Introduction

The IDEFIX rover has been integrated into the Martian Moons eXploration (MMX) mission spacecraft and is awaiting launch in October 2026. Upon arrival at the Martian moons, the rover will be deployed to the surface of Phobos and will perform the first ever technical demonstration of wheeled mobility on a small Solar System body [1]. The rover is equipped with four scientific instruments for characterizing the surface properties of Phobos: RAX, a Raman spectrometer, the NavCams, a stereo pair of cameras, miniRAD a radiometer, and the WheelCams. The WheelCams, with a pixel resolution of approximately 100 µm, will provide direct images of the surface and will capture the dynamic interaction between the rover wheels and regolith [2]. These cameras will allow for a unique, in-situ characterization of the surface material on Phobos. Still images will provide information regarding the size and morphology of the grains, the bulk mechanical properties of the regolith, and the possible layering within the shallow sub-surface of Phobos [2]. Dynamic images will be used to assess the clumping, shearing, and flow behavior of the regolith and the overall thrust and performance of the rover. The cameras can be used as a stand-alone instrument during nominal driving operations or be paired with the rover NavCams to augment the scientific output from other unplanned, but possible mobility tests, such as pivoting, driving in reverse, extending/retracting the rover legs, or excavating the regolith with a single wheel.

In anticipation of the in-situ rover operations on Phobos, we have developed a preliminary pipeline for simulating and analyzing the eventual images from the IDEFIX WheelCams. We produce representative WheelCam images using 1) optical simulations that combine the 3D rover CAD with the ANSYS programs Zemax and SPEOS and 2) experiments with the ISAE-SUPAERO WheelCam testbed [3].  Currently, the optical simulations are used to estimate the camera field of views and the quality of the images for various rover configurations, and the experimental images are used to characterize surface grain morphology [4,5], trench morphology [6,7], wheel sinkage, and wheel velocity. Together, the simulated and experimental images will provide a robust framework to support the IDEFIX operations and scientific analysis on Phobos.

Simulated images

The IDEFIX rover includes two WheelCams, which are mounted at different angles within the rover chassis. The front WheelCam is tilted at an angle of approximately 42 degrees and points at the undisturbed surface ahead of the front rover wheel. The rear WheelCam is tilted by approximately 45 degrees and shows the trench that is created by the front wheel. When the rover is in the nominal driving configuration, the front and back wheels are within the field of view of each respective camera.

Fig. 1: 3D rover CAD showing the fields of view for the front WheelCam (red) and the rear WheelCam (green)

We use the 3D rover CAD (Fig. 1), in combination with ANSYS OpticStudio to simulate the fields of view, resolution, and focus of the cameras for different rover configurations (e.g., when the rover is high vs. low sinkage configurations or when the rover legs are articulate to some off-nominal rotation angle). The simulations will be used to correct the perspective of the WheelCam images and to assist with operation planning for the WheelCam instrument.

Experimental images

In addition to performing optical simulations, we generate experimental images using the WheelCam testbed at ISAE-SUPAERO [3]. The testbed includes flight-spare LEDs, provided by CNES, and a representative rover wheel, provided by DLR. The testbed cameras are positioned to replicate the fields of view from the nominal driving configuration, and the experiments are performed with comparable exposure times and luminosity conditions as the actual WheelCams. Fig. 2 shows representative images from the front (top row) and rear (bottom row) testbed cameras for experiments with various granular materials.

Fig. 2: Representative views from the IDEFIX rover WheelCams for experiments using (a, d) gravel, (b, e) coarse sand, and (c, f) a Phobos regolith simulant [8]. The images for the front and rear testbed cameras are shown in the top and bottom rows, respectively. The rear testbed images have been rotated by 90 deg.

The image processing pipeline consists of algorithms that characterize both the wheel and surface properties. We begin by correcting the testbed images for distortion and then track points around the rim of the wheel to construct a homography matrix to transform the images based on camera perspective. The object detection is also used to determine the rotational velocity of the wheel, and the transformed images are used to calculate wheel sinkage. Static images are used to characterize the morphology of the grains around the wheel [4,5] (Fig. 3), while a series of images are used to determine local surface topography and trench morphology [6,7].

