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Journal articles on the topic 'MOLA- Mars Orbiting Laser Altimeter'

Author: Grafiati
Published: 4 June 2025
Last updated: 23 June 2025

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1

Shashank.B.H, Shreesha.R, Vineeth.K.V, and M. N. Bharath. "Review on Entry, Descent, Landing of Rovers on Mars." Journal of Industrial Mechanics 3, no. 3 (2018): 70–75. https://doi.org/10.5281/zenodo.2378745.

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Humans are trying to explore the solar system and the moon was the first. Since the recent decades the interest has shifted towards so called twin planet of Earth. Martian surface having similar features reminiscent both of impact craters of Moon and the various desert and polar ice caps of Earth. Landers and Rovers are the most effective ways to explore Mars in this existing Technology. This is a company’s Hercules job of taking the rover or Lander to the surface. The most crucial part of this type of missions is entry Descent and landing of the instruments on the surface. This process involves a lot of complicated technologies and accuracy in execution; this is discussed in the forthcoming papers
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2

Shashank.B.H, Shreesha.R, Vineeth.K.V, and M. N. Bharath. "Review on Entry, Descent, Landing of Rovers on Mars." Journal of Industrial Mechanics 3, no. 3 (2018): 70–75. https://doi.org/10.5281/zenodo.2378947.

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Humans are trying to explore the solar system and the moon was the first. Since the recent decades the interest has shifted towards so called twin planet of Earth. Martian surface having similar features reminiscent both of impact craters of Moon and the various desert and polar ice caps of Earth. Landers and Rovers are the most effective ways to explore Mars in this existing Technology. This is a company’s Hercules job of taking the rover or Lander to the surface. The most crucial part of this type of missions is entry Descent and landing of the instruments on the surface. This process involves a lot of complicated technologies and accuracy in execution; this is discussed in the forthcoming papers
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3

Kolb, Kelly J., and Chris H. Okubo. "Coregistration of Mars Orbiter Laser Altimeter (MOLA) topography with high-resolution Mars images." Computers & Geosciences 35, no. 12 (2009): 2304–13. http://dx.doi.org/10.1016/j.cageo.2009.04.008.

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4

Anangonó-Tutasig, Ronny Steveen, Francisco Javier De Cos Juez, and Susana Fernández Menéndez. "High-resolution topography of Gusev crater using CTX data (Mars)." Geogaceta 75 (June 29, 2024): 91–94. http://dx.doi.org/10.55407/geogaceta100671.

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High-resolution Digital Terrain Models (DTMs) of Mars are both limited and crucial for studying surface processes. The available DTMs generated from Mars Orbiter Laser Altimeter (MOLA) and High-Resolution Stereo Camera (HRSC) data offer limited resolution for working on a metre scale. The MER-A mission’s exploration of the Gusev crater was based on the data provided by MOLA and HRSC. However, with the introduction of the stereoscopic images obtained by the Context Camera (CTX) on board the Mars Reconnaissance Orbiter (MRO), it has been possible to generate topographic data with greater detail, significantly improving the MOLA and HRSC data. This has resulted in the generation of new DTMs with a resolution of ~5 m/pixel. Comparative analysis of these CTX DTMs with the MOLA and HRSC data provides an updated perspective of the Gusev topography and its geological features. The prominent advantage of using CTX stereo images lies in their wide coverage, as they have mapped 99.9% of the Martian surface. This wide coverage allows the creation of high-resolution models that will prove invaluable for future studies and missions.
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5

Zuber, Maria T., David E. Smith, Roger J. Phillips, et al. "Shape of the northern hemisphere of Mars from the Mars Orbiter Laser Altimeter (MOLA)." Geophysical Research Letters 25, no. 24 (1998): 4393–96. http://dx.doi.org/10.1029/1998gl900129.

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6

Xiao, Haifeng, Alexander Stark, Hao Chen, and Jürgen Oberst. "Recomputation and Updating of MOLA Geolocation." Remote Sensing 14, no. 9 (2022): 2201. http://dx.doi.org/10.3390/rs14092201.

