Salt diapirs and their caprocks are strategically significant for natural resource exploration and as potential sites for nuclear waste and CO₂ storage. However, direct study of these systems is challenging because most diapirs are not exposed at the Earth’s surface. The Zagros Mountains in Iran, with their numerous exposed salt diapirs and caprocks, provide a rare and valuable opportunity to investigate the dynamics of active diapir-caprock systems.

In this study, we combine traditional fieldwork, space-based geodetic mapping, remote spectral analysis, and petrology to analyze the active processes and driving forces that shape salt diapir surfaces within the interconnected climate-diapir-caprock system.

The quantification of surface deformation of salt diapirs and their composition is challenging to map in field campaigns due to their rough terrain and remote location in the Zagros Mountains, southern Iran. To better understand patterns of the salt diapir’s surface deformation and composition active and passive remote sensing techniques are essential. However, the contemporary vertical surface deformation pattern is difficult to detect and interpret along disciplinary boundaries. With the aid of high-resolution PSI measurements and multispectral imagery analysis we detected high-precision spatiotemporal deformation patterns of the surfaces of several salt diapirs. In addition, time-series analysis helped to distinguish between salt-supply-driven domal uplift and vertical surface modification induced by precipitation, dissolution, and erosion.

We analysed Sentinel-1 PSI time-series, processed by the German Aerospace Center (DLR), to obtain the highest available spatiotemporal resolution of the vertical surface-deformation pattern across three diapirs – Karmostaj, Siah Taq, and Champeh – in the Zagros Mountains. We then correlated the Persistent Scatterers to the respective diapir’s composition based on multispectral analysis of Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) satellite images. Preliminary results indicate that the deformation pattern of the salt diapirs does not correlate with seasonal effects, such as precipitation and heat. The vertical surface deformation pattern on these three diapirs implies that these diapirs are active. We conclude that the strategic integration of space-based geodesy and remote spectral analysis provides an effective method for interpreting the complex surface deformation patterns of salt diapirs. The activity of salt diapirs should be considered a key factor in resource exploration, as well as in the evaluation of sites for nuclear waste and CO₂ storage.

How to cite: Rieger, S. M., Dusingizimana, M., Závada, P., Plattner, C., Brcic, R., Kahle, B., and Friedrich, A. M.: Using active and passive remote sensing techniques to quantify the surface deformation and lithology of salt diapirs, Zagros Mountains, southern Iran, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-4007, https://doi.org/10.5194/egusphere-egu25-4007, 2025.

Technological development allows new information to be derived from existing data. This saves financial resources while developing and detailing geological products such as maps. Using the data obtained for the geological map of the seabed and applying a new approach to data classification and visualisation, an information layer was created that represents a new approach to geomorphological mapping of the seabed of Poland (Southern Baltic Sea).

Data from extensive studies carried out by the Polish Geological Institute - NRI were used to produce this layer. The bathymetric background was obtained from the European Marine Observation and Data Network (EMODnet) project. Vocabularies and manuals developed by the EMODnet project team were also used to classify and visualise the data.

In the first phase of the work, bathymetric information was used. This was used to create a morphometric model using the Benthic Terrain Modeler (BTM) 3.0 for ArcGIS tool to determine the shapes present on the seafloor. The next step was to combine the resulting morphometric model with geological and genetic information from geological studies. The third step was to classify the extracted bathymetric-geological forms according to the EMODnet vocabularies and manuals. The fourth step was to generalise and unify the data for dissemination through a dedicated EMODnet Map Viewer.

How to cite: Pączek, U., Kaulbarsz, D., and Szarafin, T.: A New Perspective on Marine Geomorphological Mapping through Advanced Data Visualization in the southern Baltic Sea area (preliminary results), EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-5534, https://doi.org/10.5194/egusphere-egu25-5534, 2025.