Fig. 3: Identified grains for the trench morphology analysis from WheelCam testbed experiments in (a) gravel, (b) Lunar simulant, (c) Phobos simulant, and (d) coarse sand [5].

As part of future work, the pipeline will be extended to characterize regolith flow around the wheel, identify and track the motion of clumps, determine rover forward velocity, and extract trench features such as the angle of repose. Together, these observables will be linked to the physical properties of the Phobos surface, providing a robust foundation for the in-situ data analysis and ultimately contributing to the broader MMX science objectives regarding the origin and evolution of the Martian moons.

Acknowledgements

This work was funded by CNES in the context of the MMX IDEFIX rover and the WheelCams.

References

[1] Ulamec, S., et al. Acta Astronautica 210 (2023): 95-101.

[2] Murdoch, N., et al. Progress in Earth and Planetary Science 12.1 (2025): 54.

[3] Sunday, C., et al. Review of Scientific Instruments. In preparation (2026).

[4] Robin, C. Q., et al. Nature communications 15.1 (2024): 6203.

[5] Robin, C. Q. Institut Supérieur de l’Aéronautique et de l’Espace. PhD Thesis (2026).

[6] Amsili, A., et al. EPSC2024-407. Copernicus Meetings (2024).

[7] Amsili, A., et al. Advances in Space Research. Submitted (2026).

[8] Miyamoto, H., et al. Earth, Planets and Space 73.1 (2021): 214.

How to cite: Sunday, C., Billot, D., Amsili, A., Duchene, A., Robin, C., Vivet, D., Wright, E., Baroukh, J., Lalucaa, V., Théret, N., Torres, A., Tardivel, S., Bertrand, J., Vernazza, P., Michel, P., Ulamec, S., and Murdoch, N.: Simulated images from the IDEFIX rover WheelCams, Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-426, https://doi.org/10.5194/epsc2026-426, 2026.

Introduction

The primary goal of the ESA Rosalind Franklin mission (RFM) is to search for past and present life on Mars [1], launching in 2028. Enfys is a new near-infrared spectrometer, added to the mission in 2023, with Flight Model delivery in 2026. The RFM rover will land in Oxia Planum in 2030, and Enfys will form part of the suite of remote sensing instruments used for exploration and target selection. Given the importance of near-infrared spectroscopy in selection of the landing site [2-4], Enfys will play a major role not only in mission operations, but also in helping to link orbital and in situ observations and interpretations, vital for rover missions [e.g. 5].

Updated Instrument Design

The function of Enfys is based around two near-infrared Linear Variable Filters (LVTs), each with a dedicated detector. An uncooled InGaAs photodiode is paired with a LVF covering the wavelength range 0.9 – 1.7 mm. A cooled and enhanced InGaAs photodiode is paired with a LVF covering the wavelength range 1.6 – 2.5 mm. Both LVFs are translated simultaneously on a mechanical stage. The Enfys Optical Box sits on top of the EMRF mast, co-aligned with and directly underneath the High Resolution Camera (HRC) element of the Panoramic Camera (PanCam) instrument [6].

Instrument Synergy

Embedded within the design is an overlap in wavelength range with PanCam, allowing synergy between multispectral imaging and point spectroscopy. Together these instruments provide contextual remote sensing information, prior to selection of drill sites. Enfys data will be complementary to the other near-infrared spectrometers on EMRF, namely Ma-MISS [7], which will collect data from within the drill hole, and MicrOmega [8], which will analyze the drill core once collected, prepared and delivered into the analytical suite inside EMRF.