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The Mars Orbiter Laser Altimeter (MOLA) Precision Experiment Data Records (PEDR) serve as the geodetic reference of Mars. However, these MOLA footprints were geolocated using outdated auxiliary information that dates back to 2003. In this study, we recompute the MOLA PEDR footprint locations and investigate the impact of the updated spacecraft orbit model and Mars rotational model on MOLA’s geolocation. We observe quasi-exponential increases near the poles of up to 30 m in the recomputation residuals for the nadir profiles. Meanwhile, we demonstrate that limitations exist in the stored MOLA PEDR attitude records, which can shift the footprint up to hundreds of meters laterally and several meters radially. The usage of the Navigation and Ancillary Information Facility (NAIF)-archived attitude information instead can circumvent this issue and avoid the approximation errors due to discrete samplings of the attitude information used in geolocation by the PEDR dataset. These approximation errors can be up to 60 m laterally and 1 m radially amid controlled spacecraft maneuvers. Furthermore, the incorporation of the updated spacecraft orbit and Mars rotational model can shift the MOLA profiles up to 200 m laterally and 0.5 m radially, which are much larger in magnitude than the aforementioned dramatic increases near the poles. However, the shifted locations of the reprocessed profiles are significantly inconsistent with the PEDR profiles after the global cross-over analysis.
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7

Montgomery, David R., and Alan Gillespie. "Formation of Martian outflow channels by catastrophic dewatering of evaporite deposits." Geology 33, no. 8 (2005): 625–28. http://dx.doi.org/10.1130/g21270ar.1.

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Abstract Geological mapping based on topographic analysis of Mars Orbiter Laser Altimeter (MOLA) data, together with photointerpretation of Mars Orbiter Camera (MOC) images and thermodynamic and heat-flow considerations, frame a new hypothesis for the formation of Martian outflow channels through catastrophic dewatering of evaporite deposits. MOLA transects across Valles Marineris show that the valley is located at the crest of a 3-km-high topographic bulge on the flank of the much larger Tharsis Rise. Interpretation of MOC images showing layered deposits within Valles Marineris as unconformably underlying Hesperian-age lava flows means that these thick deposits, thought to contain hydrous sulfates, were heated by an increased geothermal gradient due to development of Tharis. Increased temperatures adequate to dehydrate hydrous evaporites would trigger significant volumetric expansion and catastrophically release tremendous amounts of overpressured water.
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8

Ivanov, Anton B., and Duane O. Muhleman. "Opacity of the Martian atmosphere from the Mars Orbiter Laser Altimeter (MOLA) observations." Geophysical Research Letters 25, no. 24 (1998): 4417–20. http://dx.doi.org/10.1029/1998gl900060.

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9

Williams, Rebecca M. E., and Roger J. Phillips. "Morphometric measurements of martian valley networks from Mars Orbiter Laser Altimeter (MOLA) data." Journal of Geophysical Research: Planets 106, E10 (2001): 23737–51. http://dx.doi.org/10.1029/2000je001409.

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10

Abramov, O., and A. McEwen. "Technical note: An evaluation of interpolation methods for Mars Orbiter Laser Altimeter (MOLA) data." International Journal of Remote Sensing 25, no. 3 (2004): 669–76. http://dx.doi.org/10.1080/01431160310001599006.

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11

Head, James W., Mikhail Kreslavsky, Harald Hiesinger, et al. "Oceans in the past history of Mars: Tests for their presence using Mars Orbiter Laser Altimeter (MOLA) data." Geophysical Research Letters 25, no. 24 (1998): 4401–4. http://dx.doi.org/10.1029/1998gl900116.

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12

Wang, Binliang, Shuangming Zhao, Xinyi Guo, and Guorong Yu. "A Mars Local Terrain Matching Method Based on 3D Point Clouds." Remote Sensing 16, no. 9 (2024): 1620. http://dx.doi.org/10.3390/rs16091620.

