adsabs/AstroCLIMB huggingface dataset:
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for Rheasilvia outer flank, blue, greenish rims (Rof2). (b). Crater size–frequency distribution and randomness plots calculated from ADM for Rheasilvia outer flank, blue, greenish rims (Rof2).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for Rheasilvia outer flank, greenish-yellow (Rof1). (b). Crater size–frequency distribution and randomness plots calculated from ADM for Rheasilvia outer flank, greenish-yellow (Rof1).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for the Oppia crater. (b). Crater size–frequency distribution and randomness plots calculated from ADM for the Oppia crater.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: (a). Crater size–frequency distribution and randomness plots calculated from LDM for Octavia crater. (b). Crater size–frequency distribution and randomness plots calculated from ADM for the Octavia crater.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Color-composite image of LOLA roughness, with each baseline assigned to a different color. White boxes are the current 13 Artemis III candidate regions.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Height differences of spots <1 m apart poleward of 80° S before (left panel) and after (right panel) the track adjustment process (note the difference in vertical scale). Each panel is a 2D histogram with each column normalized by the total number of points in that column. The color scale gives the fraction of each column’s total within each bin. The solid white lines are the median and interquartile range of each column. Dashed lines show a simplified model that ignores sub-footprint terrain roughness but has ACR geolocation errors of 7.00/7.00/0.40 m (magenta), 1.00/1.00/0.15 m (red), and 0.00/0.00/0.00 m (black).
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure 3, but for NAC image M151364517. Points labeled A–C are examples of likely spurious noise points.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Effective resolution in meters (left), rms elevation uncertainty in meters (middle), and rms slope uncertainty in degrees (right) for the 80 km tile centered at (−114 km, −114 km) for a pixel scale of 20 m pixel−1. The color scale limits correspond to the 1st and 99th percentiles of each panel.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: The rms elevation error (left) and rms slope error (right) as a function of effective resolution for a pixel scale of 20 m pixel−1. The color scale gives the fraction within a bin relative to the total within that bin’s column. The dashed white lines are the piecewise linear spline fits.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Close-up of box A in Figures 9 and 10 showing slope (left column) and roughness (right column) on 200 m (top) and 1600 m (bottom) baselines.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: 200 m baseline slope in degrees (left) and roughness in meters (right). The roughness color scale ranges from the 2nd to the 98th percentile.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure 9, but for a 1600 m baseline.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Distribution of ACR offsets for all track segments in 80°–90° S. Note that the radial offsets have been scaled by a factor of 10 for clarity.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: (a) Subregion of a 20 m pixel−1 map-projected NAC image M1188426614; (b) 20 m pixel−1 rendered LDEM; (c) LDEM effective resolution in meters; (d) LDEM counts pixel–1. The 1 km long arrows indicate the direction to the south pole (orange) and stereographic +X/+Y (purple/brown).
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Hillshade of LDEM showing the locations of NAC images in Figures 3–4 and A12–A18.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A12, but for NAC image M1311409938.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A12, but for NAC image M155368056.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A12, but for NAC image M139356343.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Box plots of FeO (left), high-Ca pyroxene (middle), and low-Ca pyroxene (right) for the k-means classes. Each box shows the median (horizontal line), mean (plus sign), interquartile range (box edges), and 9th/91st percentiles (whiskers).