The European Marine Observation and Data Network (EMODnet) is a long-term initiative funded by the European Commission to assemble and make accessible high-quality marine data from diverse sources across Europe. Since its beginning (2009), EMODnet has aimed to support sustainable marine and coastal management by providing open-access FAIR data and data products that are needed by scientific research, policymaking, and industry applications. Today, this network of more than 120 organizations covers several broad disciplinary themes: bathymetry, biology, chemistry, geology, human activities, physics, and seabed habitats. Each of these themes contributes to a comprehensive understanding of Europe’s marine environment and provides a wide range EMODnet datasets available through the EMODnet Central Portal (https://emodnet.ec.europa.eu/en).

EMODnet Geology, one of the thematics, focuses on the collection and harmonisation of marine geological data. This thematic provides extensive datasets on seabed substrate, sedimentation rates and seabed erosion index database, sea floor geology including lithology and stratigraphy, Quaternary geology and geomorphology, coastal behaviour, geological events such as submarine landslides and earthquakes, marine mineral resources, as well as submerged landscapes of the European continental shelf at various time frames. It is providing the full areal coverage of European seas as well as expanding to new areas, as also the Caspian and the Caribbean Seas are included in the geographical scope of the current project phase. EMODnet Geology focuses on delivering harmonised interpreted data layers (i.e., maps) rather than the underlying data. However, the metadata provides information on the data holder in case user needs to access the raw data. By integrating data layers from national geological surveys, research institutions, and marine organizations, EMODnet Geology ensures the availability of accurate and standardized geological information to support maritime spatial planning, environmental impact assessments, and resource management.

The current EMODnet Geology project phase (2023-2025) aims to further enhance data coverage and quality. It is coordinated by the Geological Survey of Finland (GTK), and it is executed by a consortium of 40 partners and subcontractors. The core of the partnership is formed by members of the EuroGeoSurveys network, supported by other partner organizations with valuable expertise and data.

EMODnet Geology also supports third-party data submission. Third party data can be submitted either straight to EMODnet Geology or through EMODnet Data Ingestion (www.emodnet-ingestion.eu), which is reaching out to potential data providers from private bodies and public. By facilitating data sharing and collaboration, EMODnet Geology continues to support informed decision-making and sustainable management of marine environments. It is a dynamic initiative where existing datasets are continuously updated with new data.

The EMODnet Geology project is funded by The European Climate, Environment and Infrastructure Executive Agency (CINEA) through contract EASME/EMFF/2020/3.1.11 - Lot 2/SI2.853812_EMODnet – Geology.

How to cite: Kaskela, A., Vallius, H., Kihlman, S., and Kotilainen, A. T. and the EMODnet Geology project consortium: EMODnet Geology - Supporting sustainable use of the European maritime areas and their resources , EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-17425, https://doi.org/10.5194/egusphere-egu25-17425, 2025.

Salt-diapir-caprock systems form both subsurface and surface halokinetic features. The world’s best exposed salt-diapir-caprock systems are hosted in the Zagros Mountains, in the arid and mountainous part of Iran. Due to their economic significance, subsurface salt-diapir-caprock systems in various tectonic settings have long been the focus of geosciences research. Biogeochemical subsurface processes, which are thought to be responsible for caprock formation, are also genetically linked to the formation of Pb-Zn deposits and some of the largest native sulfur deposits. In addition, the subsurface systems form hydrocarbon traps that are important for energy exploration. For this reason, extensive studies have been conducted on subsurface caprocks to establish a conceptual lithological model that describes the formation processes and the spatiotemporal relationships of salt-diapir-caprock facies. On the contrary, studies on fully extruded caprock systems remain limited. This scarcity hampers the comparative assessment of the lithological makeup of both extruded and subsurface salt-diapir caprock systems. It also restricts our understanding of the compositional evolution of salt-diapir and caprock materials as they diapirically extrude and become exposed to further modification by subaerial surface processes.

In this study, we explored the potential of satellite-based multispectral ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer) and hyperspectral EnMAP (Environmental Mapping and Analysis Program) remote sensing for producing lithological maps of exposed salt-diapir-caprock features in the Zagros Region. We tested our method on three geomorphologically different salt diapirs ― Karmostaj, Siah Taq, and Champeh. We further examined the similarities and differences between our results and the established lithological model of subsurface salt-diapir-caprock systems.