Scientific Preparations

To maximise the scientific return from Enfys, a variety of geological analogue testing is currently underway with Enfys emulators and simulations. Expected performance of the Enfys instrument will be presented through (1) analogue samples collected during fieldwork campaigns, (2) ESA mission analogue reference sample analysis, (3) end-to-end spectroradiometric numerical simulations of the Enfys response to spectral libraries ofof phyllosilicate, and other likely martian minerals.

Acknowledgements: We are grateful for support from the UK Space Agency (grants ST/Z510427/1, ST/Z510415/1, ST/Y005996/1, ST/Y005287/1).

References: [1] Vago, J.L., et al. (2017) Astrobiol. 17, 471-510. [2] Quantin-Nataf, C. et al. (2021) Astrobiol. 21, 345-366. [3] Mandon, L., et al. (2021) Astrobiol. 21, 464-480. [4] Brossier, J. et al. (2022) Icarus 115114. [5] Fraeman, A.A. et al. (2020) JGR 125, e2019JE006294. [6] Coates, A.J. et al. (2017) Astrobiol. 17, 511-541. [7] De Sanctis, M.C. et al. (2017) Astrobiol. 17, 612-620. [8] Bibring, J.-P. et al. (2017) Astrobiol. 17, 621-626. [9] Seelos, K.D. et al. (2019) LPSC 50, #2745. [10] Million, C.C. et al. (2022) LPSC 53, #2533.

How to cite: Grindrod, P. M., Cousins, C., Stabbins, R., Hagan-Fellowes, S., Nielson, G., Marsh, H., Langston, J., Tomes, J., and Gunn, M.: Scientific Preparation for the Enfys Spectrometer on the Rosalind Franklin Rover, Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-466, https://doi.org/10.5194/epsc2026-466, 2026.

Introduction

An important component in the exploration of planetary bodies, such as Mars, relies heavily on in-situ mineralogical analysis to uncover the geological history and also investigate potential habitability and organic content. Raman spectroscopy has emerged as a cornerstone technique in planetary in-situ exploration as it enables the identification of minerals and organic compounds [1]. It had its debut in planetary research with two Raman instruments on NASA’s Perseverance rover [2,3] which landed in Jezero crater, Mars, in February 2021 and has been collecting in-situ Raman data from the Martian surface since then. Raman spectroscopy will also be used in upcoming planetary missions, such as JAXA’s Martian Moons eXploration (MMX) mission with the RAman spectrometer for MMX (RAX) [4, 5] and ESA’s ExoMars rover with the RLS (Raman Laser Spectrometer) [1], both operating at 532 nm. In this study we present external-cavity diode lasers (ECDLs) as a promising alternative to frequency-doubled Nd:YAG lasers for space-borne Raman Spectroscopy.

Background

External-Cavity diode lasers (ECDLs) address the growing demand for compact, tunable, and energy-efficient laser sources in planetary Raman spectroscopy, where in-situ mineralogical analysis requires high spectral resolution. Due to their compact design, high electrical-to-optical conversion efficiency, direct electrical modulation capability, and low étendue [6], diode lasers are especially attractive for space-borne instruments. Recent advances in semiconductor technology now enable green-emitting diodes (520–530 nm), offering a flexible, semiconductor-based alternative to traditional frequency-doubled Nd:YAG lasers at 532 nm. By embedding these diodes in an external cavity, we narrow their broad gain spectrum to longitudinal single-mode operation with linewidths of 1cm⁻¹, meeting the requirements for high-precision Raman measurements. The tunability of ECDLs further enables shifted-excitation Raman difference spectroscopy (SERDS), which suppresses fluorescence by capturing spectra at slightly shifted wavelengths (~1 nm), thereby enhancing the signal-to-noise ratio for weak Raman signals in fluorescent backgrounds [7, 8].

Methodology

In this work, we present two external-cavity setups for green diodes, specifically designed for in-situ Raman measurements under planetary conditions:

• A Littrow configuration, known for its simplicity and reliability (see Figure 1).
• A filter-based configuration, combining a narrow bandpass filter with a cat’s-eye reflector.

