Over five decades of space exploration have revealed that the Galilean moons—Io, Europa, Ganymede, and Callisto—exhibit a wide spectrum of geological and surface features shaped by the interplay of endogenous and exogenous processes. Each moon displays distinct characteristics: Callisto’s ancient, heavily cratered terrain; Ganymede’s contrasting dark and bright regions; Europa’s extensive fracture networks; and Io’s intense volcanic activity. Their surfaces are primarily composed of water ice mixed with salts, volatiles, and organic compounds, with the exception of Io, and reflect gradients resulting from complex interactions between impact processes, resurfacing mechanisms, and radiation exposure. Surface composition offers valuable clues about potential habitability of subsurface oceans, particularly on Europa, which shows evidence of recent geological activity, liquid water-rock interactions and energy sources. This paper examines how forthcoming data from the Juice and Europa Clipper missions will significantly advance our geological understanding of the moons’ surface environments and their links to the subsurface. By providing high-resolution data and long-term observations from orbit, these missions will help confirm the distribution of subsurface liquid water reservoirs, identify key chemical species—including organics—across surfaces of varying ages, and pinpoint geologically interesting, potentially habitable sites. This information, in addition to laboratory studies or field work, among other efforts will be crucial for designing future in situ exploration to one or more moons or sample return missions, enabling a deeper investigation into the origin and evolution of the Jovian system and the search for signs of life.

Ganymede is the only known moon with an active dynamo today. Previous studies interpret Ganymede's dynamo as arising from convection in a metal core that formed billions of years ago. However, Ganymede likely accreted too cold to form with a metal core, which confounds interpretations of Ganymede's magnetic field as a constraint on the moon's broader history. Here, we reevaluate the thermal evolution of Ganymede's rock-metal interior from a cold start. Our models show that Ganymede's observed dynamo is consistent with ongoing core formation, a process not yet observed elsewhere. If Ganymede has an Fe-FeS core with a sub-eutectic composition, then gradual mantle warming may expel dense Fe melt onto the growing protocore and stir liquid metal, sustaining a dynamo for billions of years.

Europa Clipper will arrive in the Jupiter system in 2030 to explore Jupiter’s moon Europa, where it will investigate the habitability of Europa’s subsurface ocean. Characterizing Europa’s ice shell and ocean through geophysical measurements will enable this overarching goal. We present a methodology to combine static gravity, magnetic induction, gravitational tides, and rotational state and orientation measurements with compositional data to characterize Europa’s hydrosphere, simultaneously constraining the ice shell thickness and the ocean thickness and salinity. We applied this methodology to a large number of plausible interior configurations to simulate a broad range of possible scenarios that Europa Clipper might encounter. The result is a prediction of the interior measurement capabilities of the mission, provided in terms of the quality of the interior recovery from the data. We find that the combination of static gravity, magnetic induction, and tidal response enables a full characterization of Europa’s hydrosphere consistent with Europa Clipper’s requirements. Measuring Europa’s tidal response will be crucial to breaking the degeneracies of the interior models to derive the ocean’s salinity. We predict that Europa Clipper will be able to meet its interior science objectives in the vast majority of cases, with the only outliers being end-member cases where the ice shell or ocean is only a few kilometers thick.