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: 100 m baseline slope in degrees (left) and roughness in meters (right). Map projection is stereographic centered at the pole. The roughness color scale ranges from the 2nd to the 98th percentile.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A19, but for a 1600 m baseline.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A12, but for NAC image M154940551.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A12, but for NAC image M1312308500.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A12, but for NAC image M184288222.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A19, but for a 200 m baseline.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A19, but for a 800 m baseline.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure A19, but for a 400 m baseline.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: Standard deviation of each frame for cloud movies between sol 150 and 300 plotted against sol number and LS. The orange box between sol 236, LS 111.93°, to sol 310, LS 147.52°, encompasses the overall time period when water-ice clouds were observed, with the peak period seen between sol 284, LS 134.59°, to sol 294, LS 139.5°.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: MFS-processed frame from sol 292 (left) containing water-ice cloud features and from sol 319 (right) containing dust cloud features toward the top right corner of the frame.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: Functional box-counting method used to determine the resolution dependence of cloud feature fraction calculations. The top is the original image with L = 0.1 km pixel−1, and the bottom is degraded to L = 0.8 km pixel−1. Unprojected images are used here for visualization purposes only.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: Graph of the standard deviation vs. cloudiness index. The frames with standard deviations above 9, the dashed blue line, contain water-ice cloud features, and standard deviations below 5, dotted green line, do not contain any water-ice cloud features. Cloud frames with a standard deviation between 5 and 9 would require further investigation.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: Mean frame subtracted frame from sol 247, 292, 294 and 321, their corresponding histograms followed by three sets of binary images using three different thresholding techniques: mean thresholding, Otsu thresholding, and same-value thresholding using 0.55. Unprojected frames are used for showcasing as they are visually better suited.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: (a) Image of Earth clouds (credit: Author’s own photograph, 2021). (b) Corresponding 2D FFT of Earth clouds, and (c) NavCam image of clouds from sol 292 (d) with the corresponding 2D FFT of Mars clouds.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: (a) Fractional sky cover in log scale against the cloudiness index, (b) PPR against the cloudiness index, and (c) FSC against PPR in log–log space.
Paper: Geometric Properties of Water-ice Clouds as Observed from Jezero Crater in the First 600 sols with the NavCam Instrument On Board the Mars2020 Rover, Perseverance
Authors: Priya Patel, Leslie Tamppari, Manuel de la Torre Juárez, Mark Lemmon, Andrew Coates, Michael Wolff, Daniel Toledo, Graziella Branduardi-Raymont, Geraint Jones, Charissa Campbell, John Moores, Justin Maki, Jacqueline Ryan
Figure caption: Panel (a) MFS-processed and projected frame at h = 40 km from sol 292 containing cloud features, and (b) MFS-processed frame from sol 321 containing no cloud features (noisy frame). Panels (c) and (d) are their respective radially averaged power spectra. Panel (e) shows the overlaid power spectra, and panel (f) shows the ratio of the two spectra, revealing where in the wavelength space the cloud features lie.
Paper: VLT/MUSE Characterization of Dimorphos Ejecta from the DART Impact
Authors: Brian P. Murphy, Cyrielle Opitom, Colin Snodgrass, Matthew M. Knight, Jian-Yang Li, Nancy L. Chabot, Andrew S. Rivkin, Simon F. Green, Paloma Guetzoyan, Daniel Gardener, Julia de León
Figure caption: All white-light images from the NFM portion of our campaign, with AO online. Morphological evolution of the ejecta cone is seen in panels (b) and (c), before gravitational interactions with the binary begin to curve the bases of the ejecta cone edges into spiral features by panels (d) and (e). By panel (f), the northern spiral has detached from the central system and propagates anti-sunward until panel (g). Intensities are in units of 10−20 erg s−1 cm−2. Convert to mks units using 1 erg = 10−7J and 1 cm2 = 0.0001 m2. The yellow arrow indicates the projected angle toward the Sun, the cyan arrow represents heliocentric orbital motion of the system, and the red arrow is the DART spacecraft approach angle. Lengths of arrows are arbitrarily varied for clarity.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Linear fit to phase curve of (38628) Huya in c and o filters, with two-dimensional histograms showing density plots of error distributions of linear phase coefficient and absolute magnitude. Best-fit function extended to α = 0° for ease of viewing any potential opposition surge. Note the nominally negative β  c  value, whose associated uncertainty nevertheless makes it consistent with a flat-sloped phase curve, consistent with atmosphereless surface reflectance.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Upper plots: linear phase coefficients in ATLAS c (left, black squares) and o (right, black squares), calculated from the phase angle range 0.1° ≤ α ≤ 6°, with literature values in Johnson–Cousins broadband filters (blue: B; green: V; red: R; gray: I) with which ATLAS filters exhibit significant overlap. Lower plots: upper plots magnified for clarity. AC16: Alvarez-Candal et al. (2016); AL18: Ayala-Loera et al. (2018); Bu03: Buratti et al. (2003); B97: Buie et al. (1997); B06: Bagnulo et al. (2006); R05: Rousselot et al. (2005); R06: Rabinowitz et al. (2006); R07: Rabinowitz et al. (2007); SJ02: Sheppard & Jewitt (2002); SR02: Schaefer & Rabinowitz (2002).