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To address the matching challenge between the High Resolution Imaging Science Experiment (HiRISE) Digital Elevation Model (DEM) and the Mars Orbiter Laser Altimeter (MOLA) DEM, we propose a terrain matching framework based on the combination of point cloud coarse alignment and fine alignment methods. Firstly, we achieved global coarse localization of the HiRISE DEM through nearest neighbor matching of key Intrinsic Shape Signatures (ISS) points in the Fast Point Feature Histograms (FPFH) feature space. We introduced a graph matching strategy to mitigate gross errors in feature matching, employing a numerical method of non-cooperative game theory to solve the extremal optimization problem under Karush–Kuhn–Tucker (KKT) conditions. Secondly, to handle the substantial resolution disparities between the MOLA DEM and HiRISE DEM, we devised a smoothing weighting method tailored to enhance the Voxelized Generalized Iterative Closest Point (VGICP) approach for fine terrain registration. This involves leveraging the Euclidean distance between distributions to effectively weight loss and covariance, thereby reducing the results’ sensitivity to voxel radius selection. Our experiments show that the proposed algorithm improves the accuracy of terrain registration on the proposed Curiosity landing area’s, Mawrth Vallis, data by nearly 20%, with faster convergence and better algorithm robustness.
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13

Eyton, J. Ronald. "Unusual Displays of DEMs." Cartographic Perspectives, no. 50 (March 1, 2005): 7–23. http://dx.doi.org/10.14714/cp50.414.

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Three procedures for producing new ways to visualize landforms as maps or images derived from Digital Elevation Models (DEMs) are given. One procedure is used to create a highly detailed circular gray scale image from an azimuthal distribution. A second procedure utilizes the principles associated with x-ray tomography for the construction of a volumetric map from DEM cross-sectional ‘slices’. The conversion of a DEM to a Digital Distance Model (DDM) comprises the third procedure, to provide ‘side-looking’ views of the DEM in a variety of map formats including stereograms. DEMs generated from Mars Orbital Laser Altimeter (MOLA) data were used to produce illustrations utilizing the three procedures.
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14

Tao, Yu, Greg Michael, Jan-Peter Muller, Susan J. Conway, and Alfiah R. D. Putri. "Seamless 3D Image Mapping and Mosaicing of Valles Marineris on Mars Using Orbital HRSC Stereo and Panchromatic Images." Remote Sensing 13, no. 7 (2021): 1385. http://dx.doi.org/10.3390/rs13071385.

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A seamless mosaic has been constructed including a 3D terrain model at 50 m grid-spacing and a corresponding terrain-corrected orthoimage at 12.5 m using a novel approach applied to ESA Mars Express High Resolution Stereo Camera orbital (HRSC) images of Mars. This method consists of blending and harmonising 3D models and normalising reflectance to a global albedo map. Eleven HRSC image sets were processed to Digital Terrain Models (DTM) based on an opensource stereo photogrammetric package called CASP-GO and merged with 71 published DTMs from the HRSC team. In order to achieve high quality and complete DTM coverage, a new method was developed to combine data derived from different stereo matching approaches to achieve a uniform outcome. This new approach was developed for high-accuracy data fusion of different DTMs at dissimilar grid-spacing and provenance which employs joint 3D and image co-registration, and B-spline fitting against the global Mars Orbiter Laser Altimeter (MOLA) standard reference. Each HRSC strip is normalised against a global albedo map to ensure that the very different lighting conditions could be corrected and resulting in a tiled set of seamless mosaics. The final 3D terrain model is compared against the MOLA height reference and the results shown of this intercomparison both in altitude and planum. Visualisation and access mechanisms to the final open access products are described.
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15

Jarmołowski, Wojciech, and Jacek Łukasiak. "A Study on Along-Track and Cross-Track Noise of Altimetry Data by Maximum Likelihood: Mars Orbiter Laser Altimetry (Mola) Example." Artificial Satellites 50, no. 4 (2015): 143–55. http://dx.doi.org/10.1515/arsa-2015-0012.