Our results indicate that satellite-based remote sensing offers an efficient approach to producing lithological maps of exposed salt deposits and related caprocks, hence allowing the identification of caprock lithological facies. However, the accuracy of these maps depends on the spectral and spatial resolutions of satellite data. Furthermore, the results allow us to define the fundamental compositional differences between caprock formed under subsurface biogeochemical environments and caprock formed under the influence of surface processes. Specifically, subsurface salt dissolution results in the accumulation of a substantial anhydrite cap. Microbially-driven subsurface caprock-forming processes alter Ca-sulfates into an extensive calcite cap and simultaneously cause iron sulfide mineralization. As diapiring microbial iron sulfides reach shallow-depths and subaerial conditions, they alter into ferric oxides and ferric oxy-hydroxides. Therefore, together with microbial carbonate, the ferric oxides and oxy-hydroxides serve as diagnostic proxies for subsurface caprocks. In contrast, under surface conditions, microbial processes are likely to be unfavorable, leading to the limited amount or lack of biogenic calcite caprocks and iron sulfide mineralization. Caprocks formed under surface conditions thus predominantly comprise quartz- and clay-rich lithologies, which are the main residuals of the dissolution of salt-rich extruded materials, and a limited amount of the Ca-sulfates as surface processes hamper their accumulation.

How to cite: Dusingizimana, M. W., Friedrich, A., Kahle, B., Rieger, S., Heuss-Aßbichler, S., Závada, P., and Zebari, M.: Lithological Characterization of Extruded Salt-Diapir-Caprock Systems in the Zagros Mountains in Iran Using Satellite-Based Multispectral and Hyperspectral Remote Sensing , EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-17849, https://doi.org/10.5194/egusphere-egu25-17849, 2025.

Harmonisation of marine geological data across the EEZ , both semantically and geometrically, is key to understand geological information across national borders. There is a multitude of EEZ boundaries in the European Seas which are partly intense and partly hardly mapped. This presents a considerable challenge.

The European EMODnet geology project is running since the year 2009. One of the aims is to provide geological data of the European Seas, harmonized as far as possible and available according to FAIR data principles.

Within the workpackage seafloor geology several international teams are working on semantic and geometric data harmonisation in seven marine areas, the so-called prototype areas. One of them focusses on the Western Baltic Sea with participants from Poland, Sweden, Denmark and Germany. The data  being compiled and harmonized centrally at BGR, Germany. The heterogenity of the geological information from each of the partners derive from the following reasons: data exist in some regions in patches or ribbons, e.g. along research vessels‘ tracks, the mapping results and classifications of terms differ due to different scientific approaches, the mapping took place in different scales and at differing ages. Thus, it was crucial to set up common standards, especially controlled vocabularies based on international standards (INSPIRE Directive, IUGS) as a base and to also practically discuss and agree on the continuation of geological structures across EEZ boundaries.

The poster demonstrates differing national classifications approaches, outlines the method of agreeing on the continuation and naming of geological structures and presents the first results of a geological map of the Quaternary of the Western Baltic Sea.

How to cite: Müller, A., Asch, K., Pączek, U., and Kaulbarsz, D.: EMODnet geology and data harmonisation: Seafloor mapping of the Western Baltic Sea , EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-20030, https://doi.org/10.5194/egusphere-egu25-20030, 2025.

Harmonisation of geological data, both semantically and geometrically, is key to foster the understanding of geological information across national borders. Hereby, the multitude of national borders in Europe, coupled with the intensity of geological mapping efforts, present a considerable challenge.

The building of geological databases for Europe started in 1995 with the project of the International Geological Map of Europe and Adjacent Areas (IGME 5000). For the first time a spatial geological database for the entire Europe was built which covered Europe’s on-shore and off-shore regions. The project was finished in 2005, and the map database is available online since 2006. In 2007, the European INSPIRE Directive came into force requiring standardized data availability within a pan-European geodata infrastructure of 34 themes, including geology, according to common standards and data specifications/vocabularies. The INSPIRE geology data specifications/vocabulary were based on those developed by the OneGeology-Europe project (OneG-E ) which had the aim to make European geological data interoperable, harmonize them as far as possible and make them available for free according to the FAIR data principles. One of the vocabularies described the lithology of rock units.

