I am working on understanding and contributing towards the LISA “Global Fit” problem, starting with the existing approaches in the literature and a critical evaluation of their respective strengths and limitations. Building on this groundwork, I will be working on developing and refining new statistical frameworks in an iterative fashion, incorporating advanced sampling techniques to improve efficiency and robustness, in addition to using GPU acceleration and modern programming design patterns to optimize performance. These methods will first be tested on simplified or restricted versions of the full Global Fit problem before being extended to more exotic scenarios. Thus, I will execute and expand existing data analysis pipelines, integrating machine learning-assisted inferences and inference tools into a single, coherent environment to enhance the construction of the so-called "global fit" and reconstruct the LISA sky
The solar atmosphere consists of the photosphere, chromosphere, transition region, and corona. The corona, the outermost layer, extends for hundreds of thousands of kilometers into interplanetary space and is much fainter than the solar disk, making it invisible to the naked eye except during a total solar eclipse or with dedicated instruments. The Sun undergoes an 11-year activity cycle, during which the corona’s structure changes significantly, displaying different properties and features. During solar maximum, sunspots, coronal mass ejections (CMEs), and flares increase, exciting various magnetohydrodynamic (MHD) waves, including quasi-periodic fast-propagating (QFP) magnetosonic wave trains. The physical mechanism responsible for the generation and propagation of QFP wave trains in the solar corona remains poorly understood. While several events have been analyzed and modeled via numerical simulations, key questions regarding the origin and evolution of this phenomenon remain open. To investigate further, we analyze a coronal event that occurred on October 5, 2023, in which a CME was followed by QFP wave trains. Using high-cadence data in visible light from the METIS coronagraph onboard Solar Orbiter, we measure the physical parameters of the magnetosonic wave train.
Ultra luminous X-ray sources (ULX) are extragalactic, off-nuclear X-ray sources exceeding the Eddington luminosity of stellar-mass black holes and it is believed that ULXs host super-Eddington accreting neutron stars or stellar mass black holes. However, the exact proportion of the two populations of compact objects is not yet known. I am conducting a comprehensive X-ray spectral analysis of the two ULXs in the nearby galaxy NGC 1313, using new (2025) XMM-Newton and NuSTAR observations complemented by archival datasets. I have performed the data-reduction and a complete spectral analysis of the available datasets, performing broadband modeling in the 0.3–30 keV range to constrain the geometry of the accretion flow and a tempted to unveil the nature of the compact objects host in these sources. A central goal of the project is to investigate emission and absorption features around ~1 keV, which produce persistent residuals in several observations, and may be the imprint of a powerful optically thick outflow in the systems.
The inclusion of archival data enables a systematic study of the stability and variability of these spectral features over time, helping to clarify the physical conditions of the circum-source environment and the role of supercritical accretion processes in shaping the observed spectra.
Since coherent pulsations are not always detectable, spectral diagnostics become crucial for distinguishing between accreting neutron stars and black holes. This work aims to clarify the nature of the ULX population in the NGC 1313 galaxy and to improve our understanding of extreme accretion regimes.
Very Low Earth Orbit (VLEO, <250 km) presents significant advantages, including reduced communication latency, enhanced imaging resolution, and improved radiation shielding. However, maintaining operations at these altitudes is challenging due to increased atmospheric drag. To overcome this, Air-Breathing Electric Propulsion (ABEP) systems have been proposed, enabling satellites to collect and ionize residual atmospheric gases as propellant—eliminating the need for onboard fuel storage.
Among the potential propulsion technologies, Electron Cyclotron Resonance (ECR) thrusters are particularly well suited to VLEO’s low-density gas environment due to their efficient plasma generation using high-frequency microwaves. Nonetheless, developing compact and power-efficient ECR systems for CubeSats remains a major challenge. Conventional microwave systems often suffer from low conversion efficiency, especially at frequencies above 2.4 GHz.
The aim of this research is to develop compact and efficient microwave power electronics for ECR-based ABEP systems suitable for CubeSat platforms. During the first months of this research, efforts have been focused on understanding techniques to enhance the efficiency of power amplifiers (PAs) for the specific application of plasma generation.
Our research stems from the acknowledgment of the gap in the understanding of women’s health as compared to men’s. This project will develop on two parallel levels, focusing on human behaviour and cellular environment.
Both anxiety and vestibular dysfunctions are among the most reported complaints in space travels.