Introduction: The Cassini spacecraft orbited Saturn from 2004 to 2017, performing over a hundred flybys of Titan, Saturn’s largest moon. Ten of these flybys were dedicated to gravity measurements, yielding unprecedented insight into the moon’s interior. The first four flybys revealed a weakly differentiated deep interior, consisting of a large (~2000 km, Titan’s radius is 2575 km) and low-density (~2600 kg/m3) rocky core and a ~600 km thick hydrosphere (Iess et al., 2010). Subsequent additional radio tracking data allowed the first measurement of Titan’s response to the gravitational tides exerted by Saturn, quantified by the real part of the complex tidal Love number, Re(k2) (Iess et al., 2012; Durante et al., 2019). The inferred large value (Re(k2) ~0.6) was 2-3 times larger than pre-Cassini predictions (Rappaport et al., 2008) and indicated strong deformability over the tidal timescale. This finding was interpreted as evidence of the existence of a global subsurface ocean beneath Titan’s ice shell but escaped complete explanation. A large Re(k2) can be also generated by a viscoelastic and oceanless interior (Rappaport et al., 2008). This configuration would also produce strong tidal dissipation through shear friction, which is quantified by the imaginary part Im(k2). The detection of Im(k2) was thus indicated as a criterion to break the degeneracy between models with and without a subsurface ocean (Rappaport et al., 2008), but earlier analyses of Cassini radio tracking data could not measure the Im(k2) contribution to Titan’s gravity field.A recent analysis derived the imaginary part of k2 from Titan’s rotation state as observed by Cassini’s RADAR images, revealing a large value of Im(k2) = 0.120 ± 0.027 (Downey and Nimmo, 2025). This value corresponds to a low tidal quality factor Q ~ 5 (the Q of solid Earth is ~300), indicating strong tidal dissipation in Titan’s interior.We reanalyzed Cassini radio tracking data with improved techniques, including processing of open loop data and phase compression, to improve the assessment of Titan’s gravity field and tidal response and to confirm the recent observation of Im(k2) (Petricca et al. 2025).Figure 1: Posterior distributions for Titan’s tidal Love number k2 compared to the observations for models with and without a subsurface ocean.Results: We succeeded in measuring Titan’s gravity field and tidal response with reduced uncertainties compared to previous studies. The measured Re(k2) = 0.608 ± 0.048 confirmed the earlier value. The improved precision allowed us to detect for the first time the contribution of tidal dissipation to Titan’s gravity field, resulting in Im(k2) = 0.135 ± 0.035, consistent with results derived from Titan’s rotation (Downey and Nimmo, 2025). Because the presence of an ocean reduces the tidal dissipation generated below it, these new measurements indicate the absence of a global ocean inside Titan (Figure 1). Instead, the observations are explained by a model in which the dissipation is concentrated in high-pressure ice layer that is close to its melting point globally, as inferred from our inversion of the measurements, and is thus “slushy” (Figure 2). In addition to explaining the tidal response, the oceanless model that we introduce is the first model of Titan’s interior that can also reproduce Titan’s static gravity field and obliquity, reconciling all the geophysical observations acquired by Cassini, while requiring a geologically recent event as the source of Titan’s orbital eccentricity.The presence of a slushy layer instead of a global ocean might have profound implications for Titan’s astrobiological potential. The absence of a global ocean in Titan, despite strong tidal heating, suggests that ocean worlds may be less common than has been supposed in recent years. Although a global ocean has been considered ideal for supporting habitability, the presence of slushy layers potentially makes this world even more interesting. The interior configuration inferred from the data implies the widespread presence of melt pockets throughout the hydrosphere, potentially creating sites with highly concentrated organic and saline aqueous solutions. These solutions could be transported upward by strong convection in the ice shell, which is both indicated by the data and required to prevent the ice from melting into a global ocean. Multiple Dragonfly investigations will help constrain the physical structure of Titan’s interior, testing the ocean-free model introduced here with an independent dataset. Figure 2: The strong tidal response amplitude and dissipation preclude a global subsurface ocean and indicate a slushy high-pressure ice layer, comprising ice III (light green), ice V (light blue), ice VI (light purple) and small amounts of partial melting (fuchsia).ReferencesBabin, M. et al. 2025, Life in the frozen ocean. Ann. Rev. Marine Sci.Downey and Nimmo (2025), Titan’s spin state as a constraint on tidal dissipation, Science Advances, 11, eadl4741Durante et al. 2019, Titan’s gravity field and interior structure after Cassini, Icarus, 326, 123–132Iess et al. 2010, Gravity field, shape, and moment of inertia of Titan, Science, 327, 1367–1369Iess et al. 2012, The tides of Titan Science, 337, 457–459Petricca et al. 2025, Titan’s strong tidal dissipation precludes a subsurface ocean, Nature, 648, 556–561’Rappaport et al. (2008), Can Cassini detect a subsurface ocean in Titan from gravity measurements?, Icarus 194, 711–720.

Saturn's moon Titan exhibits remarkable parallels to the Earth in many geophysical and geological processes not found elsewhere in the solar system at the present day. These include a nitrogen atmosphere with a condensible gas - methane - replacing the Earth's water, leading to an active meteorology with rainfall and surface manifestations including rivers, lakes and seas, and the dissolution of karstic terrain. Other phenomena such as craters, dunes, and tectonic features are found elsewhere - e.g. on Mars and Venus - but their continuing alteration by pluvial, fluvial and lacustrine processes can be studied only on Earth and Titan. Meanwhile Titan also hosts an interior liquid water ocean with similarities to the Earth as well as to ocean worlds such as Europa and Enceladus. Our focus in this review paper is twofold: to describe the geophysical and geological parallels between Earth and Titan, and to evaluate the yet-underexploited possibilities for field analog research to gain new knowledge about these processes. To date, Titan's much colder temperature and different atmospheric and crustal materials have led to a skepticism that useful analogs can be found on Earth. Our conclusion, however, is that a much larger range of useful analog field work is possible and this work will substantially enhance our knowledge of both worlds. Such investigation will supplement the existing sparse data for Titan returned by space missions, will greatly enhance our understanding of such datasets, and will help to provide science impetus and goals for future missions.