By embedding the diodes in an external cavity, we narrow their inherently broad emission to achieve longitudinal single-mode operation with linewidths of 1 cm⁻¹ (Littrow setup), meeting the requirements for high-resolution Raman spectroscopy.

For the Littrow configuration, we systematically evaluated eight laser diodes based on emission wavelength, optical output power, and tuning range. The filter-based setup was tested with two diodes to assess their tuning range and maximum single-mode output power. The Littrow configuration was selected as the primary setup due to its established reliability and simplicity, making it ideal for initial testing and characterization of the diodes and ECDL system.

Figure 1: Sketch of the Littrow configuration, where the grating is mounted on a piezo actuator for fine adjustment of the cavity length [9].

Results  

Our results with the Littrow setup demonstrate wide tuning ranges across multiple diodes, with three diodes achieving the target wavelength of 532 nm which is demonstrated in Fig. 2. This positions them as direct, semiconductor-based alternatives to frequency-doubled Nd:YAG lasers for instruments like RAX [9]. The filter-based setup exhibits different tuning behavior compared to the Littrow configuration. Furthermore, its maximum single-mode output power is lower, indicating limited suitability for our application. Additionally, initial radiation hardness tests confirm the operational robustness of the diodes, marking a critical step toward flight qualification.

Figure 2: Tuning range of eight different diodes in the Littrow setup. Three of them achieving the target wavelength of 532nm.

Conclusion

This study bridges the gap between laboratory characterization and practical space applications, demonstrating that green ECDLs are a viable alternative to Nd:YAG lasers for next-generation planetary instruments. Key findings show that the Littrow setup is better suited for such applications than the filter-based configuration. The compact size, efficiency, and tunability of ECDLs make them a compelling alternative to traditional solid-state lasers, while their compatibility with 532 nm ensures seamless integration into existing mission instruments. Additionally, their ability to perform SERDS further enhances their utility, enabling high-sensitivity Raman measurements even in the presence of strong fluorescence.

References:

[1]: Rull et al., 2017
[2]: Bhartia et al., 2021
[3]: Lopez-Reyes et al., 2025
[4]: Hagelschuer et al., 2022
[5]: Schröder et al., this conference
[6]: Angel et al., 1995
[7]: Zhao et al., 2002
[8]: Böttger et al., 2017
[9]: Lukaszewski et al., in revision

How to cite: Lukaszewski, J., Dietz, E., Schröder, S., Buder, M., and Hübers, H.-W.: Green External-Cavity Diode Lasers for Space-Borne Raman Spectroscopy, Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-495, https://doi.org/10.5194/epsc2026-495, 2026.

Introduction

Understanding the geological history of planetary surfaces profits from linking the chemical composition of samples to their texture at fine scales. In the context of planetary exploration, this has been demonstrated, for example, by the mapping x-ray fluorescence instrument PIXL onboard NASA's rover Perseverance [1,2,3].

Another technique that has proven valuable for in-situ elemental analysis on the Martian surface is Laser-Induced Breakdown Spectroscopy (LIBS) [4,5,6,7]. By focusing a pulsed laser beam onto a target, a small plasma is generated whose emission spectrum yields information on major and minor elements including light elements such as H. LIBS requires no sample preparation, removes surface dust, and can be operated at standoff distances of several meters.

While the first generation of planetary in-situ LIBS instruments [4,5,6,7] were designed for point-to-point analysis at several meters, current efforts focus on developing LIBS instruments capable of resolving submillimeter heterogeneity by performing multiple LIBS measurements in a raster [8,9] at smaller working distances.

As a partner for the µLIBS development led by CNES and IRAP [8,9], DLR developed a particularly lightweight scanning unit (<130 g) to acquire dense elemental grids on geological samples at sub-millimeter resolution. The main drivers for the design were the low mass and volume budgets. The DLR scanner prototype allows for 2D scanning by using a two-axes configuration and was developed to TRL6 for Mars in 2024.