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Abstract The work investigates the spatial correlation of the data collected along orbital tracks of Mars Orbiter Laser Altimeter (MOLA) with a special focus on the noise variance problem in the covariance matrix. The problem of different correlation parameters in along-track and crosstrack directions of orbital or profile data is still under discussion in relation to Least Squares Collocation (LSC). Different spacing in along-track and transverse directions and anisotropy problem are frequently considered in the context of this kind of data. Therefore the problem is analyzed in this work, using MOLA data samples. The analysis in this paper is focused on a priori errors that correspond to the white noise present in the data and is performed by maximum likelihood (ML) estimation in two, perpendicular directions. Additionally, correlation lengths of assumed planar covariance model are determined by ML and by fitting it into the empirical covariance function (ECF). All estimates considered together confirm substantial influence of different data resolution in along-track and transverse directions on the covariance parameters.
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16

Kreslavsky, M. A., and J. W. Head. "Kilometer-scale slopes on Mars and their correlation with geologic units: Initial results from Mars Orbiter Laser Altimeter (MOLA) data." Journal of Geophysical Research: Planets 104, E9 (1999): 21911–24. http://dx.doi.org/10.1029/1999je001051.

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17

Sakimoto, Susan E. H., Herbert V. Frey, James B. Garvin, and James H. Roark. "Topography, roughness, layering, and slope properties of the Medusae Fossae Formation from Mars Orbiter Laser Altimeter (MOLA) and Mars Orbiter Camera (MOC) data." Journal of Geophysical Research: Planets 104, E10 (1999): 24141–54. http://dx.doi.org/10.1029/1999je001044.

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18

Landais, F., F. Schmidt, and S. Lovejoy. "Universal multifractal Martian topography." Nonlinear Processes in Geophysics 22, no. 6 (2015): 713–22. http://dx.doi.org/10.5194/npg-22-713-2015.

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Abstract. In the present study, we investigate the scaling properties of the topography of Mars. Planetary topographic fields are well known to roughly exhibit (mono)fractal behavior. Indeed, the fractal formalism reproduces much of the variability observed in topography. Still, a single fractal dimension is not enough to explain the huge variability and intermittency. Previous studies have claimed that fractal dimensions might be different from one region to another, excluding a general description at the planetary scale. In this article, we analyze the Martian topographic data with a multifractal formalism to study the scaling intermittency. In the multifractal paradigm, the apparent local variation of the fractal dimension is interpreted as a statistical property of multifractal fields. We analyze the topography measured with the Mars Orbiter Laser altimeter (MOLA) at 300 m horizontal resolution, 1 m vertical resolution. We adapted the Haar fluctuation method to the irregularly sampled signal. The results suggest a multifractal behavior from the planetary scale down to 10 km. From 10 to 300 m, the topography seems to be simple monofractal. This transition indicates a significant change in the geological processes governing the Red Planet's surface.
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19

Fishbaugh, Kathryn E., and James W. Head. "North polar region of Mars: Topography of circumpolar deposits from Mars Orbiter Laser Altimeter (MOLA) data and evidence for asymmetric retreat of the polar cap." Journal of Geophysical Research: Planets 105, E9 (2000): 22455–86. http://dx.doi.org/10.1029/1999je001230.

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20

Ivanov, M. A., and J. W. Head. "Chryse Planitia, Mars: Topographic configuration, outflow channel continuity and sequence, and tests for hypothesized ancient bodies of water using Mars Orbiter Laser Altimeter (MOLA) data." Journal of Geophysical Research: Planets 106, E2 (2001): 3275–95. http://dx.doi.org/10.1029/2000je001257.

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21

Landais, F., F. Schmidt, and S. Lovejoy. "Universal multifractal Martian topography." Nonlinear Processes in Geophysics Discussions 2, no. 4 (2015): 1007–31. http://dx.doi.org/10.5194/npgd-2-1007-2015.