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Upper row: Lomb–Scargle periodogram power spectra for 2012 TW236 in the o (orange), c (cyan), and combined c and o (blue) filters. The black dashed and dotted lines represent the 95% and 99.7% false-alarm probability levels. Lower row: the o (orange, left), c (cyan, center), and combined c and o (right) data sets of 2012 TW236, each phase-folded to the rotation period value corresponding to maximum peak in the power spectrum. The combined filter data set shows a clear sinusoidal light curve.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Plots of phase-angle-corrected reduced magnitude vs. MJD in ATLAS c (turquoise, upper) and o (orange, upper) and phase curves of reduced magnitude vs. phase angle in ATLAS c (turquoise, lower) and o (orange, lower) for (60558) Echeclus. Red points denote observations taken from nights with ≥3 observations of which 75% are brighter than 2σ from the object’s sigma-clipped median magnitude. Magenta points denote observations within a 30 days bin whose median magnitude is 0.2 mag and 1 standard deviation brighter than the object’s sigma-clipped median magnitude.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Best-fit linear phase curves for all objects in our sample, divided by filter (c filter left, o filter right) and dynamical classification, spanning the phase angle range of each data set in each filter. All phase curves are normalized to 0 mag at opposition (α = 0 deg) to enable comparison of slope values.
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption: Plots of tested parameter pairs derived from ATLAS observations for our full object sample (first column); Centaurs, JFCs, and Transition Objects (second column); KBOs (third column); dwarf planets (fourth column); and non-dwarf planets (last column).
Paper: Phase Curves of Kuiper Belt Objects, Centaurs, and Jupiter-family Comets from the ATLAS Survey
Authors: Matthew M. Dobson, Megan E. Schwamb, Susan D. Benecchi, Anne J. Verbiscer, Alan Fitzsimmons, Luke J. Shingles, Larry Denneau, A. N. Heinze, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young
Figure caption:  c and o phase curves of Haumea, before (upper plots) and after (lower plots) correction for rotational modulation. Linear best-fit functions plotted as black line, with residuals from the fit displayed beneath each plot.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: CSFDs of PSRs for two simulated clones of the 80 × 80 km tiles centered at (−273, −273) km (left) and (−39, −39) km (right). Each point represents an increment of 1 pixel (4 × 10−4 km2) in PSR area. Gaps between LOLA laser spots increase in size and number moving farther from the pole, causing the recovered CSFD (orange) to be progressively lower than the true CSFD (blue) farther from the pole. All else being equal, the completeness rate decreases as PSR size decreases because smaller PSRs are more likely to lie in gaps between LOLA spots.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Fractional error in recovered PSR area for two simulated clones of the 80 × 80 km tiles centered at (−273, −273) km (left) and (−39, −39) km (right). Fractional error is defined in the sense of (recovered area—true area)/true area. The x-axis is the recovered PSR area. Blue points are individual PSRs, with a small random offset added in x and y to show point density more clearly. Orange circles with error bars denote the mean and standard deviation.
Paper: A New View of the Lunar South Pole from the Lunar Orbiter Laser Altimeter (LOLA)
Authors: Michael K. Barker, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber, James W. Head, Xiaoli Sun
Figure caption: Same as Figure 23, but showing the false-positive rate for individual PSR pixels within PSRs of a given area. The false-positive fraction is defined as the fraction of pixels within a PSR that are incorrectly classified as permanently shadowed.