Here, we show its integration into a LIBS setup with an imager and a vacuum chamber to simulate extraterrestrial low pressure environments analog to Mars or airless bodies. The configuration of the setup is described and first measurements obtained on a natural heterogeneous rock are reported.


Setup

The LIBS setup with the prototype scanner is shown schematically in Figure 1. A Nd:YAG laser (1064 nm, 5 ns) delivers pulses of ≈8 mJ. After beam expansion, the laser is transmitted through a dichroic beam splitter and focused. The two-axes prototype scanning mirror directs the focused beam through an optical window onto the sample. The system achieves a maximum scan area of 8×8  cm at a working distance of ≈25 cm, and a minimum repeatable step size for grid points of 0.73 mrad in the tilt-axis direction and 1.46 mrad in the rotary-axis-direction.

The plasma emission is collected coaxially along the same optical path, ensuring that the collection efficiency remains uniform across the entire scan field and that each spectrum corresponds to the exact location addressed by the scanning mirror. So far, the setup requires adjusting the focus manually or bringing the sample into the focus distance. Plasma emission and light collected by the camera are separated from the laser line by the dichroic and filtered by a short-pass with an effective cut-off near 765 nm. A 10:90 beamsplitter divides the light between two detection channels: the larger fraction is coupled to a compact spectrometer (350–900 nm, 0.4 nm) via an optical fiber, while the remaining fraction is imaged onto a commercial camera. Each spectrum is co-registered with a context image of the ablation position and it is possible to define a precise pixel coordinate in contextual images for each spectrum.

While the sample chamber will allow for measurements in low pressures, the first results presented below were acquired in ambient air.

Figure 1: Left: schematic drawing of the µLIBS-Scanner-Setup. Right: Picture taken of the setup in the lab.

First results

5x5 grids of LIBS measurements with a scanner step size of down to 1.46 mrad step size were acquired on flat, heterogeneous natural rock samples (Figure 2). At each point, 30 LIBS spectra were recorded using an integration time of 300 µs and averaged. Typical characteristic atomic and ionic emission lines can be seen, confirming the presence of several major and minor elements (Si, Al, Ca, Na, Fe, Mg, H, N, O, Li). N emission comes from the ambient atmosphere.

To demonstrate the elemental mapping capability without having a quantification in place, we are indicating the major emission of two major elements in the LIBS spectrum per raster position with a colored circle.  We chose Na as felsic indicator of the light toned matrix and Ca emission as an indicator of the darker mafic material. 

Raman spectroscopy revealed quartz and plagioclase on the light-toned areas and Ca amphibole (hornblende) from the darker areas.

Figure 2: Left: Full scale context image where red circles mark the 5x5-LIBS grid. Top right: Zoomed-in view. Bottom left: Color markers placed on each grid point for the dominant Ca or Na lines.

Summary and outlook

We show the implementation of a particularly small and lightweight scanning unit prototype (TRL6) into a laboratory LIBS setup that also hosts a co-aligned imaging system. Using a vacuum chamber, Martian atmospheric conditions can be simulated. The system can ignite suitable plasmas within a raster of 8x8 cm on flat samples without refocusing. Minimal reproducible angle between measurement positions is 1.46 mrad which translates to distances of ≈0.35 mm on the sample surface.

First measurements on a heterogeneous natural rock sample demonstrate the setup's ability to identify compositional variation at submillimeter scale. Ongoing work includes the acquisition of LIBS data at simulated Martian atmospheric and airless conditions and advance data processing and analytical methods in combination with image data for improved insights on geochemically heterogeneous targets including potentially limiting operational aspects.