Starting from the epidemiological observations that highlight the comorbidity between vestibular disorders and anxiety pathologies, and that hint to some putative shared cortical areas devoted to the processing of these functions, the aim is to deepen the knowledge on this relationship and on the influence gender may have on it. The hope is to pave the way for new therapeutic strategies, possibly involving the use of neuromodulatory techniques.
The other part of the project has the objective of better characterising the influence that altered gravity has on the cellular functions. The higher prevalence of anxiety in women suggests the investigation of sex-specific steroidal hormones as possible contributors to this epidemiological difference. Human SH-SY5Y cell cultures will be used to understand the effects of microgravity on cellular stress and inflammation markers and how this equilibrium changes at different concentrations of female sex hormones, oestradiol and progesterone, to replicate the different phases of the menstrual cycle.
I am Riccardo Chiartano, a first-year PhD student in Space Science and Technology (SST) at the University of Trento, currently based at the INAF-Astrophysical Observatory of Turin (OATo). Under the supervision of Dr. Silvano Fineschi and Dr. Roberto Susino, my research focuses on the diagnostics and instrumentation for space weather investigation from multiple solar missions.
My expertise in coronal studies is rooted in both space-borne and ground-based observations. I presented a poster at the Space It Up! Days conference regarding the April 2024 Total Solar Eclipse campaign in Mexico. During this campaign, I contributed to the data analysis and laboratory calibration of E-KPol instrument, a polarimetric study of the solar corona that serves as a precursor and validation tool for current space missions.
Currently, my work is deeply integrated into the ASPIICS/Proba-3 mission. I contributed to the instrument's polarimetric and radiometric calibration and developed a web application for data analysis and visualization, which I recently presented at the First ASPIICS Data Workshop in Bucharest (November 2025). Recently, my technical activity has also focused on improving the continuum subtraction techniques for ASPIICS narrow-band images, in the Fe XIV and He I D3 lines.
My doctoral research aims to exploit the scientific synergy between ASPIICS and Metis/Solar Orbiter, integrating multi-instrument datasets to better understand the physical mechanisms of the solar corona.
Tsunamis are the most dangerous natural disasters that can affect lots of regions and have an economic and demographic impact. These phenomena can be described as giant waves caused by earthquakes or volcanic eruptions under the sea.
My research activity consists of the description of this kind of phenomenon using a high-resolution numerical simulation. This computational tool couples a modified Surface Gradient Method with high-order shock-capturing techniques and validates the implementation against standard benchmark tests.
I explore multiple risk scenarios associated with Marsili-induced tsunamis. The model solves the depth-averaged Shallow Water Equations using a shock-capturing HLL scheme combined with the cut-cell technique to represent coastal boundaries accurately. Realistic bathymetric data were employed to simulate tsunami propagation over an area of approximately 69 km², encompassing northern Sicily, western Calabria, and the Aeolian Islands. The results provide scenario-based constraints that support tsunami preparedness planning and offer a numerical framework for future, more detailed inundation assessments in the southern Tyrrhenian Sea.
Another phenomenon that is part of the research is the meteo-tsunami dynamics. Unlike tsunamis are produced by seismic activity or an underwater landslide, meteo-tsunamis are driven by the weather (pressure often plays a substantial role), and in most cases are associated with fast-moving storm systems.
I am working on the characterization of Low Gain Avalanche Diodes (LGADs) for space applications. The LGADs are silicon sensors that use impact ionization to achieve an internal gain of O(10) and timing resolution of O(30 ps). The typical channel size in high-energy physics experiments is about few mm square. Experiments in space could benefit from a Time-of-Flight system with precise timing capability to distinguish the primary particle shower from the back-scattered component. However, the requirement of low power consumption on space-based experiments imposes that a low number of channels must be read-out and therefore the channel size must be scaled up to cover a larger area. This impacts the timing capability of the detector due to increased capacitance and signal propagation effects.
My work focuses on the study of signal propagation in large area LGAD sensors. I am characterizing strip sensors produced at FBK with radioactive sources and a Transient Current Technique setup equipped with a red and an infrared laser that mimics the passage of a charged particle in sensor. I am comparing measurements with SPICE simulations in which capacitive and inductive coupling effects with neighbouring strips and with the PCB back plane are included. Preliminary results show that simulations can qualitatively reproduce the non-uniformity effects observed experimentally in the signal shape in of large area LGAD sensors.