While these past projects were comprehensive, they showed a lack of
a) vocabularies to describe detailed spatial databases (e.g. geology), and
b) thematic properties such as anthropogenic units, lithotectonic features, metamorphic and textural features, etc.

In 2022, within the EU Horizon Europe programme, the project GSEU (Geological Service for Europe) started to build a geological framework. This encompasses to build a pan-European data model, a metadata system, methods to visualize 3-D models and the creation of hierarchical machine-readable vocabularies based on the earlier IGME 5000, OneG-E and INSPIRE Geology terminology.

Within GSEU, hierarchical scientific vocabularies for lithology, anthropogenic deposits and lithotectonic units are being set up for defining the concepts to which geometrical descriptions (lines, polygons, and volumes) can be linked. In future, these vocabularies will be made available in several languages to scientists in the field and in the office settings so that they can add the proper name to their mapped rock types in a harmonized way. This poster is focussing on the development of the lithology vocabularies.

The main challenges the endeavour is facing are:

• to set up vocabularies that take into account differing nomenclatures which classify the same concept (term),
• to cope with obsolete and strictly regional terms,
• to take into account multiple hierarchies and
• to include genetically related terms, qualifiers and compound names.

Custom programming scripts, written in Python and JavaScript help to automatise the data handling and visualisation of the hierarchical relations of the lithology concepts.

The poster presents the historical background of building pan-European geological vocabularies, demonstrates graphically the actual status of the created GSEU lithology vocabulary and provides an outlook to the future development.

How to cite: Asch, K., Bauer, H., Bergman, S., Flindt, A.-C., Heckmann, P., Le Guern, C., Krenmayr, H.-G., Németh, Z., Novak,, M., Pantaloni, M., Piessens, K., Schäfer, R., and Stepien, U.: One step beyond: The rocky path towards the new GSEU lithology vocabularies, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-11629, https://doi.org/10.5194/egusphere-egu25-11629, 2025.

Uncrewed Aircraft Systems (UAS) are becoming increasingly accessible to the masses.  Most small commercial drones are equipped with a camera system, and their operation is affordable by anyone.  Geological maps and models of Earth are commonly developed by a systematic investigation of the expressions of the geology outcropping on the topographic surface.

UAVs can move in three dimensions over the ground, offering the geologic surveyor a privileged point of view.

In November 2023, we organized a field campaign at the Rio Tinto area in southwestern Spain, which is considered a terrestrial analog of  Mars.  At Rio Tinto, we combined drone surveys with field investigations to understand the spatial relationship between rocks and biosignatures.  We used the drone in its basic functionalities: by acquiring overlapping images from the flying platform, we produced image mosaics and digital terrain models (DTMs) by applying Structure from Motion (SfM) algorithms.  Those images and digital terrain models become the basemaps of our large-scale geologic mapping of key portions of our study area.  Here, we will discuss the methods, the type and quality of data acquired, and the evolution of our knowledge of the problem during and after the campaign.  

Four years after the first flight on Mars by the Ingenuity Mars Helicopter, we are now experimenting on Earth with new methods for geologic survey and what will be the future of space explorations, where robotic systems will support human surveys. 

How to cite: Frigeri, A. and Skinner, J.: Geologic Mapping with UAS: New Perspectives in Geologic Surveying with the Support of Drones in Earth and Planetary Exploration., EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-18984, https://doi.org/10.5194/egusphere-egu25-18984, 2025.

The GEOS experiment onboard Amadee24 crewed simulated mission to Mars

Selina Schindler, Alessandro Frigeri, Seda Özdemir-Fritz, Gernot Grömer

During the AMADEE24 mission in Armenia, the GEOS experiment focuses on geologic survey activities at the simulated Martian landing site. GEOS applies classic geological field survey methods to a simulated mission to Mars, drawing on the experience of the lunar field survey built by Apollo missions.

