adsabs/AstroCLIMB huggingface dataset:
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Apophis’s trajectory profile during ECA in the J2000 coordinate frame viewed from different angles. The blue line shows the trajectory. The blue arrows indicate the direction of the asteroid’s movement. The spheres show the Earth in orange, the planet’s rigid Roche limit (RRL) in light blue, and the planet’s fluid Roche limit (FRL) in light green. The Sun’s direction is also given in red. The plot is given in the J2000 Earth-fixed inertial frame. The figure is adapted and updated from M. Hirabayashi (2026).
Paper: The Caltech Mission to Apophis: Accelerating Planetary Science and Planetary Defense
Authors: Adriana Daca, Masatoshi Hirabayashi, Yaeji Kim, Joseph DeMartini, Carol Raymond, Alain Herique, Mark Haynes, Dirk Plettemeier, Bjorn Davidsson, José Andrade
Figure caption: Apophis's spin state at 19:00 on 2029 April 13 UTC. The spin uncertainties were propagated from the measured spin state at the reference epoch provided by recent work (H.-J. Lee et al. 2022). The blue dot at the top indicates the direction of the Earth from Apophis. The color represents the probability in a linear scale, where a darker blue represents a higher probability.
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Light curve resulting from statically stable wavelets centered at ﹩{\bar{f}}_{{\rm{c}}{\rm{y}}{\rm{l}}}﹩ = 0.5, 0.1, and 0.025 and Lz/H0 = 0.13, 0.42, and 0.49. Here the waves are in perfect focus (just shy of ray crossing). In contrast to Figure 8, here the spikes exceed the unocculted flux level. At amplitudes smaller than perfect focus, Abel inversions remain valid (regions A, B, and C in Figure 6).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Occultation light curve with statically stable wavelets at ﹩{\bar{f}}_{{\rm{c}}{\rm{y}}{\rm{l}}}﹩ = 0.5, 0.1, and 0.025 and Lz/H0 = 0.60. We again plot an occultation light curve as distorted by waves. Note that for these values the peak of all spikes remains at or below the unocculted baseline level. This limit corresponds to the boundary between regions B and C in Figure 6.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Simulated light curve for a statically stable wavelet at ﹩{\bar{f}}_{{\rm{c}}{\rm{y}}{\rm{l}}}=0.5﹩, with Lz/H0 = 5.14  and ccrit = 0.75. Here we plot an occultation light curve as distorted by a single wavelet (solid) and the undistorted light curve (dotted). For this wavelet, the end of the upward fluctuation is level with the beginning of the downward fluctuation, resulting in a nonnegative light-curve slope throughout. A statically stable wavelet at a smaller wavelength would result in a discernible spike.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Calculating Occultation Light Curves Using Wavelets: Exponential Atmospheres and the Constraints of Static Stability
Authors: Leslie A. Young, Michael J. Person
Figure caption: Simulated occultation light curve with a statically stable wavelet at ﹩{\bar{f}}_{{\rm{c}}{\rm{y}}{\rm{l}}}=0.5﹩ and Lz/H0 = 0.0032. At this wavelength, the light is scattered to a distance of the characteristic wavelength around the center of the perturbation, but not beyond. Note how tightly confined all light-curve effects are at these small wavelengths.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: An example of a spectrum from 2022 June 25 in the region of the C2 (0, 0) bandhead is shown. The top panel is the molecular emission spectrum plus the absorption and continuum from dust reflected sunlight. The bottom panel shows that spectrum with the solar contribution removed. In the lower panel, many emission lines are quite obvious that cannot be seen in the upper panel, including the C2 (0, 0) bandhead at ∼5165 Å.
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The CN B2Σ+—X2Σ+ order of the spectra for each preperihelion night except 2022 January 15 are shown. There are clearly no CN lines in the spectrum from 18 October 2021 when the comet was at a heliocentric distance of 5.06 au. By the time the comet is at 3.39 au on 2022 April 22, the CN band is well developed. The dashed lines indicate the lowest j-levels of the P branch (right two) and of the R branch (left two).
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The C3 A1Πu—X﹩{}^{1}{{\rm{\Sigma }}}_{g}^{1}﹩ (0, 0, 0)–(0, 0, 0) order of the spectra for each preperihelion night except 2022 January 15 are shown. There are clearly no C3 lines in the spectrum from 2021 October 18 at a heliocentric distance of 5.06 au nor at Rh = 3.39 au on 2022 April 22. By 2022 May 9 at 3.24 au, the Q-branch bandhead at 4050 Å is clearly visible.