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Abstract. In the present study, we investigate the scaling properties of the topography of Mars. Planetary topographic fields are well known to roughly exhibit (mono)fractal behavior. Indeed, the fractal formalism is reproduces much of the variability observed in topography. Still, a single fractal dimension is not enough to explain the huge variability and intermittency. Previous studies have claimed that fractal dimensions might be different from one region to an other, excluding a general description at the planetary scale. In this article, we are analyzing the Martian topographic data with a multifractal formalism to study the scaling intermittency. In the multifractal paradigm, the apparent local variation of the fractal dimension is interpreted as a statistical property of multifractal fields. We analyze the topography measured with the laser altimeter MOLA at 300 m horizontal resolution, 1 m vertical resolution. We adapted the Haar fluctuation method to the the irregularly sampled signal. The results suggest a multifractal behavior from planetary scale down to 10 km. From 10 km to 300 m, the topography seems to be simple monofractal. This transition indicates a significant change in the geological processes governing the Red Planet's surface.
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22

Tao, Yu, Siting Xiong, Susan J. Conway, et al. "Rapid Single Image-Based DTM Estimation from ExoMars TGO CaSSIS Images Using Generative Adversarial U-Nets." Remote Sensing 13, no. 15 (2021): 2877. http://dx.doi.org/10.3390/rs13152877.

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The lack of adequate stereo coverage and where available, lengthy processing time, various artefacts, and unsatisfactory quality and complexity of automating the selection of the best set of processing parameters, have long been big barriers for large-area planetary 3D mapping. In this paper, we propose a deep learning-based solution, called MADNet (Multi-scale generative Adversarial u-net with Dense convolutional and up-projection blocks), that avoids or resolves all of the above issues. We demonstrate the wide applicability of this technique with the ExoMars Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) 4.6 m/pixel images on Mars. Only a single input image and a coarse global 3D reference are required, without knowing any camera models or imaging parameters, to produce high-quality and high-resolution full-strip Digital Terrain Models (DTMs) in a few seconds. In this paper, we discuss technical details of the MADNet system and provide detailed comparisons and assessments of the results. The resultant MADNet 8 m/pixel CaSSIS DTMs are qualitatively very similar to the 1 m/pixel HiRISE DTMs. The resultant MADNet CaSSIS DTMs display excellent agreement with nested Mars Reconnaissance Orbiter Context Camera (CTX), Mars Express’s High-Resolution Stereo Camera (HRSC), and Mars Orbiter Laser Altimeter (MOLA) DTMs at large-scale, and meanwhile, show fairly good correlation with the High-Resolution Imaging Science Experiment (HiRISE) DTMs for fine-scale details. In addition, we show how MADNet outperforms traditional photogrammetric methods, both on speed and quality, for other datasets like HRSC, CTX, and HiRISE, without any parameter tuning or re-training of the model. We demonstrate the results for Oxia Planum (the landing site of the European Space Agency’s Rosalind Franklin ExoMars rover 2023) and a couple of sites of high scientific interest.
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23

Tao, Yu, Jan-Peter Muller, Susan J. Conway, and Siting Xiong. "Large Area High-Resolution 3D Mapping of Oxia Planum: The Landing Site for the ExoMars Rosalind Franklin Rover." Remote Sensing 13, no. 16 (2021): 3270. http://dx.doi.org/10.3390/rs13163270.

