0.5. The fractions confined between the vertical lines represent the time average period for the respective column below it: black for early winter (late fall), blue for midwinter, and red for late winter (early spring). Second row: zonal mean zonal wind (ms−1). Third row: mass streamfunction (kg s−1). Fourth row: vertical structure of temperature (K). Fifth row: eddy momentum flux convergence (ms−2).
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Top: vertically integrated EKE (shading, 106 Jm−2; Equation (1)) and zonal mean zonal wind (contours; contour intervals are 10 ms−1) seasonal cycle at a height of σ = 0.3 for an Earth-like simulation (a) and a simulation with ω = 4, γ = 30°, and Ω = 1/2 (b), the same simulation used for the late winter jet split). Bottom: scatter plot of vertically integrated EKE (106 Jm−2) as a function of the jet strength (ms−1) for an Earth-like simulation (c) and a simulation with ω = 4, γ = 30°, and Ω = 1/2 (d). Each point represents the value of the vertically integrated EKE at the latitude of maximum zonal mean zonal wind in each day.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: The PV (solid) and zonal mean zonal wind (dashed) meridional structure in the summer hemisphere for different parameter values for a temporal mean of days 180–240, vertically averaged between σ = 0.5 and 0.85. Each line is normalized by its maximum value in the summer hemisphere. Black is for γ = 20°, blue is for γ = 50°, and red is for γ = 80°; other parameters are constant, with ω = 1 and Ω = 1/16.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: The PV (shading, potential vorticity potential vorticity unit, PVU, i.e., 10−6 K m2 s−1 kg−1) and zonal mean zonal wind (contours; contour interval 10 m s−1) seasonal cycle at a height of σ = 0.5 for different values of rotation rates (Ω) with γ = 30° and ω = 1.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Model planet-to-star flux ratio spectra for water, carbon monoxide, carbon dioxide, and methane (top to bottom panels). The blue and orange solid curves show the TRANSIT code and the Morley radiative transfer spectra, respectively (Gaussian-smoothed for better visualization). The planetary atmospheric model is the same as in Figure (3), with additional uniform mixing ratios of 10−4 for the respective species in each panel. The stellar model corresponds to a blackbody spectrum of a 1 R ⊙ radius and 5700 K surface-temperature star. The dashed gray lines indicate the flux ratio for planetary blackbody spectra at 1090 and 1620 K (atmospheric maximum and minimum temperatures). The CIA opacity comes from Richard et al. (2012). For H2O and CH4 both models used the line lists from Partridge & Schwenke (1997) and Yurchenko & Tennyson (2014), respectively. For CO2, Morley used Huang et al. (2013) and Huang et al. (2014), whereas TRANSIT used HITEMP. For CO, the Morley models used the line list from Goorvitch (1994), whereas TRANSIT used the HITEMP line list. The spectrum for each species shows a good agreement between TRANSIT and Morley’s models.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: TRANSIT flow chart. The white boxes denote the main routines, the blue boxes the code inputs, and the gray box the output spectrum file. TRANSIT sequentially executes the routines from the top down. The items in brackets are optional steps. The execution consists of two main steps. The initialization step reads the input files, creates the (equi-spaced) wavenumber array, calculates the layer’s altitude and species density and partition function, and computes or reads a tabulated opacity grid (optional). The second main step updates the atmospheric model (if requested) and computes the atmospheric opacity over the spectral range, the light-ray path, the optical depth, and the intensity and flux spectra. Once the initialization is executed, the user can produce multiple spectrum calculations for desired atmospheric models, for example, during an MCMC the code cycles over the bottom section.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Model emission spectra for pure CIA. The blue and green curves show the TRANSIT spectra for HITRAN and Borysow CIA opacities, respectively. The orange curve shows the HITRAN CIA spectrum of C. Morley. All spectra were calculated for an atmospheric model with uniform mole mixing ratios composed of 85% H2 and 15% He, for a planet with a 1 R Jup radius and a surface gravity of 22 m s−2. The inset shows the atmospheric temperature profile as a function of pressure.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Transit geometry observation diagram. The atmospheric model consists of a set of one-dimensional spherically symmetrical shells (gray gradient) around the planet center. All the observed light rays (blue dashed line) travel nearly parallel to each other, and hence the optical depth for each ray depends exclusively on the impact parameter (b), where the path traveled between two layers (blue solid line) is given by ﹩{s}_{i}(b)=\sqrt{{r}_{i}^{2}-{b}^{2}}-\sqrt{{r}_{i+1}^{2}-{b}^{2}}﹩.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Selected simulations demonstrating the most dominant types of seasonal behavior within the parameter space. Plots show the zonal mean zonal wind vertically averaged between σ = 0.25 and 0.5. The x-axis represents the year fraction; the year starts during the southern summer solstice. Column A shows the jet dependence on obliquity (γ) in the case of a short orbital period (ω = 1/8) and an Earth-like rotation rate (Ω = 1), i.e., weak seasonality. Column B shows the jet’s dependence on the orbital period (ω) for a moderate obliquity (γ = 30°) and rotation rate (Ω = 1/2). Columns C and D show the jet’s dependence on the rotation rate (Ω) for an Earth-like orbital period (ω = 1) and an obliquity of 30° and 70°, respectively. Highlighted panels are the representative cases of the distinct jet behavior in the parameter space and are summarized in Figure 3. Note that there is a different color scale for each column.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Zonal mean zonal wind vertically averaged between σ = 0.25 and 0.5 (shading) and surface temperature (contours; contour interval 5 K) for the different jet seasonal cycle regimes detected in the parameter space. These panels are the ones highlighted in Figure 2. The details of each case are summarized in the text.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Comparison of the seasonal cycle of three simulations, Ω = 1, 1/4, and 1/16, with ω = 1, γ = 30°. Top row: temperature at σ = 0.5 (K; shading) and the pattern of the top of the atmosphere forcing (Wm−2; contours). Second row: mass streamfunction at σ = 0.5 (kg s−1; red is southward flow). Third row: zonal mean zonal wind at σ = 0.5 (ms−1). Fourth row: vertical velocity at σ = 0.5 (Pa s−1).