Paper: Watching a Comet Turn On: High Spectral Resolving Power Observations of Comet C/2017 K2 (PanSTARRS)
Authors: Anita L. Cochran, Adam J. McKay, Youssef Moulane
Figure caption: The CH A2Δ—X2Π band does not have many lines. No CH lines are visible until 2022 June 10 at Rh = 2.95 au. The spectrum from 2022 May 9 is ambiguous for a line detection.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: The Athena lander in lunar orbit and on the Moon’s south pole, as seen from one of its navigation cameras. The TRIDENT drill is to the left of MSOLO (the white rectangle) between the legs of the lander. The TRIDENT avionics box can be seen in the foreground on both images. On the surface image, the TRIDENT avionics box is covered in dust. Note the crescent Earth in the background. Images: Intuitive Machines.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: VIPER will include three instruments. From left to right: NSS, NIRVSS, and MSOLO.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: The TRIDENT deployment linear stage and drill feed linear stage are used to deploy the footpad to the surface and feed the drill bit and drill head into the ground during drilling. Actuator control and power transmission are accomplished using flex cables.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: PRIME-1 (left) and VIPER (right) missions to the south pole. TRIDENT is mounted to the side of the lander on the PRIME-1 mission and in the middle of VIPER. The Intuitive Machines IM-2 lunar lander, named Athena, is just over 4 m tall, while VIPER stands approximately 2.5 m tall.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: The TRIDENT drill subsystems. The drill is ∼1.75 m tall.
Paper: TRIDENT Ice Mining Drill for Lunar Volatile Prospecting for PRIME-1 and VIPER Missions
Authors: Kris Zacny, Philip Chu, Vincent Vendiola, Gale Paulsen, Paul Creekmore, Samuel Goldman, Jameil Bailey, Philip Ng, Carter Fortuin, Jaqueline Stamboltsian, Alex Wang, Anchal Jain, Paul Chow, Emily Seto, Nicholas Bottomley, Robert Huddleston, Ezra Bailey-Kelly, Raymond Zheng, Aaron Norlinger, Isabel King, Zach Mank, Jack Wilson, Jake Fishman, Helen Xu, Dean Bergman, Erik Mumm, Kiel Davis, Jason Beck, Stella Dearing, Mark Hill, Jackie Quinn, Amy Eichenbaum, Janine Captain, Julie Kleinhenz, Anthony Colaprete, Rick Elphic, Kimberly Ennico-Smith, Darlene S. S. Lim, Zara Mirmalek, David Lees, Valentin T. Bickel, Ariel N. Deutsch, Nicholas C. Schmerr, Kevin Lewis, Benjamin Fernando, Kathryn Gansler
Figure caption: 1 m Class Drill Maturation History.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Target ROIs (white polygons) pointed to by arrows with the site names of D. De Rosa et al. (2012). Pink dotted circles with labels represent named craters listed in the IAU nomenclature. Light blue dots show the distribution of the purported exposed water ice (S. Li et al. 2018b). The colorized shaded map is based on the LOLA DTM, gridded at 40 m resolution in south polar stereographic projection.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Comparison of SP DTMs in the vicinity of CR1. Each dataset is presented as a shaded-relief image in a south polar stereographic projection with an illumination altitude of 30° and an azimuth of 315° clockwise from north. The DTMs shown are as follows. (a) LALT DTM (ID: LALT_GT_SP_NUM; regridded at ~236.90 × 236.90 m). (b) LDEM (ID: LDEM_875S_5M_FLOAT; we used this product as a vertical source of controlled DTMs as described later). (c) One of SPLDEM2021 (ID: Site01_final_adj_5mpp_surf). (d) DTM TC ORTHO (each product shows NoData holes from per-scene coverage and shadow masking), four overlapping DTMs without manual georeferencing (see Table 2 for IDs of CR1; we used this product as a vertical source of controlled DTMs as described later). (e) DEM TC ORTHO (each of them is a composite product that gap-fills across scenes but can introduce horizontal/vertical offsets at joins), ID: DTMTCOw01_00570S897E1937PS. (f) SLDEM2013, 41 DTMs (products with IDs between DTM_MAP_01_S89E200S90E201SC and DTM_MAP_01_S89E240S90E241SC in sequential order). (g) LROC DTM produced by the ESA lander mission (ID: NAC_DTM_ESALL_CR1). (h) LROC DTM produced by the USGS (ID: MOON_LRO_NAC_DEM_89S210E_4mp). (i) CE2 CCD stereo global DEM (ID: CE2_GRAS_DEM_20m_N001_87S000W_A). DTMs around the CR1 region that contain many NoData pixels, have insufficient spatial resolutions, or are publicly inaccessible are not included.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Workflow overview. The pipeline has three stages. (1) Inputs and controls: build controlled TC DTM/LDEM and orthomosaics and assemble a control network with GCPs tied to LOLA. (2) NAC pair processing: seam-aware NACL/NACR coregistration, NACR transform, and local ratio-based normalization yield a seamless NAC mosaic per pair. (3) Multiview SfS and geodetic control: ASP’s parallel_sfs refines the initial DEM using six NAC mosaics; the SfS result is aligned to LOLA (globally and locally), and all NAC orthos are map-projected onto the final SfS DTM at 1 m pixel−1 to form the controlled orthomosaic. A full command-level flowchart appears in the Appendix, which is a full-resolution vector version for zoom-in viewing.