Many of the outer Solar System’s icy satellites feature known or suspected subsurface oceans, at least some of which are likely situated atop rocky interiors. Water–rock interactions at and beneath these seafloors might support active chemoautotrophic habitats, with subseafloor fluid flow facilitated by active faulting and hydrothermal systems. Absent such phenomena, however, any attainment of chemical equilibrium between the seafloor and ocean might limit the availability of chemical energy for life. Here, we characterise the stress state of the seafloor of Jupiter’s moon Europa, and thus the prospect for fracturing and associated sub-seafloor fluid flow there. We consider stresses from tidal forcing, global contraction, mantle convection, and serpentinisation. We find that none of these mechanisms is likely able to drive slip along even weak, pre-existing fractures in the present. Ocean water–rock reactions taking place today are therefore probably restricted to fluid flow through only the upper few hundred metres of the seafloor. Any processes able to sustain habitable conditions at the Europan seafloor today must therefore be independent of ongoing tectonic activity. In this study, the authors model the current mechanical properties of the seafloor of Jupiter’s icy moon Europa, and find those rocks to be too strong to allow the kind of fracturing that, on Earth, enables rock–water chemical reactions on which chemosynthetic life relies.

Many icy bodies in the Solar System are hypothesized to harbor subsurface liquid-water oceans, with Jupiter's moon Europa among the most promising for astrobiology research. NASA's Europa Clipper mission will collect magnetic induction measurements to constrain Europa's ocean composition and thickness. Interpreting this information requires accurate electrical conductivity data extending to the range of possible compositions, temperatures, and pressures in Europa's ocean. Here, we report more comprehensive laboratory measurements of electrical conductivity for Europa-relevant brines (NaCl, MgSO4, NH4Cl, Na2CO3, and their mixtures) in the temperature range from 263.15-298.15 K and concentrations up to 150 g/kgH2O, at ambient pressure. This project provides critical experimental constraints for interpreting upcoming Europa Clipper data and enables stronger assessments of Europa's ocean composition and its potential to support life

Characterizing Europa's subsurface ocean is a key objective of the Europa Clipper and JUICE missions in the search for life beyond Earth. Although the ocean's induced magnetic field provides key constraints on habitability, interpretation is complicated by perturbations arising from Jupiter's plasma interaction with Europa. Physics-based models (e.g. magnetohydrodynamic, MHD) required to characterize these effects are physically comprehensive, but have a prohibitive computational cost. To address this, we introduce Learning Europa's Atmosphere and Plasma (LEAP), a transformer-based surrogate trained on outputs from a state-of-the-art multi-fluid MHD code to predict magnetic field perturbations along spacecraft trajectories. LEAP evaluates in milliseconds on a laptop, whereas MHD takes 12 hrs on a high-performance computer ( 40,000x speed-up). The model has test set errors of -/+ 2.6 nT, and for the Galileo E4 and E14 flybys of Europa it matches the parent MHD model in accuracy. Its enhanced speed enables large-scale parameter surveys and probabilistic estimations of plasma conditions, establishing a new framework for accelerated plasma interaction modeling. LEAP can also inform future MHD simulations while learning from them. Beyond Europa, this framework could be expanded to planning future missions or to other high-priority bodies, including Uranus and Neptune.

Surface observations of Saturn's moon Titan revealed features characterized as dissected, elevated plateaus with high valley density known as labyrinth terrains. Of this terrain class, a subtype referred to as radial labyrinth is described as dome-shaped uplifts with radial channel patterns. Uplift of these radial labyrinths has previously been explained as cryomagmatic intrusions at the brittle-ductile transition zone. Here we propose an alternative hypothesis that crustal heterogeneities in Titan's upper clathrate crust introduce density differentials due to ethane-methane substitution, as ethane-rich liquids percolate into methane clathrate, inducing solid state flow and generating domal topography. This mechanism is analogous to salt tectonics on Earth and has similarly been evoked for dome formation on the dwarf planet Ceres. We show that the elevation and width of the observed radial labyrinths are consistent with domal uplift driven by a hydraulic head within the uppermost portion of Titan's crust, given a plausible set of elastic parameters for clathrate hydrates. Additionally, the insulating effect of clathrate, combined with partial mixing with water-ice, allows for sufficiently low viscosity for geologic flow on a relevant timescale: uplift of the domes could have occurred within the last billion years.