Within the LiteBIRD collaboration, a satellite mission scheduled for the 2030s to conduct full-sky polarization measurements of the Cosmic Microwave Background (CMB) in search of signatures from primordial gravitational waves induced by cosmic inflation, my research focuses on spin-based mapmaking. This technique enables the fast and accurate simulation of stationary systematic effects by deprojecting time dependencies onto "h-maps" at the mapmaking level. These h-maps encapsulate information about the scanning strategy; the systematics are then modeled as additional spin maps alongside the spin-0 and spin-±2 components corresponding to intensity and polarization. By circumventing the need for full time-ordered data (TOD) simulation, this method drastically reduces computational costs. Furthermore, it may used as a tool for systematics mitigation, allowing for the deprojection of unwanted spin signals induced by systematic effects directly during the mapmaking process.
My current research focuses on the use of innovative matched filter techniques for greenhouse gas (GHG) detection and flux estimation from hyperspectral imagers, with particular emphasis on PRISMA and future IRIDE missions. A key component of this work is the exploitation of TROPOMI–IASI synergy to identify GHG concentration anomalies, which are subsequently investigated at higher spatial resolution using hyperspectral imaging data.
Previously, my research centered on atmospheric radiative transfer modeling in the mid-infrared for IASI applications, contributing to improved forward modeling accuracy in cloudy conditions. I also conducted studies on Antarctic cloudiness, including analyses of cloud properties over the Antarctic Plateau and intercomparisons between ground-based and satellite-derived cloud products.
As a complementary line of research, I develop methodologies for the performance assessment of binary classifiers in the presence of imperfect or noisy labels, with applications to remote sensing and environmental data analysis.
Model-Based Engineering and Formal Methods for Space Systems.
Space systems become more complex nowadays. A spacecraft must perform its mission in nominal mode as much as possible, but also stay usable even though faults occurs. There are many things that can goes wrong in such system. Sensors can drift, software cane behave unexpectedly. The question is: how do we design systems that can remain reliable?
This research explores the use of formal methods to bring a rigor and automation into the design of space systems. Instead doing safety analysis as an afterthought, the goal is to build it the same time as the design process from the very beginning, using a shared mathematical model of the system itself that everyone on the team works on.
The practical focus is on Fault Detection, Isolation, and Recovery (FDIR). The component that allows a system to recognize fault, contain it, and recovery from it. Using the ROSACE flight controller as a case study, system requirements have been formally defined using LTL/STL like-wise formula, and verified against simulation traces, confirming that the controller meets properties like settling time, overshoot limits,...
The next steps involve injecting realistic faults into the simulation, building automated recovery logic, and explore how machine learning can support anomaly detection. The goal is define a breakthrough way to design robust and dependable space systems.
My PhD project focuses on the study of compact objects - primarily black holes and neutron stars - through the time-domain behaviour of high-energy transients. By analysing variability, outbursts and spectral state changes in accreting systems, I aim to constrain the physical mechanisms that govern accretion flows and their coupling to outflows over a broad range of luminosities and timescales.
My approach combines X-ray spectral and timing analyses with multi-wavelength context, using observations from major high-energy facilities and time-domain surveys to build consistent physical interpretations for individual events and source populations. I rely on robust data-reduction and analysis workflows, systematic source characterisation, and rapid follow-up strategies to identify the most informative episodes (e.g. fast flares, quasi-periodic variability, transient spectral features) and to link observable diagnostics to the geometry and energetics of the inner accretion region.
Beyond advancing our understanding of compact-object accretion and transient phenomenology, this work contributes to maximising the scientific return of modern time-domain astronomy by improving the identification and interpretation of rare or short-lived high-energy events.
Skeletal muscle atrophy is a debilitating condition characterized by the loss of mass, strength, and function. During spaceflight, gravitational unloading acts as a primary catalyst for muscle wasting, driven by profound disruptions in energy homeostasis and protein turnover. Current research is limited by the lack of translatable human models; thus, we are developing an Engineered Muscle Tissue (EMT) platform: a physiologically relevant 3D biomimetic model designed to recapitulate microgravity-induced atrophy in vitro. By employing integrated transcriptomic and metabolomic profiling, we seek to comprehensively map the molecular signatures and metabolic shifts driving this degradation. The platform is currently being optimized for integration with Random Positioning Machines (RPM) to simulate microgravity. We hypothesize that unloading will elicit hallmark atrophic markers, including decreased Smad1/5/8 phosphorylation and the up-regulation of E3 ubiquitin ligases, such as Atrogin-1 and MuRF1. Within this framework, we aim to demonstrate that Tacrolimus can attenuate these effects by enhancing BMP signaling, whereas iron supplementation might have a role in optimizing mitochondrial function and mitigating oxidative stress, consistent with findings in other atrophy models. Ultimately, this EMT platform will provide a pivotal tool for validating pharmacological countermeasures and supporting drug repurposing in space medicine.