The elements of GEOS are the mapping, the sampling, and the compositional measurements. The mapping phase involves developing mission-specific cartography from orbital remote sensing to large-scale mapping produced during and after the mission (Ozdemir et al., 2020). The real-time refinement of geological maps during the mission, using data from drones, rovers, and on-site observation, highlights the methodology's adaptability and receptivity. The core element of GEOS is the sampling, providing the ground truth of the remote sensing observation. AMADEE24 Rovers and Analog astronauts have done rock and terrain sampling along transects on base maps supplied by RSS (Remote Science Support) and Flight Planning (FP) for the Extra Vehicular Activities (EVAs). Part of the samples will return from the simulated Martian habitat, and made available for more advanced laboratory analyses. In-habitat compositional measurements offer a first estimate of the mineralogy and geochemistry of the samples. Specifically, AMADEE24 carried a RAMAN spectrometer in the field.

Here, we will present the results of AMADEE24/GEOS and the importance of collaborative efforts and innovative methodologies in remote science operations.

How to cite: Schindler, S., Frigeri, A., Özdemir-Fritz, S., and Grömer, G.: The GEOS experiment onboard Amadee24 crewed simulated mission to Mars, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-11685, https://doi.org/10.5194/egusphere-egu25-11685, 2025.

The Apollo mission data and samples have led to substantial advancements in our understanding of the Moon's geological history and processes. By incorporating new data from recent orbital missions, we systematically developed high-resolution geological maps for each Apollo landing site [e.g., 1-3]. The present study offers a detailed geological map for the Apollo 15 site. The Apollo 15 mission is noteworthy for its significant contributions to lunar geology, leading to substantial advancements in our understanding of volcanic activity, impact cratering, and the Moon's thermal evolution. Notwithstanding this progress, there are as yet unanswered scientific questions, which have been articulated as objectives for future missions such as the 500-day Hadley Max design reference mission (DRM) [4,5].

The Apollo 15 landing site is located east of Hadley Rille on mare basalts that border the Imbrium basin. A thorough geological mapping of the area has revealed the presence of multiple units associated with the Imbrium basin, including its rim and ejecta deposits. These units have been classified based on their distinguishing topographic features. The surrounding area also contains plains deposits, such as Imbrian light plains, along with several mare basalt units of Eratosthenian and Imbrian age [6]. Materials from nearby craters, Autolycus and Aristillus [7,8], also contribute to the region's geological diversity. The linear rilles in proximity to the site have been mapped and categorized by age, employing a combination of stratigraphic relationships and morphological analysis.

The newly developed maps have enhanced the measurement of crater-size frequency distributions (CSFDs), leading to improved N(1) values and a refined lunar cratering chronology [1-3]. Furthermore, the maps facilitate the identification of potential sample sources, thereby enhancing our comprehension of lunar stratigraphy [4,5]. Finally, these maps provide a fundamental framework for the evaluation of in-situ resources and the testing of novel technologies for forthcoming lunar missions [9].

[1] Iqbal et al. (2019) Icarus 333, 528-547.

[2] Iqbal et al. (2020) Icarus 352, 113991.

[3] Iqbal et al. (2023) Icarus 407, 115732.

[4] Daniti et al. (2024) LPSC 55, #1667.

[5] Iqbal et al. (2024) LPSC 55, #1010.

[6] Hiesinger et al. (2000) JGR 105, 29239-29275.

[7] Hiesinger et al. (2000) JGR 105, 29239-29275.

[8] Carr et al. (1971) USGS, I-723.

[9] van der Bogert, et al. (2020) LPSC 51, #1876.

How to cite: Iqbal, W., Head, J. W., Scott, D. R., van der Bogert, C. H., Wueller, L., and Hiesinger, H.: A New Geological Map of the Apollo 15 Landing Site and Its Implications, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-6065, https://doi.org/10.5194/egusphere-egu25-6065, 2025.