Field studies at terrestrial analogue sites represent an important contribution to the science of ocean worlds. The value of the science and technology investigations conducted at field analogue sites depends on the relevance of the analogue environment to the target ocean world. We accept that there are no perfect analogues for many of the unique environments represented by ocean worlds but suggest that a one-to-one matching of environmental characteristics and conditions is not crucial to the success or impact of the work. Instead, we must determine which processes and parameters are required to map directly to the target ocean world environment with high fidelity to address the science question. In this review paper, we discuss the outcomes of a workshop aimed at developing a new framework for evaluating the suitability of analogue field locations for ocean worlds research. Here we present a two-step approach to (a) identify the most crucial processes and parameters associated with a given science question and (b) assess the fidelity of these processes and parameters at a proposed field site to those expected for the target ocean world. We demonstrate this approach in a test case evaluating three types of ocean world analogue environments with respect to a science question. The consensus document presented here equips veteran and new investigators with valuable tools to better assess and justify their analogue site selections.

The analysis of micrometer-sized ice grains emitted into space by Saturn’s moon Enceladus suggests that the moon’s subsurface ocean may be habitable. However, the formation conditions of these ice grains are largely unknown. Upon cooling, ocean droplets may supercool and then form a crystalline or glassy state, or a mixture of both. To investigate the processes of supercooling and glass formation in Enceladus’s ice grains, we performed differential scanning calorimetry experiments with Enceladus-relevant salt mixtures at cooling rates ranging from 5 K minute ^−1 to ∼1227 K minute ^−1 and extrapolated our results to faster cooling rates. We modeled the freezing of these solutions and associated mineral assemblages using the thermodynamic chemistry packages PHREEQC and Reaktoro. Our results indicate supercooling of ∼25–30 K upon freezing from Enceladus’s saline ocean. Freshly formed ice grains should be predominantly crystalline but contain up to 5% glass. Fast cooling rates and high salt concentrations favor the formation of glasses, potentially enabling the preservation of organics and cells, if present. Salts in the grains crystallize in the following sequence: first phosphate, followed by carbonates, and then chlorides. We find that the recently detected phosphates in Enceladus’s ice grains are likely Na _2 HPO _4 :12H _2 O. The pH values appear to vary among individual ice grains, depending on the stage of the freezing process, and these values may slightly differ from the pH of the moon’s bulk ocean. Our experiments and models are relevant to other icy worlds with salty water reservoirs in their subsurfaces, such as Jupiter’s moon Europa or the dwarf planet Ceres.

Europa, the most visibly active icy moon of Jupiter, is a prime target for the search for life in the outer solar system. Two spacecraft missions, Europa Clipper from the National Aeronautics and Space Administration (NASA) and the Jupiter Icy Moon Explorer (JUICE) from the European Space Agency (ESA), will observe its surface, probe its interior structure, and characterize the space environment starting in 2030. Occasional eruptions of water sourced from Europa’s interior may provide a window on the interior conditions and habitability of the moon. Here, we investigate the storage and evolution of briny water in Europa’s ice shell and propose a framework to interpret spectral, thermal, radar and gravity data collected by future missions. We show that it is possible to discriminate between water erupting from the deep ocean or from shallow liquid reservoirs using combined measurements of the material’s salinity, surface temperature and ice shell thickness.

Chemically stratified layers in the deep oceans of icy moons may strongly influence the oceans’ dynamics, thermal and chemical evolution, and therefore their habitability. Such layers can form during the differentiation of the refractory cores as they heat up due to the decay of long-lived radioactive elements. In the case of Ganymede, salts could be transported through the high-pressure ice layer to form a denser salt water layer at the base of the ocean. Such a layer would inhibit ocean convection, limiting chemical and thermal transport. It is therefore crucial to understand how these layers form and what specific signatures they may leave in geophysical observations of future space missions. The present work describes numerical simulations of the formation of stratified layers and the predicted observables that could be detected by instruments on the JUICE spacecraft. 3-D numerical simulations of Ganymede’s rotating ocean are performed with the PARODY code. Rayleigh-Bénard convection is imposed. We investigate the effect of either a constant flux of heavy salts or a fixed composition at the base of the ocean. Two regimes are identified by varying the dimensionless chemical Rayleigh (buoyancy over viscosity) and Schmidt numbers (viscosity over diffusivity). In the first regime, heavy salts are entrained and mixed in the convective region. In the second regime, the entrainment is too weak and a chemically stratified layer develops, eventually filling the entire ocean. Extrapolation to Ganymede suggests the current existence of a chemically stratified layer at the base of the ocean with a thickness close to 30 km. By considering different stratifications in Ganymede’s ocean in the PlanetProfile and ForcedTides codes, we show that signatures of stratified layers might be detected in the gravity field, induced magnetic field, and tidal deformation responses. The problem of non-uniqueness in the individual observations points to the need to jointly invert these datasets from the JUICE mission to constrain the existence and properties of stratified oceanic layers.

