Peter Fawdon

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ExoFiT: ExoMars-Like Field Trials – a Mission Simulation

HAL is a multi-disciplinary open access archive for the deposit and dissemination of scientific r... more HAL is a multi-disciplinary open access archive for the deposit and dissemination of scientific research documents, whether they are published or not. The documents may come from teaching and research institutions in France or abroad, or from public or private research centers. L’archive ouverte pluridisciplinaire HAL, est destinée au dépôt et à la diffusion de documents scientifiques de niveau recherche, publiés ou non, émanant des établissements d’enseignement et de recherche français ou étrangers, des laboratoires publics ou privés. ExoFiT: ExoMars-Like Field Trials – a Mission Simulation A. Hall, B. Dobke, M. Lisle, M. Shilton, E. Allouis, L. Waugh, J. Carroll, G. Doignon, M. Azkarate, M. Van Winnendael, et al.

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Mounds in Oxia Planum: The Burial and Exhumation of the ExoMars Rover Landing Site

Journal of Geophysical Research: Planets

Analyses of dendritic ridges within Antoniadi crater, Mars, from CaSSIS and HiRISE data

&lt;p&gt;&lt;strong&gt;Introduction&lt;/strong&gt;&lt;/p&gt; &amp... more &lt;p&gt;&lt;strong&gt;Introduction&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;Antoniadi basin is a 330 km diameter Noachian basin localized in the eastern Arabia Terra that contains a network of dendritic ridges. Branched, dendritic ridges, such as these can form by a variety of processes including the inversion of fluvial deposits, thus potentially highlighting aqueous processes of interest for understanding Mars&amp;#8217; climate evolution. Here, we test this hypothesis by analyzing in details data from Colour and Stereo Surface Imaging System (CaSSIS), High Resolution Imaging Science Experiment (HiRISE) and High Resolution Stereo Camera (HRSC).&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Age of landforms&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;Antoniadi&amp;#8217;s interior plains are filled by deposits interpreted to be Hesperian or younger and volcanic in origin, possibly coeval with the volcanic episodes of the nearby Syrtis Major Planum [1]. The dendritic ridges lie on these volcanic plains to the south of a 28 km-diameter well-preserved crater (Fig. 1). Although this crater predates the branched ridges it is devoid of any fluvial erosion and appears mostly similar to many fresh, Amazonian age craters. While some erosion has affected the ridges, there is no indication of exhumation of these ridges from putative layers above the current plains surface. The crater size frequency distribution of the volcanic plains gives a model age of 2.5&amp;#177;0.5 Gy, using diameters of 200 m to 2 km. Thus, the branched ridges are Early Amazonian or younger.&lt;/p&gt; &lt;p&gt;&lt;img src="" alt="" width="600" height="594" /&gt;&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Figure. 1: &lt;/strong&gt;Four Cassis images projected on CTX mosaic. The fresh crater to the north has been covered by fresh lava flows which themselves have been covered by the dendritic features.&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Morphometry and topography&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;Individual ridges are easily recognizable with their dark tone in visible images compared to surrounding plains (Fig. 2), which display a slightly lighter tone. The ridges are organized as a dendritic network reaching a Strahler order of 4, i.e. the degree of hierarchy from the primary branches counting the number of junctions. Assuming tributary flows, this organization indicates a northward flow direction. However, the local slope is of 0.2&amp;#176; toward South, and thus contrary to the apparent network organization (assuming tributary flows). The branched ridges are also present on some of the lowest areas of these plains, but there is no evidence of terminal fans nor of erosional features affecting the plains in their more elevated areas.&lt;/p&gt; &lt;p&gt;The texture of ridges at HiRISE scale (25cm/pixel) is rubbly with the occurrence of blocks up to ~1 m in size and a complete lack of layering in all HiRISE images where they are present unlike sedimentary strata usually observed within inverted channels on Mars. A HiRISE elevation model shows that branched ridges are between 1-5 m high, although erosion can explain some variations in height among the ridges. Ridges are up to 10 km long and 10-200 m wide without any obvious trends in width, i.e. ridges are not wider with increasing Strahler order. The order 1 branches are also peculiar in plan-view shape. They frequently display lobate shapes and are up to 100 m wide, which is wider than the ridge measured after the junction with several order 1 branches. North of the main pattern, a 500 m wide sinuous ridge present in the middle of the plain displays the same internal texture (rubbly) suggesting that it formed by the same process (white arrow at the top of Fig. 1).&lt;/p&gt; &lt;p&gt;&lt;strong&gt;&amp;#160;&lt;/strong&gt;&lt;img src="" alt="" /&gt;&lt;/p&gt; &lt;p&gt;&lt;strong&gt; &lt;/strong&gt;&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Figure 2:&lt;/strong&gt; Close-up on the dendritic network with CaSSIS images.&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Conclusion&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;Previous assessments of these landforms favored an origin as inverted channels [2]. Yet, our observations show many inconsistencies with this interpretation: (i) The rubbly texture lacks any layering at meter scale, a typical feature of inverted channels observed elsewhere on Mars [e.g., 3, 4]. (ii) The order 1 branches display a lobate shape and a larger width than higher order branches unlike river flows as observed on Earth. (iii) There is no increase in width from degree 1 branches of the network towards the north as would be expected for channels with increasing discharge rates downstream. (iv) The slope towards the south is contrary to the inferred flow direction to the north assuming a tributary network. Wrinkle ridges may be evidence for post-depositional changes in topography, but these uplifts appear localized (Fig. 1). Thus, the detailed analysis of these branched ridges shows characteristics difficult to reconcile with inverted fluvial…