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We demonstrate an end-to-end application of the in-house deep learning-based surface modelling system, called MADNet, to produce three large area 3D mapping products from single images taken from the ESA Mars Express’s High Resolution Stereo Camera (HRSC), the NASA Mars Reconnaissance Orbiter’s Context Camera (CTX), and the High Resolution Imaging Science Experiment (HiRISE) imaging data over the ExoMars 2022 Rosalind Franklin rover’s landing site at Oxia Planum on Mars. MADNet takes a single orbital optical image as input, provides pixelwise height predictions, and uses a separate coarse Digital Terrain Model (DTM) as reference, to produce a DTM product from the given input image. Initially, we demonstrate the resultant 25 m/pixel HRSC DTM mosaic covering an area of 197 km × 182 km, providing fine-scale details to the 50 m/pixel HRSC MC-11 level-5 DTM mosaic. Secondly, we demonstrate the resultant 12 m/pixel CTX MADNet DTM mosaic covering a 114 km × 117 km area, showing much more detail in comparison to photogrammetric DTMs produced using the open source in-house developed CASP-GO system. Finally, we demonstrate the resultant 50 cm/pixel HiRISE MADNet DTM mosaic, produced for the first time, covering a 74.3 km × 86.3 km area of the 3-sigma landing ellipse and partially the ExoMars team’s geological characterisation area. The resultant MADNet HiRISE DTM mosaic shows fine-scale details superior to existing Planetary Data System (PDS) HiRISE DTMs and covers a larger area that is considered difficult for existing photogrammetry and photoclinometry pipelines to achieve, especially given the current limitations of stereo HiRISE coverage. All of the resultant DTM mosaics are co-aligned with each other, and ultimately with the Mars Global Surveyor’s Mars Orbiter Laser Altimeter (MOLA) DTM, providing high spatial and vertical congruence. In this paper, technical details are presented, issues that arose are discussed, along with a visual evaluation and quantitative assessments of the resultant DTM mosaic products.
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24

Kirk, R. L., E. Howington-Kraus, K. Edmundson, et al. "COMMUNITY TOOLS FOR CARTOGRAPHIC AND PHOTOGRAMMETRIC PROCESSING OF MARS EXPRESS HRSC IMAGES." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLII-3/W1 (July 25, 2017): 69–76. http://dx.doi.org/10.5194/isprs-archives-xlii-3-w1-69-2017.