The lunar South Pole-Aitken (SPA) basin, the oldest, largest, and deepest impact basin on the Moon, is a high-interest target for future lunar exploration missions due to its unique geology and insights into the formation and evolution of the Moon [1]. Existing large-scale geological maps of the SPA basin [2-6] have improved our understanding of regional and global geological units [7]. However, these large-scale maps do not provide sufficient information about the detailed geology within SPA, including superposed impact basins such as the Poincaré basin, which is critical for mission planning, landing site safety assessment, resource utilization potential, and traverse planning. This study presents a detailed 1:200,000 scale geological map of the Poincaré region (159°E to 179°W, 48° to 64°S). With a diameter of 349 km, the Poincaré basin is one of the largest multiring basins superposed on the southwestern floor of SPA [3, 8-10]. Our map aims to provide the necessary geologic context for detailed planning of future exploration missions, such as the Endurance mission [2, 7].

We utilized high-resolution images from the Lunar Reconnaissance Orbiter (LRO) Wide-Angle Camera (100 m/pixel) [11], topographic data from the LRO Lunar Orbiter Laser Altimeter (118 m/pixel) [12], and Clementine data (100 m/pixel) [13]. Our map follows the standards of the Federal Geographic Data Committee [14], following the stratigraphic scheme originally proposed by [6].

We identified 10 geologic units, categorized as terra, plains, and crater materials. Our stratigraphy is based on superposition relationships and degradation stages, with absolute model ages available from the literature [e.g., 4,6,9]. The Poincaré region has a complex history dominated by impact and volcanic processes. The southern central parts of Poincaré crater are crossed by the traverses designed for the NASA Endurance rover [2]. Hence, our geologic map can contribute to the development of this mission, the definition of its scientific objectives, and evaluating the different lithologies that could be sampled by this mission and eventually returned to Earth.

[1] Duke, (2003), Adv. Space Res. 31

[2] Keane et al. (2021), Endurance mission concept

[3] Poehler et al. (2020), LPSC 51 #1951

[4] Fortezzo et al. (2020), Unified Geologic Map of the Moon, 1:5M, USGS

[5] Yingst et al. (2017), LPSC 48, #1964

[6] Wilhelms et al. (1987), USGS Prof. Pap. 1348

[7] Mouginis-Mark et al. (2021), Bull. AAS 53

[8] Pasckert et al. (2018), Icarus, 299

[9] Poehler et al. (2021), EPSC2021-646

[10] Spudis (2008), Cambridge University Press

[11] Robinson et al. (2010), Space Sci. Rev., 150

[12] Barker et al. (2016), Icarus, 273

[13] Pieters et al. (1994), Science, 266

[14] FGDC (2006), FGDC-STD013-2006

How to cite: Wueller, L., Theiner, T., Iqbal, W., van der Bogert, C. H., and Hiesinger, H.: Geologic Map of the Poincaré Region, Moon., EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-9518, https://doi.org/10.5194/egusphere-egu25-9518, 2025.

We present a detailed geologic mapping of the Bose and Bhabha crater region within the South Pole-Aitken (SPA) Basin on the farside of the Moon. This area is of significant scientific interest due to the presence of diverse geological features. The SPA Basin is thought excavate material from the lunar crust or mantle [1,2], and has been a priority for exploration, prompting numerous mission studies [e.g., 3]. The mapping was conducted using standard geologic mapping protocols [4,5] with LROC Wide Angle Camera data [6], LOLA/SELENE digital elevation models [7], and Clementine spectral data [8]. The analysis identified various geological units, including Pre-Nectarian and Nectarian materials, which represent ancient highland remnants and heavily degraded craters. Additionally, Imbrian-aged light and dark plains were identified, with the dark plains being interpreted as volcanic in origin. Eratosthenian craters, distinguished by their relatively recent morphology, were were delineated. Secondary crater chains formed across several periods; however, they are primarily observed during the Copernican period. Nevertheless, no primary Copernican craters were observed in the mapping region at the map scale. This comprehensive mapping effort provides critical information about the geological evolution of the SPA Basin and supports future mission planning, such as NASA's Endurance mission, by identifying key terrains and features of interest for exploration.