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Equivalent June–August temporal mean of the vertical structure of temperature (K; first row), zonal mean zonal wind (ms−1; second row), and mass streamfunction (kg s−1; third row) that represents the mean meridional circulation (red denotes counterclockwise circulation) for γ = 10° (left column) and 90° (right column) with Ω = 1 and ω = 1/8.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Top row: maximum zonal mean zonal wind speed (ms−1) for a vertical mean between σ = 0.25 and 0.5 in the southern hemisphere during southern hemisphere winter. Bottom row: latitude of maximum winds (shading) and latitude of descending branch of the Hadley cell. In panels (a) and (d), ω = 1; in (b) and (e), γ = 30°; and in (c) and (f), Ω = 1.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Solar phase curves from the Earth-based and New Horizons LORRI observations in Tables 4–10 and 12–13 for all DPs, large KBOs, and satellites observed by New Horizons. All data at phase angles α < 2° are from Earth-based observations summarized in Tables 3 and 11, and all data at phase angles α > 2° are from New Horizons LORRI (filled circles) and Voyager 2 (open circles). See Section 2 for descriptions of the data sets for each object and Figure 4 for details of the near-opposition portion of each solar phase curve. All phase curves are normalized to 0 mag at opposition (α = 0°) to enable direct comparison of their shapes. All lines are fits to the Hapke (2012b) photometric model using parameters given in Table 14 for the DPs, large KBOs, Triton, and Charon. Error bars represent one standard deviation from the mean reflectance in all images at each visit.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Near-opposition portions of all solar phase curves in Figure 3 for each DP, large KBO, and satellites. All phase curves are normalized to 0 mag at opposition (α = 0°) to enable direct comparison of their shapes at phase angles α < 2°.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Relationships between transparency-related Hapke model parameters. Open circles represent hypervolatile surfaces, filled circles describe H2O-rich surfaces, and diamonds represent nonvolatile surfaces or surfaces of undetermined composition. Red data points identify surfaces dominated by forward-scattering regolith grains, blue data points by backscattering grains, and black points by isotropically or symmetrically scattering grains. (a) SHOE amplitude parameter B  oS  vs. the SPPF effective asymmetry parameter g eff for DPs and large KBOs. In most cases, the SHOE is most prominent in regoliths composed of nearly opaque grains (B  oS  > 0.8). Forward-scattering grains typically diminish projected shadows, resulting in low SHOE amplitudes, although Makemake appears to be an exception. (b) Relationship between the SPPF effective asymmetry parameter g eff and single-scattering albedo ﹩{\tilde{\omega }}_{o}﹩ suggests a trend from dominantly backscattering low-albedo particles (g eff < 0) to dominantly forward-scattering (g eff > 0) high-albedo grains. Hypervolatile-rich surfaces consistently have grains that are both highest in single-scattering albedo and forward scattering. Nonvolatile surfaces have low particle albedos and range from moderately backscattering to nearly isotropic or with symmetric forward- and backscattering lobes. The behavior of H2O-rich surfaces tends to lie in between the hypervolatile and nonvolatile surfaces.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: A McGuire & Hapke (1995) “hockey stick” plot showing SPPF c vs. b parameters for all DPs, satellites, and DKBOs observed by New Horizons. Filled circles are objects studied in this work; open circles are the smaller, darker DKBOs studied by Verbiscer et al. (2019b), which include cold and hot classical KBOs, Plutinos, and scattered disk and resonant objects. The thick solid curve is Hapke’s empirical “hockey stick” relation (Hapke 2012a), ﹩c=3.29\exp (-17.4{b}^{2})﹩ − 0.908, that approximates the behavior of a broad range of particulate surfaces and may represent most particles found in planetary regoliths. The surfaces of the smaller DKBOs are more backscattering than those of the DPs. This more strongly backscattering behavior parallels the hockey stick curve as shown as a solid thin curve, but the trend is shifted toward characteristics of smoother, more euhedral particles, b values, by 0.13 ± 0.01. This trend is characteristic of many low-albedo solar system bodies.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Near-opposition portions of solar phase curves of satellites and DPs with (a) volatile-rich and (b) water ice-rich and nonvolatile surfaces, although the surface compositions of 2002 MS4 and 2014 OE394 have not yet been determined. The scatter in the low phase angle points for 2014 OE394 and Ixion is due to the variation in their reflectance with rotation (i.e., rotation curve). The Makemake, Eris, Pluto, Triton, Haumea, Charon, 2002 MS4, and Quaoar observations have all been corrected for variation in reflectance due to their rotation curves. Error bars represent one standard deviation from the mean reflectance in all images at each phase angle. (a) DPs and satellites with hypervolatile-rich surfaces. (b) DPs and large KBOs with H2O-rich (Haumea, Quaoar, and Charon), volatile-poor (Ixion), and undetermined (2002 MS4 and 2014 OE394) surface compositions.