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: SfS DTMs gridded with 1 m pixel−1. They are color-coded by their elevations (50% opacity) overlaid on their own shaded reliefs. (a) CR1, (b) GR1, (c) GR2, (d) LP1, (e) MP1, (f) MP2. The spatial extent of each panel is the same as that in Figure 3. The relative height with a range of 55 m is coded with 11 colors, so that each color represents an interval of 5 m in height. Individual color bars of elevation values include both upper and lower limits, which were used to stretch the colors in each map, and are exactly the same as those of the LDEMs in Figure 3 for comparison. NoData pixels are not rendered, allowing the black backgrounds to remain visible. White closed polylines show our specified areas that are suitable for future landing/roving activities. The shaded-relief base map of each DTM is visually enhanced with 10× vertical exaggeration and light illumination from above each DTM.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: The total population of valid overlapping pixels among individual orthoimages. (a) CR1, (b) GR1, (c) GR2, (d) LP1, (e) MP1, (f) MP2. Each of the orthomosaics in Figure 10 was produced from these orthoimage pixels. The spatial extents and white polygons are the same as those in Figure 9. NoData pixels of DTMs in Figure 9 (orthoimage pixel values ≤0.004) are counted as zero.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Close-up views of the six target sites, represented by color-coded elevation of the 10 m pixel−1 SPLDEM2021 mosaic (M. K. Barker et al. 2023) combined with shaded relief. (a) CR1, (b) GR1, (c) GR2, (d) LP1, (e) MP1, (f) MP2. The relative height range of 55 m is divided into 11 5 m intervals. White polygons indicate areas we identify as suitable for future landing/roving. The shaded relief is visually enhanced with 10× vertical exaggeration and overhead illumination.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Close-ups of an NACL/NACR seam treated by two methods. (a) Default ASP lronac2mosaic.py mosaicking leaves a visible seam. (b) Our seam-aware registration plus local ratio normalization produces a seamless merge. The width of each panel is 260 pixels (~224 m). Orange arrows indicate small craters straddling the seam whose shapes are corrected after the NACR transform. Black arrows show a horizontal (sample) position of the same seam of each mosaic. An image coordinate of the upper left corner pixel (sample, line) is (2340, 17685). LROC NAC ID M131418183 (a CR1 source image).
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Six source orthoimages of CR1. The spatial extent and a white ROI polygon in each view are the same as those of CR1 in Figure 9(a). NoData pixels (orthoimage pixel values ≤0.004) are not rendered, allowing the blue backgrounds to remain visible. An original NAC image ID is shown at the bottom of each panel.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: The orthomosaics of our SfS DTMs. Image resolution is ~1 m pixel−1. (a) CR1, (b) GR1, (c) GR2, (d) LP1, (e) MP1, (f) MP2. NoData pixels are not rendered, allowing the light blue backgrounds to remain visible. Each orthomosaic is contrast-enhanced. The spatial extents and white polygons are the same as those in Figure 9.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Pipeline to prepare datasets of horizontal and vertical control sources (controlled TC DTMs and controlled TCOrtho mosaics). For CR1 and GR2, we used the smoothed LDEMs for vertical controls. Application boxes include commands with specific arguments that were required in its processing.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Full command-level flow for image preparation, multiview SfS, and control to LOLA (detailed version of Figure 5).
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Log–log plots showing rms bidirectional slopes derived from our MP1 DTM and MMDTM2024.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Close-up comparisons of the orthomosaic and shaded-relief renderings for the six newly generated DTMs. Shaded-relief maps were produced using illumination from directly overhead (solar altitude = 90°). For each map, we inverted the color ramp from black-to-white to white-to-black to better approximate the visual appearance of the orthomosaics derived from NAC orthoimages acquired under multidirectional illumination. Craters visible in both the orthomosaic and shaded relief are highlighted with green circles, while those discernible only in the orthomosaic are marked with red circles. The white lines correspond to the segments of the white polygons depicted in Figure 9. NoData pixels have been omitted to preserve the light blue background.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Differences in elevation between individual SfS DTM pixels and valid LOLA RDR points. (a) CR1, (b) GR1, (c) GR2, (d) LP1, (e) MP1, (f) MP2. Base maps are orthomosaics. NoData pixels are not rendered, allowing the light blue backgrounds to remain visible. Histograms of individual elevation differences are shown in Figure 17, and their statistics are listed in Table 6. The spatial extents and white polygons are the same as those in Figure 9.
Paper: LROC NAC-derived Meter-scale Topography of the Moon’s South Polar Landing Sites: Digital Terrain Models and Their Quality Assessments
Authors: Ryodo Hemmi, Hiroka Inoue, Hiroshi Kikuchi, Hiroyuki Sato, Hideaki Miyamoto, Hisashi Otake, Mitsuo Yamamoto
Figure caption: Examples of artifacts included in DTMs. The shaded-relief base maps are the same as those in Figure 9. The close-up views have been cropped to highlight the artifacts. Pink arrowheads outline the artifacts. White lines are part of the white polygons in Figure 9. Such artifacts were not identified on the shaded-relief map of LP1. NoData pixels are not rendered, allowing the light blue backgrounds to remain visible. The shaded-relief base map of each DTM is visually enhanced by using GDAL application gdaldem with 10× vertical exaggeration and light illumination from above each DTM.