Evaluation of style, settings and timing of martian fluvial deposition troughs inverted channel studies

&lt;p&gt;&lt;strong&gt;Introduction: &lt;/strong&gt;Inverted channels are... more &lt;p&gt;&lt;strong&gt;Introduction: &lt;/strong&gt;Inverted channels are sinuous ridges comprising fluvial facies, which have gained a positive relief due to differential erosion [e.g., 1, 2]. Many have been found preserved on Mars in terrains dated between the Mid-Noachian to Early Hesperian in the region of Arabia Terra [1, 3, 4]. The distribution of these features is well known [e.g., 2, 3] but timing, geological settings, their relative timescales of liquid water stability and the nature of the early climate under which fluvial deposition was possible are still under debate. We present results from studies conducted on three morphologically different inverted channel systems in the region of Arabia Terra: Arago Dorsa (within the Arago crater), Cantabras Dorsum and Piscinas Serpentes (in Meridiani Planum). The analysis includes interpretations of the formation settings of the three systems and estimation of the volume of preserved alluvial materials and the consequent required period of fluvial activity for such deposition.&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Methodology:&amp;#160;&lt;/strong&gt; Digital morphostratigraphic maps (scale 1:10,000) were constructed using ArcGIS software using 25 cm/pixel HiRISE images [5]. A CTX mosaic [6] was used to study the general context of the study area, and to assist the analysis of stratigraphy. HiRISE DEMs [7] were used to calculate thicknesses of units interpreted as fluvial facies and to characterise and interpret the stratigraphic relationships of the different geological units. When HiRISE DEMS were not available, the HRSC-MOLA DEM [8] was used. The ridges&amp;#8217; morphometric parameters (length, thickness, width) were used to estimate both the preserved volume of alluvial material and the duration of fluvial activity of the systems, assuming sedimentation rates of 0.01-0.7 m/Kyr from terrestrial comparisons [4, 9].&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Inverted channel types and settings: &lt;/strong&gt;The &lt;strong&gt;&lt;em&gt;Arago Dorsa&lt;/em&gt;&lt;/strong&gt; ridges are the result of channel belt aggradation [10], as shown by the presence of a well-organized multi-level structure made of candidate channel fills and overbank deposits. We interpret the overall structure as a candidate relict aggrading fluvial fan preserved within a continental highland basin in a distal portion from the source where inverted channel belts are usually formed [11]. &lt;strong&gt;&lt;em&gt;Cantabras Dorsum &lt;/em&gt;&lt;/strong&gt;represents a complex package of fluvial sediments, and presents two distinct ridges. The smaller, a sinuous flat-topped ridge with a rectangular cross-section [following 2], is developed on top of a wider one (Fig. 1). We interpret the structure as alluvial deposits deposited by an avulsed channel on the floor of a wider valley which progressively reduced the cross-sectional area, terminating in a smaller channel now expressed by the upper inverted ridge. &lt;strong&gt;&lt;em&gt;Piscinas Serpentes &lt;/em&gt;&lt;/strong&gt;presents a network of fine-scale valleys that transition downstream (north of the studied site) into pitted channels and finally ridges (Fig. 2). The ridges of Piscinas Serpentes, are more likely the result of channel fill in a ribbon-like channel.&lt;/p&gt; &lt;p&gt;&amp;#160;&lt;/p&gt; &lt;p&gt;&lt;img src="" alt="" /&gt;&lt;/p&gt; &lt;p&gt;&lt;em&gt;Figure 1: HiRISE-DEM oblique view of Cantabras Dorsum. Vertical exaggeration = 5 times. a- Main ridge (9.13&amp;#176;N, -5.47&amp;#176;E). b- Lateral oblique view of the upper ridge (9.13&amp;#176;N, -5.48&amp;#176;E).&lt;/em&gt;&lt;/p&gt; &lt;p&gt;&lt;em&gt;&lt;img src="" alt="" /&gt;&lt;/em&gt;&lt;/p&gt; &lt;p&gt;&lt;em&gt;Figure 2: Detail of Piscinas Serpentes system (ESP_048489_1845; 4.51&amp;#176;N, -1.17&amp;#176;E), where the passage from positive inverted relief in the northern part of the image to negative relief in the south is visible.&lt;/em&gt;&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Estimation of volume and timing for fluvial deposition: &lt;/strong&gt;The estimated vertical thickness of the ridges and the estimated duration of fluvial activity (Table 1) are in line with those measured for terrestrial analogues [12]. Aggrading systems like Arago Dorsa and Cantabras Dorsum should have been stable for between 10&lt;sup&gt;4&lt;/sup&gt;-10&lt;sup&gt;6&lt;/sup&gt; years.&lt;/p&gt; &lt;p&gt;&lt;em&gt;Table 1: Morphometric data of the studied systems and estimation of volume and formation timescale of fluvial activity.&lt;/em&gt;&lt;/p&gt; &lt;div&gt; &lt;table&gt; &lt;tbody&gt; &lt;tr&gt; &lt;td&gt; &lt;p&gt;&lt;strong&gt;System&lt;/strong&gt;&lt;/p&gt; &lt;/td&gt; &lt;td&gt; &lt;p&gt;&lt;strong&gt;Vertical Thickness (m)&lt;/strong&gt;&lt;/p&gt; &lt;/td&gt; &lt;td&gt; &lt;p&gt;&lt;strong&gt;Exposed Length (m)&lt;/strong&gt;&lt;/p&gt; &lt;/td&gt; &lt;td&gt; &lt;p&gt;&lt;strong&gt;Width (m)&lt;/strong&gt;&lt;/p&gt; &lt;/td&gt; &lt;td&gt; &lt;p&gt;&lt;strong&gt;Volume of alluvial…

Jezero crater, Mars: application of the deep learning NOAH-H terrain classification system

Journal of Maps

Oxia Planum, Mars, classified using the NOAH-H deep-learning terrain classification system