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The High Resolution Stereo Camera (HRSC) on the Mars Express orbiter (Neukum et al. 2004) is a multi-line pushbroom scanner that can obtain stereo and color coverage of targets in a single overpass, with pixel scales as small as 10 m at periapsis. Since commencing operations in 2004 it has imaged ~ 77 % of Mars at 20 m/pixel or better. The instrument team uses the Video Image Communication And Retrieval (VICAR) software to produce and archive a range of data products from uncalibrated and radiometrically calibrated images to controlled digital topographic models (DTMs) and orthoimages and regional mosaics of DTM and orthophoto data (Gwinner et al. 2009; 2010b; 2016). Alternatives to this highly effective standard processing pipeline are nevertheless of interest to researchers who do not have access to the full VICAR suite and may wish to make topographic products or perform other (e. g., spectrophotometric) analyses prior to the release of the highest level products. We have therefore developed software to ingest HRSC images and model their geometry in the USGS Integrated Software for Imagers and Spectrometers (ISIS3), which can be used for data preparation, geodetic control, and analysis, and the commercial photogrammetric software SOCET SET (® BAE Systems; Miller and Walker 1993; 1995) which can be used for independent production of DTMs and orthoimages. <br><br> The initial implementation of this capability utilized the then-current ISIS2 system and the generic pushbroom sensor model of SOCET SET, and was described in the DTM comparison of independent photogrammetric processing by different elements of the HRSC team (Heipke et al. 2007). A major drawback of this prototype was that neither software system then allowed for pushbroom images in which the exposure time changes from line to line. Except at periapsis, HRSC makes such timing changes every few hundred lines to accommodate changes of altitude and velocity in its elliptical orbit. As a result, it was necessary to split observations into blocks of constant exposure time, greatly increasing the effort needed to control the images and collect DTMs. <br><br> Here, we describe a substantially improved HRSC processing capability that incorporates sensor models with varying line timing in the current ISIS3 system (Sides 2017) and SOCET SET. This enormously reduces the work effort for processing most images and eliminates the artifacts that arose from segmenting them. In addition, the software takes advantage of the continuously evolving capabilities of ISIS3 and the improved image matching module NGATE (Next Generation Automatic Terrain Extraction, incorporating area and feature based algorithms, multi-image and multi-direction matching) of SOCET SET, thus greatly reducing the need for manual editing of DTM errors. We have also developed a procedure for geodetically controlling the images to Mars Orbiter Laser Altimeter (MOLA) data by registering a preliminary stereo topographic model to MOLA by using the point cloud alignment (<i>pc_align</i>) function of the NASA Ames Stereo Pipeline (ASP; Moratto et al. 2010). This effectively converts inter-image tiepoints into ground control points in the MOLA coordinate system. The result is improved absolute accuracy and a significant reduction in work effort relative to manual measurement of ground control. <i>The ISIS and ASP software used are freely available; SOCET SET, is a commercial product.</i> By the end of 2017 we expect to have ported our SOCET SET HRSC sensor model to the Community Sensor Model (CSM; Community Sensor Model Working Group 2010; Hare and Kirk 2017) standard utilized by the successor photogrammetric system SOCET GXP that is currently offered by BAE. In early 2018, we are also working with BAE to release the CSM source code under a BSD or MIT open source license. <br><br> We illustrate current HRSC processing capabilities with three examples, of which the first two come from the DTM comparison of 2007. Candor Chasma (h1235_0001) was a near-periapse observation with constant exposure time that could be processed relatively easily at that time. We show qualitative and quantitative improvements in DTM resolution and precision as well as greatly reduced need for manual editing, and illustrate some of the photometric applications possible in ISIS. At the Nanedi Valles site we are now able to process all 3 long-arc orbits (h0894_0000, h0905_0000 and h0927_0000) without segmenting the images. Finally, processing image set h4235_0001, which covers the landing site of the Mars Science Laboratory (MSL) rover and its rugged science target of Aeolus Mons in Gale crater, provides a rare opportunity to evaluate DTM resolution and precision because extensive High Resolution Imaging Science Experiment (HiRISE) DTMs are available (Golombek et al. 2012). The HiRISE products have ~ 50x smaller pixel scale so that discrepancies can mostly be attributed to HRSC. We use the HiRISE DTMs to compare the resolution and precision of our HRSC DTMs with the (evolving) standard products. <br><br> We find that the vertical precision of HRSC DTMs is comparable to the pixel scale but the horizontal resolution may be 15–30 image pixels, depending on processing. This is significantly coarser than the lower limit of 3–5 pixels based on the minimum size for image patches to be matched. Stereo DTMs registered to MOLA altimetry by surface fitting typically deviate by 10thinsp;m or less in mean elevation. Estimates of the RMS deviation are strongly influenced by the sparse sampling of the altimetry, but range from <thinsp;50thinsp;m in flat areas to ~ 100thinsp;m in rugged areas.
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25

Heavens, N. G., M. I. Richardson, and A. D. Toigo. "Two aerodynamic roughness maps derived from Mars Orbiter Laser Altimeter (MOLA) data and their effects on boundary layer properties in a Mars general circulation model (GCM)." Journal of Geophysical Research 113, E2 (2008). http://dx.doi.org/10.1029/2007je002991.

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26

Heldmann, Jennifer L., Ella Carlsson, Henrik Johansson, Owen B. Toon, and Michael T. Mellon. "Observations of martian gullies and constraints on potential formation mechanisms." January 1, 2007. https://doi.org/10.1016/j.icarus.2003.11.024.