Distributed Multiple-Input Multiple-Output (MIMO) radar systems represent a breakthrough technology for airborne and spaceborn applications, offering enhanced spatial resolution and superior target detection capabilities. However, the distributed nature of these networks introduces critical signal processing challenges, particularly regarding geometric uncertainties and phase errors that severely degrade signal coherence and image quality.
My research activity focuses on advancing signal processing techniques explicitly tailored for distributed MIMO systems. The core activity revolves around two main pillars: detection algorithms and autofocus algorithms.Firstly, the research investigates robust detection algorithms with a strong emphasis on geometric calibration. Accurately estimating and correcting the spatial positions of distributed radar nodes is essential to ensure phase synchronization across the entire network. Secondly, the project develops advanced autofocus algorithms, such as the Phase Gradient Autofocus (PGA) technique. These algorithms are critical for estimating and compensating for residual, unmeasured phase errors typically caused by platform motion, orbital variations, and atmospheric anomalies.
By combining precise geometric calibration with PGA-based autofocus, this research aims to restore optimal signal coherence. The ultimate goal is to significantly improve imaging, focus and overall reliability of next-generation distributed MIMO radars.
I am an Electronics Engineer and M.Sc. Astronomy with experience in design and development of astronomical instrumentation for radio astronomy, solar physics, interferometry and satellite communications. My background includes the development of a radio interferometer to study radio emissions from the Sun, particularly from active regions, and its impact on space weather. Also I was in charge of the design, characterization, testing and verification of satellite communications antennas for CURIE (Cubesat Radio Interferometry Experiment).
My current research focuses on the development of high-sensitivity X-ray detectors for astronomical imaging, spectroscopy, and polarimetry. I am currently working on the development of a hybrid pixel detector with a custom analog-readout ASIC, designed for high resolution spectroscopy and imaging in the 1-50 keV energy range. I perform tests for the experimental validation of the prototype, in terms of gain, energy resolution and position reconstruction, as well as analyse the data collected on each test-run. Additionally, I contribute to the development and refinement of the software tool to perform simulations and data analysis.
In parallel, I also conduct tests to characterize alternative prototypes for gas pixel detectors for X-ray polarimetry, with embedded charge-multiplication stage, and improvements on gain and energy resolution, with respect to previous generations of GPDs, for optimal spectral and polarimetric performance.
Davide Luchina's research focuses on computational and observational cosmology, in relation with both space- and ground-based experiments, with particular emphasis on the Sunyaev-Zel'dovich effect and other secondary anisotropies in the Cosmic Microwave Background (CMB). He is a member of the Euclid Collaboration, working on the cross-correlation between these anisotropies and the survey's main probes: galaxy clustering and cosmic shear.
My current work revolves around the 4 Test Mass (4-TM) facility, one of the two torsion pendula in the LISA Laboratory at the University of Trento. This is the main instrument aimed at the investigation of the force noise for LISA, an ESA mission whose planned launch date is in July 2035. Once in orbit, this constellation of 3 satellites will be the first detector of gravitational waves in space; it will open new possibilities for the observation of low-frequency gravitational waves, allowing, in particular, for the study of supermassive black holes in a completely new way.
The 4-TM facility allows for the measurements of very small forces (under 0.1 pN) in an environment representative of that of LISA. Until now, I had the opportunity to perform measurements to characterize a force given by the position sensing itself, the so-called "stiffness". In addition, in order to prepare for a facility upgrade that should finish near the end of March 2026, we performed charge measurements of the test masses. Once the work on the facility is completed, we will perform extensive testing in order to characterize the new performance levels.
More long-term, I will participate in the LISA testing campaign for one piece of the satellite, the Gravitational Reference System (GRS). A number of Italian universities and industries, coordinated by ASI, are responsible for the delivery of the GRS subsystem for the final integration on the satellites.