References

1. Liu Y. et al. (2022) Science 377, 1513–1519.

2. Kizovski T. et al. (2025), nature communications, 16, 6470

3. Christian J. et al. (2026) Icarus, 453, 117060

4. Maurice S. et al. (2021) Space Sci Rev 217,

5. Wiens R. C. et al. (2022) Adv. 8, eabo3399.

6. Beyssac O. et al. (2023) JGR: Planets, 128, 7

7. Xu W. et al. (2021) Space Sci. Rev. 217, 64.

8. Rapin W. et. Al (2024) LPSC 2024, 2670

9. Rapin, W. et al. (2025) EPSC-DPS2025-1829

How to cite: Krybus, N., Schröder, S., Dietz, E., Bergen, T., Buder, M., Egerland, C., Mourlin, F., Rammelkamp, K., Rapin, W., Schrandt, F., Seel, F., Walter, I., and Hübers, H.-W.: Advancing LIBS for geochemical micro-mapping with lightweight prototype scanner, Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-959, https://doi.org/10.5194/epsc2026-959, 2026.

Introduction: Analyses of extraterrestrial samples enables to better assess the processes responsible for the wide diversity of solar system properties. Specifically, NIR hyperspectral imagery complement the NIR remote sensing of asteroids and planetary surfaces, in enabling tracking diagnostic major and minor constituents of sampled material, that are witnesses of the formation and evolution of their parent bodies, with their potential role when imbedded within Solar System objects. MicrOmega has been developed to detect and map such key constituents in mm-sized samples, directly in situ as a space instrument, and in the laboratory whenever returned samples are available.

The Instrument: MicrOmega is a near-IR hyperspectral microscope developed at the Institut d’Astrophysique Spatiale in Orsay, France [1]. The instrument delivers (x,y λ) spectral cubes from 0.99 to 3.65 µm, over a 5×5 mm² field of view, with a ~20 µm pixel size. Its spectral range, spectral sampling and focal depth have been chosen to enable, in a compact, light and robust instrument, the identification of most potential constituents: silicates, oxides, salts, hydrated minerals, ices and frosts, as well as organic compounds, discriminating between specific members in each family (e.g. low and high Ca pyroxenes, forsterite and fayalite, Mg and Al rich phyllosilicates, aliphatic and aromatic compounds, different types of carbonates and sulfates, etc. [2]). One prime goal is to observe the interrelation between the various phases and minerals, including those only present in small abundances (e.g. a few grains within the rock) or restricted to fractures or pores. Moreover, data processing enables not only to identify and locate grains of specific composition, but also to quantify their abundance.

MicrOmega on Mars: MicrOmega has been developed to be the first instrument to analyse the drilled samples inside the Rosalind Franklin rover of the ExoMars mission, to be launched in 2028 [1]. The rover will drill samples down to 2 m depth at the surface of Mars, and distribute them to the Analytical Laboratory Drawer (ALD) in the body of the rover for detailed mineralogic and molecular analysis. MicrOmega aims to characterize the composition of these samples at the grain size scale, in a non-destructive way.

Together with the flight model integrated in Rosalind Franklin, a flight spare of MicrOmega is installed in a dedicated set-up at Institut d’Astrophysique Spatiale [3]. The instrument is set in a glove box under controlled atmosphere and temperature to allow the safe use of the instrument under different conditions. A large number of synthetic and natural Earth analogues for Mars have been analysed within this set-up and has shown the capability of MicrOmega to map a large diversity of minerals [2], and to detect organic molecules even in small amount, in different mineral settings.

MicrOmega and extraterrestrial samples: MicrOmega is now  also used to analyse extraterrestrial samples in the lab.

The set-up with the flight spare of MicrOmega/ExoMars allows the analysis of precious extraterrestrial samples continuously out of contact with the Earth atmosphere. Meteorites, and samples from Ryugu (JAXA/Hayabusa2 mission), Bennu (NASA/OSIRIS-ReX mission), and the Moon (CNSA/Chang’E-5 mission [4]) have been and will be analysed in this facility.

Another model of MicrOmega has been integrated in the curation facility for the Ryugu and Bennu returned samples at ISAS/JAXA extraterrestrial samples curation center (EsCuC). This MicrOmega model observes all samples from both carbonaceous asteroids curated in Japan, maintained in clean chambers under N₂, before their distribution to the scientific community [5, 6]. With these very dark samples, MicrOmega is sensitive to phyllosilicate signatures and how they are affected by space weathering (e.g. [7]), carbonates, phosphates, and CH- and NH-rich compounds as small as a few 10s µm.