[1] Pieters et al. [2001] JGR, 106(E11), 28, 001-28,22. [2] Petro et al. (2011) GSA, 477, 129-140. [3] Jawin et al. (2019) ESS, 6. [4] FGDC (2006) FGDC-STD-013-2016. [5] Skinner et al., (2022) USGS, TM11-B13. [6] Robinson et al. (2010) Space Sci. Rev. 150, 81-124.  [7] Barker et al. (2016) Icarus 273, 346-355.  [8] Pieters et al. (1994) Science 266, 1844-1848. [9] Keane et al. (2021) MCSR, NASA

How to cite: van der Bogert, C., Iqbal, W., Theiner, J., Wueller, L., Oetting, A., and Hiesinger, H.: A New Geological Map of the Bose and Bhabha region in the South Pole-Aitken Basin, Moon, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-9649, https://doi.org/10.5194/egusphere-egu25-9649, 2025.

The renewed interest in the exploration of the Moon, both human and robotic, and the technological advancement made it more feasible to look at sites previously underrated for the paucity of high-resolution data available (e.g. polar regions) and the challenges in communication (e.g. far side), accessibility and trafficability (e.g. underground cave systems).

Being characterized by a smooth basaltic infilling, optimal for landing and roving, the far side Ingenii basin (20.4°S, 129.1°E) represents a high-profile objective for the unique presence of both extensive and complex swirls, namely features related to crustal magnetic anomalies [1,2,3], and a pit with overhanging roof possibly giving access to a lava tube [e.g. 4]. In this study, we characterized the area surrounding the Mare Ingenii Pit (MIP) and performed a feasibility study for a robotic mission with a rover-hopper [5] by considering traverses of varying lengths, all providing for a hopping phase inside the pit, and simulating the environmental conditions along their paths.

More in detail, we used the Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) mosaic (up to 100 m/px) [6] for a contextual interpretation of the area together with LRO Narrow Angle Camera (NAC) images (up to 0.5 m/px) [6] for a detailed characterization of the area surrounding the MIP. The Lunar Orbiter Laser Altimeter (LOLA) and Kaguya Terrain Camera merged Digital Elevation Model (DEM) provide the most up-to-date surface height and slope information (vertical accuracy of 3-4 m) [7] and a NAC-derived Digital Terrain Model (DTM) provides the best available elevation data for the area surrounding the pit.

We quantitatively assessed the topographical characteristics of the surface within a reasonable distance from the MIP for the positioning of landing ellipses (1500 and 500 m in diameter), and automatically detected boulders >1 m using a machine learning algorithm and NAC imagery [8]. We then planned short (up to 5 km), intermediate-length (up to 10 km) and long (up to 15 km) traverses and evaluated slope and elevation variations along the paths taking into account a typical slope tolerance of maximum 15°. Finally, we used an interactive tool provided by LROC Quickmap [9] to perform simulations of the environmental conditions along each traverse path and identify a mission operating window based on illumination and temperature conditions over a lunar day.

A lunar landing candidate site located on the far side sure entails a major effort in communicating with Earth, however, the scientific relevance and peculiarity of Ingenii basin and its optimal topographical characteristics make it a site to be considered for future exploration.

References

[1] Pinet et al. (2000) JGR, 105, 9457-9475. 

[2] Hood et al. (2001) JGR, 106, 27825-27839.

[3] Garrick-Bethell et al. (2011) Icarus, 212, 408-492.

[4] Miaja et al. (2022) Acta Astronautica, 192, 30-46.

[5] Rimani et al. (2023) Aerospace, 10(8), 669.

[6] Robinson et al. (2010) Space Sci. Rev., 150, 81–124.

[7] Barker et al. (2016) Icarus, 273, 346-355.

[8] Prieur et al. (2023) JGR, 128, e2023JE008013.

[9] https://quickmap.lroc.asu.edu/

How to cite: Tognon, G., Pozzobon, R., Melchiori, G., and Massironi, M.: Ingenii Basin: characterization and feasibility as a lunar landing site, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-19461, https://doi.org/10.5194/egusphere-egu25-19461, 2025.