Journal of Maps

Ancient Alluvial Plains at Oxia Planum, Mars

&lt;p&gt;The geologic origin of the ancient, phyllosilicate-rich bedrock at Oxia Planum, ... more &lt;p&gt;The geologic origin of the ancient, phyllosilicate-rich bedrock at Oxia Planum, Mars, the landing site of ESA&amp;#8217;s ExoMars rover, is unknown. The phyllosilicates record ancient aqueous processes, but the processes that formed the host bedrock remain elusive. Here, we use high-resolution orbital image and topographic datasets (HiRISE, CTX, CaSSIS) to investigate and characterize fluvial sinuous ridges (FSRs), found across the Oxia Planum region. The FSRs form segments up to 70 km long, with sub-horizontal layering commonly exposed in ridge margins. Some FSRs comprise multi-story ridge systems; many are embedded within and are being exhumed from the phyllosilicate-rich bedrock. We interpret the FSRs as deposits of ancient, episodically active, alluvial river systems (channel-belt and overbank deposits) at Oxia Planum. Thus, the phyllosilicate-rich bedrock was formed at least partly by ancient alluvial rivers, active across the wider region. Our alluvial hypothesis does not exclude other sources of sediment playing a role in building the terrain as well. Future exploration by ExoMars can verify this interpretation and provides an opportunity to investigate some of the oldest river deposits in the Solar System.&lt;/p&gt;

NOAH-H_terrain_classifications_of_Jezero_Crater_Mars.zip

Zip folder containing data pertaining to the manuscript "Deep learning-generated map of Jeze... more Zip folder containing data pertaining to the manuscript "Deep learning-generated map of Jezero Crater, Mars: Application of the NOAH-H terrain classification system" submitted to Journal of Maps. Zip folder contains georeferenced NOAH-H terrain classified rasters, control point files used to georeference the NOAH-H rasters, the final NOAH-H terrain mosaics, and a readme file explaining the contents of the zip folder. This work was funded in part by the European Space Agency contract 4000118843/16/ NL/LvH1145 – Novelty or Anomaly Hunter (NOAH).

Well-Preserved Ice-Rich Deposits on Mars, in the Southern Midlatitude Region of Terra Cimmeria

Lunar and Planetary Science Conference, Mar 1, 2017

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Surface-Based 3D Measurements of Aeolian Bedforms on Mars and Their Application to Estimating ExoMars Rover Surface Hazard

Lunar and Planetary Science Conference, Mar 1, 2017

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Field study of exhumed channels in Green River and Hanksville areas, Utah, and a comparison with inverted channel features on Mars

EGU General Assembly Conference Abstracts, Apr 1, 2018

Geologic Stratigraphy, Delta Morphology, and Regional History of Hypanis Delta, Mars

AGU Fall Meeting Abstracts, Dec 1, 2016

The Ancient Fluvial Catchment of the Candidate ExoMars 2020 Rover Landing Site in the Oxia Planum Basin

European Planetary Science Congress, Sep 1, 2018

The Geography of Oxia Planum 03 CTX DEM Mosaic

This data is a mosaic of CTX DEM and ORI's covering the ExoMars rover landing site in Oxia Pl... more This data is a mosaic of CTX DEM and ORI's covering the ExoMars rover landing site in Oxia Planum. This data is a basemap for Oxia Planum and will act as a georeferencing base layer for future High resolution datasets of the rover landing site. Contents This data set contains 4 directories: 03_a Sets of elevation contours at 100 m and 25 m spacing made from the DEM and smoothed for use in map publications. 03_b Mosaic of orthorectified CTX images that accompany the DEM. These data are provided in an equirectangular projection centered at 335.45°E 03_c Hillshade model of the CTX DEM mosaic. These data are provided to help assess the variability and quality of the DEM. These data are provided in an equirectangular projection centered at 335.45°E 03_d CTX DEM mosaic. These data are provided in an equirectangular projection centered at 335.45°E G...