My research focuses on very-high-energy gamma-ray astrophysics and involves two major Imaging Atmospheric Cherenkov Telescope facilities: the MAGIC telescopes and LST-1, the first Large-Sized Telescope of the Cherenkov Telescope Array Observatory (CTAO). I analyse gamma-ray bursts (GRBs) observed by MAGIC and LST-1 between 2019 and 2026, with particular emphasis on events jointly observed by the two facilities. Using the magic-cta-pipe framework, I aim to improve the sensitivity to VHE emission and derive more stringent upper limits. These results will help characterise GRB emission at the highest energies and constrain the physical mechanisms powering these transient events. In parallel, I investigate subarray divergent pointing as a potential observing strategy for CTAO and other next-generation Cherenkov facilities, including ASTRI and LACT. The aim is to increase sky coverage while preserving sufficient telescope multiplicity, enabling faster follow-up observations and increasing the probability of detecting transient events. This strategy could be particularly valuable for identifying VHE counterparts of transients detected by missions such as Fermi/GBM and, in the near future, COSI. Overall, my research explores the synergy between space-based gamma-ray missions and ground-based Cherenkov observatories to maximise the scientific return of coordinated observations.
Title: The Moon’s Surface Composition, Environment, and Active Physical Processes
Abstract:
My PhD project focuses on the scientific requirements of lunar resource exploration
instruments, to aid in the detection and local mapping of resources such as Rare Earth
Element (REE) rich minerals on the lunar surface. These instruments, especially the
Gamma-ray spectrometers, X-ray fluorescence (XRF) instruments, Hyperspectral stereo
cameras and UV fluorescence spectrometers, are under development at INAF for
deployment on a lunar rover.
Currently, the work revolves around defining the spectral parameters of REE-rich minerals in
the VIS range and studying their response under ultraviolet radiation. This mainly includes studying the minerals using an optical spectrometer and the ATLAS Apex XRF
Spectrometer, which provides the initial data for building the elemental composition map of
the interested mineral. Initial works on the project also revolve around getting familiar with other necessary laboratory instruments, such as the Malvern Morphologi 4 particle analyser for regolith simulants and a lunar simulation chamber for instrument response tests.
Further, remote sensing work using Lunar Prospector - Gamma ray spectrometer data was carried out to generate lunar elemental maps with respect to thorium, potassium, uranium, etc. Remote sensing work is performed using orbital data with different spatial resolutions to examine the best resolution to map REE enrichment using spectral features. Defining the scientific requirements for these instruments forms the primary basis in their development for extended lunar surface research.
During space missions, our physiological mechanisms change dramatically, mainly due to changes in gravity. This alteration leads, among other factors, to an irregular shift of bodily fluids, with a particular impact on the vestibular system, explaining the prevalence of "space sickness" and feelings of disorientation.
The aim of the project is therefore to study whether these perturbations can influence the functionality of the auditory system, and how our ability to perceive sounds is conditioned by vestibular perturbations.
The extension of state authority beyond the Earth’s atmosphere represents one of the most complex challenges for contemporary international law, requiring a profound reflection on the intersection between physical borders and cyber domains within the corpus juris spatialis. In this context, Luca’s research is conceived as an investigation aimed at deciphering the legal framework for the protection of individuals beyond both planetary and cyber boundaries, in a setting where space law has traditionally been anchored to the concept of res communis omnium and the principle of freedom of exploration.
The core of the analysis lies in the “subtle line of demarcation” between the public powers of states—often framed as imperatives of national security—and the intangible sphere of the individual’s fundamental right to privacy. The paradigm shift in data governance finds in Regulation (EU) 2016/679 (GDPR) an inalienable pillar of fundamental rights. Its uniform application has transformed data protection from a mere technical norm into a cornerstone of the European legal order, projecting a normative due diligence that obliges operators to maintain high standards even in extra-atmospheric activities. This protection becomes critically relevant in satellite monitoring, particularly regarding Article 22 of the GDPR, which safeguards individuals from decisions based solely on automated processing that produce legal effects or significantly affect them. The ability of satellite systems to collect and process massive amounts of data using artificial intelligence algorithms necessitates constant vigilance, ensuring that outer space does not become a blind spot for individual rights.