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Earth-based rotation curve of the Haumea system (solid line) from Lacerda et al. (2008) and New Horizons LORRI observations acquired at three different epochs in 2007 October (open circles), 2017 January (filled circles), and 2020 May (triangles) (Table 6). All observations are phased to 0 rotation phase and 0° longitude at JD 2454867.042 as defined by Lockwood et al. (2014). See text for further details on the placement of LORRI observations on these rotation curves. The New Horizons observations acquired at α = 8° fall on the Earth-based light curve with amplitude 0.29 mag (Table 3), while those acquired at α = 48° demonstrate that the amplitude of Haumea’s light curve increases at higher phase angles, as expected for a nonspherical body. The dashed line is a two-term Fourier fit to the 2020 LORRI observations with total amplitude 0.6 ± 0.2 mag. Note that the secondary peak at subspacecraft longitude 270° (rotational phase 0.75) in the 2020 LORRI rotation curve coincides with the location of a dark red spot on Haumea identified by Lacerda et al. (2008). Error bars represent one standard deviation from the mean reflectance in all images at each visit.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Floating bar chart showing the nominal values of the CBOE h  C  parameters (circles with center bars) from Table 14 arranged in order of increasing angular width. The corresponding uncertainty ranges (from Table 15) are indicated by shaded boxes. Relative regolith maturity for each object is interpreted to increase from left to right in the plot. Note that the vertical scale is logarithmic. Makemake has been excluded because its available phase angle coverage was insufficient to constrain h  C  in our Hapke model fit. The two leftmost bodies (Triton and Pluto) have hypervolatile-rich surfaces. Of the six rightmost bodies, four are low-albedo objects with nonvolatile surfaces (Ixion, 2014 OE394, 2002 MS4) or H2O-rich surfaces (Quaoar). Charon’s surface is also H2O-rich but is intermediate in maturity. The remaining bodies, H2O-rich Haumea and hypervolatile-rich Eris, appear to have anomalously high albedo surfaces in comparison to the other bodies of similar maturity, although with large uncertainties.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Earth-based V-band rotation curve of Quaoar from Thirouin (2013) (solid line) with total amplitude 0.112 ± 0.011 (Table 3). New Horizons LORRI observations at α = 51° (triangles), α = 66° (crosses), α = 84° (filled circles), and 94° (open circles) fall on the Earth-based rotation curve, demonstrating that the amplitude of Quaoar’s rotation curve does not increase at higher solar phase angles. Error bars represent one standard deviation from the mean reflectance in all images at each visit. Rotation phase 0 is JD 2458400.95.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Hapke parameters from Table 14 with uncertainties from Table 15. For the objects in red, hypervolatiles such as N2 and CH4 play major roles in their surface composition. For the objects in blue, water ice plays a major role in their surface composition. Black circles correspond to parameters for objects with surface compositions dominated by nonvolatiles.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: Polar stereographic display of the volatile species of interest that have surface thermal stability regions at the north pole from 60° to 90° S (species and stability temperature given in the legend). Background data are the Lunar Orbiter Laser Altimeter (LOLA) 100 m pixel−1 shaded relief map. Each ring is 5° latitude. Black arrows on the CO2 map indicate the small thermal stability regions for CO2 at the south pole.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: Polar stereographic display of the volatile species of interest that have surface thermal stability regions at the north pole from 80° to 90° N (species and stability temperature given in the legend). Background data are the Lunar Orbiter Laser Altimeter (LOLA) 100 m pixel−1 shaded relief map. Each ring is 5° latitude.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: The locations of sulfur (yellow), water (blue), hydrogen cyanide (green), and CO2 (purple) in the same color scheme as the regional maps previously shown, at (a) Rozhdestvenskiy W crater at the north pole; (b) Haworth, Shoemaker, and Faustini craters at the south pole; and (c) Amundsen crater at the south pole. While the PSRs at Haworth, Shoemaker, and Faustini are more poleward and in smaller craters than Amundsen and Rozhdestvenskiy W craters, this region spans the final study sites for the VIPER rover landing site and includes Nobile crater, the landing site selected at the time of writing. Major latitude and longitude lines within the figure are labeled.