In particular, MicrOmega has been able to help us better understand the water/rock interactions in the Ryugu and Bennu’s parent bodies in the early Solar System. For example, the instrument has mapped and distinguished different types of carbonates in samples from both asteroids, and has quantified their presence over a large portion of the returned material [8, 9].

MicrOmega has also been used to study the presence of key elements for the appearance of life, that have been delivered to the early Earth by carbonaceous asteroids: the instrument identified in Ryugu a class of hydrated minerals rich in P, Mg and ammonium that are more easily soluble than previously identified Ca-phosphates [10] ; it has also shown a number of grains enriched in NH associated to ammonium-bearing phyllosilicates both in Ryugu and Bennu [11]. 

[1] Bibring et al. (2017) Astrobiology, 17, 621-626. [2] Loizeau et al. (2022) Astrobiology, 22, 263-292. [3] Loizeau et al. (2020) PSS, 193, 105087. [4] Jiang et al. (2026) this conference [5] Pilorget et al. (2022) Nature Astronomy, 6, 221-225. [6] Pilorget et al. (2025) Nature Comm., 16, 9532 [7] Nardelli et al. (2026) this conference. [8] Loizeau et al. (2023) Nature Astronomy, 7, 391-397. [9] Mahlke et al. (2026) accepted in the Planetary Science Journal. [10] Pilorget et al. (2024) Nature Astronomy, 8, 1529-1535. [11] Jiang et al. (2026) Nature Comm., in press.

How to cite: Loizeau, D., Bibring, J.-P., Pilorget, C., Hamm, V., and MicrOmega team, T.: MicrOmega: a generic hyperspectral microscopic imager to characterize extraterrestrial samples, in space and in the lab, Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-1084, https://doi.org/10.5194/epsc2026-1084, 2026.

The inter-planetary dust (IPD) environment offers key insights into planetary origins and poses significant hazards to space exploration. Due to their high velocities (> km/s), IPD particles, including micrometeorites, typically disrupt when they impact with a surface, and so they are difficult to collect directly or to inspect with images. Current IPD particle measurements rely on indirect surface charge estimations, providing little information on the nature of the particles, such as morphology and compactness.  Addressing these properties is vital to understand dust aggregate growth in planetary formation, and distinguishing between natural and anthropogenic debris sources as human activities in space increase. In addition to the case of IPDs, dust levitation and transport near terrestrial surfaces help understand the geological and exospheric conditions of the Moon, Mars, and comets. However there is no current method to directly track Lunar or Martian dust dynamics. Previous studies tracking cometary dust were conducted at low time resolutions, leaving gaps in understanding the dust ejection mechanisms . While ultra-high-speed imaging systems for particle sizing and dynamical measurements are well-established on Earth, there are no applications of such technology in space environments.  I will present the status of an ESA-sponsored tech-development study, conducted in collaboration with industry [LaVision GMbH], that aims to adapt Earth-based high-speed particle imaging technology to meet the scientific and technical requirements for tracking dust and debris in space. This effort is supported by ground-based experiments at the University of Stuttgart , and the results of the experiments will be discussed.

How to cite: Capelo, H.: Experiments in support of a novel technology to image and study dust-grain dynamics  in-situ , Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-1162, https://doi.org/10.5194/epsc2026-1162, 2026.

How to cite: Paton, M., Scaccabarozzi, D., Martínez-Oter, J., Genzer, M., Appiani, A., Erauzquin, M., Gonzalez, M., Juárez, D., Haukka, H., and Harri, A.-M.: Assessment of penetrator technologies for Enceladus, Europlanet Science Congress 2026, The Hague, The Netherlands, 6–11 Sep 2026, EPSC2026-609, https://doi.org/10.5194/epsc2026-609, 2026.