Chryse Planitia, Mars: Mound Morphometry and Morphology Datasets

.xlsx and .shp files containing information pertaining to the morphometry and morphology of >1... more

Aram Dorsum Morphostratigraphic map shapefiles

This dataset contains GIS shapefiles from a project to map the Aram Dorsum region of Mars. The ar... more This dataset contains GIS shapefiles from a project to map the Aram Dorsum region of Mars. The area was a candidate ExoMars Rover landing site.The dataset is a morphostratigraphic map, made using remote sensing data (6 m/pixel greyscale image basemap).The zip file contains: 1) Unit_polygons.shp: the morphostratigraphic units as polygon shapefiles (plus a Units_Aram.lyr layer file to use if you want to maintain the same approximate symbology we did)2) Unit_oultines.shp: simple outlines of these polygons. We did not specify contact types in this mapping exercise but these could be useful if you wish to specify contact types yourself.3) Structure_etc.shp: which contains minor features such as smaller channels and ridges, crate rims, etc, that are too small to represented as polygons, or would be inappropriate to be represented a polygons.

UK Space Agency Mars Utah Rover Field Investigation 2016 (MURFI): In-Situ and Remote Operations

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The Hypanis fluvial deltaic system in Xanthe Terra: a candidate ExoMars 2018 Rover landing site

The search for life on Mars is a cornerstone of international solar system exploration. In 2018, ... more The search for life on Mars is a cornerstone of international solar system exploration. In 2018, the European Space agency will launch the ExoMars Rover to further this goal. The key science objectives of the ExoMars Rover are to: 1) search for signs of past and present life on Mars; 2) investigate the water/geochemical environment as a function of depth in the shallow subsurface; and 3) to characterize the surface environment. ExoMars will drill into the sub-surface to look for indicators of past life using a variety of complementary techniques, including assessment of morphology (potential fossil organisms), mineralogy (past environments) and a search for organic molecules and their chirality (biomarkers). The choice of landing site is vital if the objectives are to be met. The landing site must: (i) be ancient (≥3.6 Ga); (ii) show abundant morphological and mineral evidence for long-term, or frequently reoccurring, aqueous activity; (iii) include numerous sedimentary outcrops tha...

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Tectonic Features in Western Arabia Terra and Their Implications for the Exomars 2022 Rover Landing Site

Introduction: Oxia Planum, the landing site of the ExoMars Rosalind Franklin rover [1], is locate... more Introduction: Oxia Planum, the landing site of the ExoMars Rosalind Franklin rover [1], is located in transitional terrain between the Arabia Terra highlands and the Chryse Planitia lowlands (Fig 1). Recent work shows that Arabia Terra hosted extensive river systems during the Noachian period (> 3.7 billion years ago) [2, 3]. In our study area in west Arabia Terra (Fig 1b), the fluvial landscape has been exhumed from beneath younger sedimentary terrains [e.g. 4] while also being modified by tectonism. The impact of tectonism, on both regional and global scales, on the geological history of west Arabia Terra is poorly understood; it could have implications for palaeohydrology and the elevation of proposed shoreline features. To provide constraints on the tectonic evolution of the region, we have constructed a preliminary map of tectonic features in west Arabia Terra (Fig 1) and analyzed their orientations.

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Mineralogy of the Oxia Planum catchment area on Mars

Hyperspectral Imaging and Applications, 2020

Mineralogy of the Oxia Planum Catchment Area on Mars and its Relevance to the Exomars Rosalind Fr... more Mineralogy of the Oxia Planum Catchment Area on Mars and its Relevance to the Exomars Rosalind Franklin Rover Mission Conference or Workshop Item How to cite: Turner, Stuart; Fawdon, Peter and Davis, J.M. (2021). Mineralogy of the Oxia Planum Catchment Area on Mars and its Relevance to the Exomars Rosalind Franklin Rover Mission. In: 52nd Lunar and Planetary Science Conference 2021, 15-19 Mar 2021, Virtual.

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ExoFiT: ExoMars-Like Field Trials – a Mission Simulation

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Mounds in Oxia Planum: The Burial and Exhumation of the ExoMars Rover Landing Site

Journal of Geophysical Research: Planets