Creating HiRISE digital elevation models for Mars using the open-source Ames Stereo Pipeline

Hepburn, Adam; Holt, Tom; Hubbard, Bryn; Ng, Felix

doi:10.5194/gi-8-293-2019

Cited by 12 publications

(4 citation statements)

References 42 publications

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“…We use the raw and unprocessed HiRISE images, that is, the Experimental Data Record products, to do bundle adjustment and produce a DEM of the study region using a stereo pair and the Ames Stereo Pipeline software (Beyer et al., 2018; Hepburn et al., 2019). This DEM is then used to orthorectify all the available images.…”

Section: Methodsmentioning

confidence: 99%

Thickness of the Seasonal Deposits at the Martian North Polar Region From Shadow Variations of Fallen Ice Blocks

Xiao,

et al. 2024

JGR Planets

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The seasonal deposition and sublimation of CO2 constitute a major element in the Martian volatile cycle. Here, we propose to use the shadow variations of the ice blocks at the foot of the steep scarps of the North Polar Layered Deposits (NPLD) to infer the vertical evolution of the seasonal deposits. We conduct an experiment at a steep scarp centered at (85.0°N, 151.5°E). We assume that no snowfall remains on top of the selected ice blocks, the frost ice layer is homogeneous around the ice blocks and their surroundings, and no significant moating is present. We show that the average thickness of the seasonal deposits due to snowfalls in Mars Year 31 is 0.97 ± 0.13 m at Ls = 350.7° in late winter. The large depth measured makes us wonder if snowfalls are more frequent and violent than previously thought. Meanwhile, we show that the average frost thickness in Mars Year 31 reaches 0.64 ± 0.18 m at Ls = 350.7° in late winter. Combined, the total thickness of the seasonal cover in Mars Year 31 reaches 1.63 ± 0.22 m at Ls = 350.7° in late winter, continuously decreases to 0.45 ± 0.06 m at Ls = 42.8° in middle spring and 0.06 ± 0.05 m at Ls = 69.6° in late spring. These estimates are up to 0.8 m lower than the existing Mars Orbiter Laser Altimeter results during the spring. Meanwhile, we observe that snow in the very early spring of Mars Year 36 can be 0.36 ± 0.13 m thicker than that in Mars Year 31. This study demonstrates the dynamics of the Martian climate and emphasizes the importance of its long‐term monitoring.

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Section: Methodsmentioning

confidence: 99%

Thickness of the Seasonal Deposits at the Martian North Polar Region From Shadow Variations of Fallen Ice Blocks

Xiao,

et al. 2024

JGR Planets

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“…We use the raw and unprocessed HiRISE images, that is, the Experimental Data Record (EDR) products, to do bundle adjustment and produce a DEM of the study region using a stereo pair and the Ames Stereo Pipeline (ASP) software (Beyer et al, 2018;Hepburn et al, 2019).…”

Section: Bundle Adjustment Dem Generation and Image Orthorectificationmentioning

confidence: 99%

Are seasonal deposits in spring at the Martian North Pole much shallower than previously thought?

Xiao,

et al. 2023

Preprint

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The seasonal deposition and sublimation of CO constitute a major element in the Martian volatile cycle. Here, we propose to use the shadow variations of the ice blocks at the foot of the steep scarps of the North Polar Layered Deposits (NPLDs) to infer the vertical evolution of the seasonal deposits at high polar latitudes. We conduct an experiment at a steep scarp centered at (85.0°N, 151.5°E). We show that the average thickness of the seasonal deposits due to snowfalls in Mars Year 31 is 0.97±0.13 m at Ls = 350.7° in late winter, which then gradually decreases in springtime. The large snow depth measured makes us wonder if snowfalls are more frequent and violent than previously thought. Meanwhile, we show that the average frost thickness due to direct condensation in Mars Year 31 reaches 0.64±0.18 m at Ls = 350.7° in late winter and quasi-linearly decreases towards the summer solstice. Combined, the total thickness of the seasonal cover in Mars Year 31 reaches 1.63±0.22 m at Ls = 350.7° in late winter, continuously decreases to 0.45±0.06 m at Ls = 42.8° in middle spring and 0.06±0.05 m at Ls = 69.6° in late spring. These estimates are up to 0.8 m lower than the existing MOLA results during the spring, which can be mainly attributed to MOLA-related biases. In terms of interannual variations, we observe that snow in the very early spring of Mars Year 36 can be 0.36±0.13 m deeper than that in Mars Year 31.

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“…To reduce the errors caused by uncertainty in the camera pointing information, bundle adjustment optimization of all input images before dense image matching was implemented. It helps ensure that point clouds are internally consistent 13 . Then we adopted SGM stereo algorithms to produce a disparity map.…”

Section: Single Photogrammetry Point Cloud Generationmentioning

confidence: 99%

“…In recent years, the global registration algorithm has been widely used, which mainly uses block adjustment method to estimate the global optimal transformation parameters in order to improve the alignment accuracy and reliability [5][6][7][8][9][10] . Point cloud fusion algorithms are classified into point-based integration 11 , mesh-based integration 12 , and voxel-based integration 13 , which helps to generate a complete point cloud model from multiple point clouds.…”

Section: Introductionmentioning

confidence: 99%

Reliability-weighted fusion of multiview photogrammetric point clouds for 3D terrain reconstruction of the lunar surface

Xu¹,

Chen²,

Xu³

et al. 2023

Earth and Space: From Infrared to Terahertz (ESIT 2022)

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Benefitting from advances in photogrammetry and computer vision, 3D point clouds generated from dense image matching have been proved to be an accurate, reliable, and cost-effective data source for lunar topographic mapping. To achieve a full coverage mapping of the lunar surface, a merging of point clouds generated from multiple observations is mandatory. Due to the limit of dense matching accuracy and accumulative registration errors, integrated point clouds normally suffer from disturbed stratification, outliers, and redundant points, resulting in sharp edges between the seams of the fused point clouds. To address the seaming problems of merged point clouds and achieve a seamless fusion result, a weighted fusion strategy evaluating the reliability of points from triangulation errors in the photogrammetry process is proposed. The global registration and post-processing of point clouds are also addressed to optimize the result. With comparisons to other software outputs, a DEM with a resolution of 6 m/pixel is produced, with a lower bias to ground truth and better visualization. As a result, the proposed method can improve the completeness and precision of digital surface model to a certain extent and satisfy the application requirements.

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Creating HiRISE digital elevation models for Mars using the open-source Ames Stereo Pipeline

Cited by 12 publications

References 42 publications

Thickness of the Seasonal Deposits at the Martian North Polar Region From Shadow Variations of Fallen Ice Blocks

Thickness of the Seasonal Deposits at the Martian North Polar Region From Shadow Variations of Fallen Ice Blocks

Are seasonal deposits in spring at the Martian North Pole much shallower than previously thought?

Reliability-weighted fusion of multiview photogrammetric point clouds for 3D terrain reconstruction of the lunar surface

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