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The formation process(es) responsible for creating the observed geologically recent gully features on Mars has remained the subject of intense debate since their discovery. We present new data and analysis of northern hemisphere gullies from Mars Global Surveyor data which is used to test the various proposed mechanisms of gully formation. We located 137 Mars Orbiter Camera (MOC) images in the northern hemisphere that contain clear evidence of gully landforms and analyzed these images in combination with Mars Orbiter Laser Altimeter (MOLA) and Thermal Emission Spectrometer (TES) data to provide quantitative measurements of numerous gully characteristics. Parameters we measured include apparent source depth and distribution, vertical and horizontal dimensions, slopes, orientations, and present-day characteristics that affect local ground temperatures. Northern hemisphere gullies are clustered in Arcadia Planitia, Tempe Terra, Acidalia Planitia, and Utopia Planitia. These gullies form in craters (84%), knobby terrain (4%), valleys (3%), other/unknown terrains (9%) and are found on all slope orientations although the majority of gullies are equator-facing. Most gullies (63%) are associated with competent rock strata, 26% are not associated with strata, and 11% are ambiguous. Assuming thermal conductivities derived from TES measurements as well as modeled surface temperatures, we find that 95% of the gully alcove bases with adequate data coverage lie at depths where subsurface temperatures are greater than 273 K and 5% of the alcove bases lie within the solid water regime. The average alcove length is 470 m and the average channel length is 690 m. Based on a comparison of measured gully features with predictions from the various models of gully formation, we find that models involving carbon dioxide, melting ground ice in the upper few meters of the soil, dry landslide, and surface snowmelt are the least likely to describe the formation of the martian gullies. Although some discrepancies still exist between prediction and observation, the shallow and deep aquifer models remain as the most plausible theories. Interior processes involving subsurface fluid sources are generally favored over exogenic processes such as wind and snowfall for explaining the origin of the martian gullies. These findings gleaned from the northern hemisphere data are in general agreement with analyses of gullies in the southern hemisphere [Heldmann, J.L., Mellon, M.T., 2004. Icarus 168, 285-304]. ; The formation process(es) responsible for creating the observed geologically recent gully features on Mars has remained the subject of intense debate since their discovery. We present new data and analysis of northern hemisphere gullies from Mars Global Surveyor data which is used to test the various proposed mechanisms of gully formation. We located 137 Mars Orbiter Camera (MOC) images in the northern hemisphere that contain clear evidence of gully landforms and analyzed these images in combination with Mars Orbiter Laser Altimeter (MOLA) and Thermal Emission Spectrometer (TES) data to provide quantitative measurements of numerous gully characteristics. Parameters we measured include apparent source depth and distribution, vertical and horizontal dimensions, slopes, orientations, and present-day characteristics that affect local ground temperatures. Northern hemisphere gullies are clustered in Arcadia Planitia, Tempe Terra, Acidalia Planitia, and Utopia Planitia. These gullies form in craters (84%), knobby terrain (4%), valleys (3%), other/unknown terrains (9%) and are found on all slope orientations although the majority of gullies are equator-facing. Most gullies (63%) are associated with competent rock strata, 26% are not associated with strata, and 11% are ambiguous. Assuming thermal conductivities derived from TES measurements as well as modeled surface temperatures, we find that 95% of the gully alcove bases with adequate data coverage lie at depths where subsurface temperatures are greater than 273 K and 5% of the alcove bases lie within the solid water regime. The average alcove length is 470 m and the average channel length is 690 m. Based on a comparison of measured gully features with predictions from the various models of gully formation, we find that models involving carbon dioxide, melting ground ice in the upper few meters of the soil, dry landslide, and surface snowmelt are the least likely to describe the formation of the martian gullies. Although some discrepancies still exist between prediction and observation, the shallow and deep aquifer models remain as the most plausible theories. Interior processes involving subsurface fluid sources are generally favored over exogenic processes such as wind and snowfall for explaining the origin of the martian gullies. These findings gleaned from the northern hemisphere data are in general agreement with analyses of gullies in the southern hemisphere [Heldmann, J.L., Mellon, M.T., 2004. Icarus 168, 285-304].
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Hiesinger, H., J. W. Head, and G. Neukum. "Young lava flows on the eastern flank of Ascraeus Mons: Rheological properties derived from High Resolution Stereo Camera (HRSC) images and Mars Orbiter Laser Altimeter (MOLA) data." Journal of Geophysical Research 112, E5 (2007). http://dx.doi.org/10.1029/2006je002717.

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