Fractures are ubiquitous in rocks, representing the mechanical stresses exerted on geological materials. They are also of considerable biological interest because of their pivotal role in facilitating fluid circulation within the subsurface. The search for signs of life beyond Earth drives the European Space Agency (ESA) ExoMars Rosalind Franklin (RF) rover mission, which selected the phyllosilicate-rich region of Oxia Planum (latitude 16 °-19 ° N, longitude 23 ° 28 ° W), Mars, as its landing site. In this context, the identification and characterization of fractures are critical in guiding the search for potential biosignatures. Fracture patterns, with spacings ranging from meters to tens of meters, are observable in the region through the Mars Reconnaissance Orbiter (MRO) HiRISE camera, which provides high-resolution optical remote sensing imagery at a resolution of 30 cm per pixel. While the ExoMars team conducted a geological survey focused on the "one-sigma" landing ellipse (approximately 66.75 × 5 km, corresponding to a 67% probability of landing), we initiated a systematic mapping of fractures using HiRISE data through a grid-based mapping approach (1 km by 1 km). Our 1:50,000 scale map represents the current understanding of the spatial distribution of fractures across the "three-sigma" landing ellipse (approximately 115 × 15 km, with a 99% probability of touchdown). Fractures are classified into three categories based on their visibility at 1:5,000 map scale: clearly observable, barely observable, and not observable. By using open geospatial formats, we ensure that datasets produced at different times and in different contexts remain comparable. In this study, we compare our map of fractures with the existing geological map of the Rosalind Franklin landing site, highlighting similarities and differences. By implementing a grid-based mapping approach, we aim to extrapolate additional information and extend the current understanding of the region, providing critical information to support the surface operations of the RF rover. This extended dataset will contribute to the planning of rover exploration activities, provide a framework for testing geological hypotheses about the formation and evolution of Oxia Planum, and facilitate the identification of astrobiologically significant terrains with the potential to preserve biosignatures.

Acknowledgments: This work is supported by the ASI-INAF Mars Exploration agreement code 2023-3-HH 0. 

How to cite: Apuzzo, A., Frigeri, A., Rasmussen, M., De Sanctis, M. C., and Altieri, F.: Mapping of Fractures at the ExoMars Rosalind Franklin Landing Site, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-9490, https://doi.org/10.5194/egusphere-egu25-9490, 2025.

The mapping of planetary surfaces represents a fundamental activity in planetary science, offering invaluable insights into the formation history, surface processes, and compositional variations of celestial bodies. In addition, accurate and detailed mapping are crucial for tasks ranging from identifying potential landing sites to planning future exploration missions. These maps are primarily constructed from visible image data sets, providing topographic and albedo information which is mostly used to delineate and define the stratigraphy of geomorphological units (i.e., morpho-stratigraphic maps). However, the creation of such maps requires the specialized knowledge of expert planetary scientists and constitutes a time-intensive and highly complex task. In addition, often these maps rely solely on a geomorphology‐led approach overlooking meaningful details about composition (i.e., multispectral data) and physical properties of the defined units, with spectral information usually supplementing rather than informing geomorphological data.

This work aims to create the first set of global, explorative classification maps of Mercury’ surface which incorporate both spectral and morpho-stratigraphic information using an unsupervised learning approach based on Gaussian Mixture Models. This work represents an ambitious and promising approach for facilitating the generation of comprehensive geological maps.

In addition, this classification will facilitate geological interpretation and enhance the mapping of the planet's unexplored regions, while enriching the understanding of already surveyed regions. Such advancements are pivotal for unraveling the complexities of Mercury's surface, contributing significantly to our understanding of the planet in anticipation of the new wave of data expected from SIMBIO-SYS (Cremonese et al., 2020) data on the BepiColombo's mission (Benkhoff et al., 2021)

How to cite: Vergara Sassarini, N. A., Re, C., La Grassa, R., Tullo, A., and Cremonese, G.: Mercury: explorative geological maps through unsupervised learning , EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-19408, https://doi.org/10.5194/egusphere-egu25-19408, 2025.