My research focuses on the development of advanced data analysis techniques for future space- and ground-based gravitational wave observatories, with particular emphasis on the LISA mission and its scientific potential. My main goal is to contribute to the development of inference methods capable of extracting accurate source information in complex, multi-signal scenarios, and to extend this approach across different detectors.
My first project investigated the potential impact of correlations among massive, transient sources on LISA data analysis, assessing how source confusion may affect their detection and Bayesian inference performance. This study aims to better understand the limitations and requirements of realistic data analysis pipelines in the presence of overlapping signals.
While my long-term research will primarily concentrate on LISA data analysis, with a focus on resolved sources, my current project extends the same global inference approach to next-generation ground-based detectors. In particular, I am implementing computationally efficient sampling strategies for a prototype multi-source framework, with the goal of enabling reliable parameter estimation in scenarios involving multiple signals.
Monitoring the distribution of Earth’s water stores over time is crucial for understanding the long-term effects of climate change and for the informed management of water resources, among other applications. Inter-satellite geodesy missions such as GRACE and its successor GRACE-FO have carried out this monitoring through the use of satellite pairs equipped with accelerometers which continuously measure the gravity field around Earth. Current missions are limited to a resolution of 10^-10 m/s^2/Hz^1/2 due to the harsh conditions of a low Earth orbit and design constraints of the accelerometers. The current LISA gravitational reference system (GRS) design has been shown to be adaptable for application in future geodesy missions with the potential for an improvement on current test mass (TM) acceleration noise limits down to the 10^-12 m/s^2/Hz^1/2 range. We continue to evaluate potential design configurations such as a LISA-like configuration and an "X preference" configuration which would eliminate actuation (and actuation noise) in the sensing X direction. The range of actuation forces applied to the TM within the GRS have a significant impact on TM acceleration noise and final performance. We investigate the level of force actuation in a low Earth orbit to determine the design configuration needed to reach the goal precision. Additionally, we will address several key design tradeoffs for implementing a GRS aimed at reaching the pm/s^2 level in a future geodesy mission.
My research project focuses on the time-domain analysis of Active Galactic Nuclei (AGN) with the goal of identifying candidate binary or dual AGN systems in current large-scale surveys. I analyze AGN light curves using a Bayesian framework based on Gaussian Processes, which provide a flexible, non-parametric approach to model stochastic variability while robustly quantifying uncertainties. AGN variability is typically dominated by red-noise processes, making it challenging to distinguish intrinsic stochastic behavior from potential periodic or quasi-periodic signals that may indicate the presence of a supermassive black hole binary. By applying Gaussian Process models within a Bayesian inference scheme, I can compare competing variability models and assess the significance of periodic components. The methodology is applied to photometric data from current time-domain surveys such as Gaia, Zwicky Transient Facility, and Pan-STARRS. By combining advanced statistical modeling with large survey datasets, the project aims to improve the reliability of binary/dual AGN candidate selection and contribute to our understanding of supermassive black hole evolution and galaxy mergers.
Advanced models for the design and characterization of deployable structures.
Deployable structures, such as large antennas and solar sails, are essential for overcoming volume constraints during space launches. Accurately predicting their nonlinear mechanical response—especially when involving complex kinematics and composite materials—remains a major engineering challenge. My research centers on the development of high-fidelity computational models grounded in high-order finite element methods and unified theoretical frameworks such as the Carrera Unified Formulation (CUF). These models are aimed at simulating the structural behavior of large deployable systems, with particular emphasis on nonlinear interactions and multi-scale mechanics of materials, including Carbon Fiber Reinforced Polymers (CFRP) and soft hyperelastic membranes, throughout the deployment process. Current work focuses on performing geometrically nonlinear simulations to evaluate stiffness evolution and stress distributions. Ongoing research integrates these structural models with multibody dynamic formulations to analyze deployment sequencing and strain energy storage. Ultimately, the numerical framework will be validated against experimental data from scaled prototypes to assess predictive accuracy and ensure structural reliability in the space environment.
My PhD research focuses on advanced signal-processing methods and the development of image-focusing and subsurface-imaging algorithms for planetary radar sounder data. The work is aligned with ESA’s Jupiter Icy Moons Explorer (JUICE) mission and its Radar for Icy Moons Exploration (RIME) instrument. The main objective is to improve the quality, resolution, and interpretation of radar images of the subsurface geology of icy moons. Current work involves developing and evaluating processing and imaging algorithms using both simulated data and real-world planetary datasets.