The Galileo mission measured the gravity field around Europa. The results indicated that the moon’s interior is mostly made of rock ( 90 wt

Introduction. Europa, the most visibly active icy moon of Jupiter, is a prime target for the search for life in the outer solar system. Two spacecraft missions, Europa Clipper from the National Aeronautics and Space Administration (NASA) and the Jupiter Icy Moon Explorer (JUICE) from the European Space Agency (ESA), will conduct extensive observations of its surface, gravity field and environment starting 2030. It has been proposed that liquid briny water reservoirs could be injected and stored in Europa’s ice shell, causing the formation of various geological features. In particular, these reservoirs could occasionally trigger eruptions [1], resulting in flows on the surface and vapor plumes in the atmosphere.If shallow liquid brine reservoirs are indeed present in Europa's ice shell, they would leave surface evidence that future missions could detect, including local thermal anomalies, ice shell thickness change, and erupted briny solutions with time varying salinity. We present a novel simulation that models thermal, physical, and compositional ice shell and reservoir evolution and eruption, and that predicts the various signatures detectable by future robotic exploration.Cryomagma chemistry. We conserve enthalpy to solve the coupled chemical evolution and pressurization of freezing brines stored in Europa’s ice shell using current best estimates of the oceanic composition [2] to predict the composition of erupted cryolava. This composition varies with time, as salts concentrate during freezing [3], which could lead to erupted brines of varying composition depending on the reservoir frozen fraction when the eruption is triggered. The equilibrium freezing of oceanic brines is modeled using the software PHREEQC to obtain the liquid and solid fraction of each component of the aqueous solution as a function of the temperature. Ice shell and reservoir modelling. We simultaneously model the ice shell and reservoir thermal, physical, and compositional evolution self-consistently building upon the framework of [4]. We solve for the conservation of enthalpy using conservative finite differences in a one-dimensional (1D) spherical shell, propagated explicitly forward in time. The thermophysical properties of the multiphase model are temperature-, pressure-, and composition dependant, thus the composition and physical state are consistently updated at every time step. Finally, modeled eruption frequency and eruptive characteristics are dependent on the properties and their gradients in ice surrounding the reservoir.Results. Outputs of the model include the temporal evolution of the temperature in the ice shell, reservoir, and at the surface, and the time of eruptions and erupted cryomagma composition (Fig. 1).Figure 1: Temporal evolution of signatures of a 1 km thick cryomagma reservoir located 1 km bellow the surface.Acknowledgements. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). This work was supported by NASA’s Solar System Workings program (grants #80NM0018F0612 and #80NSSC20K0139)References. [1] Lesage et al. (2022) PSJ 3(7), 170, [2] Melwani Daswani et al. (2021) GRL 48(18), [3] Naseem et al. (2023) PSJ 4(9), 181, [4] Howell, S. M. (2021) PSJ 2(4), 129.

The Cassini mission provided unprecedented insights into Saturn's largest moon, Titan, from its atmosphere to the deep interior1. The moon's large measured response to the tides exerted by Saturn was interpreted as evidence of the existence of a subsurface ocean2,3. This response, twice the value predicted in pre-Cassini studies, has escaped complete explanation. Here we show that the signature of tidal dissipation in Titan's gravity field is not consistent with the presence of an ocean. Our results arise from the detection of this signature through a reanalysis of the radiometric data acquired by Cassini with improved techniques. We found that substantial energy is being dissipated in the interior (approximately 3-4 TW, corresponding to a tidal quality factor Q ≈ 5), consistent with recent studies of Titan's rotational state4. Because the presence of a liquid layer reduces the tidal dissipation generated below it5, these new measurements preclude the existence of a subsurface ocean on Titan and are explained by a model in which dissipation is concentrated in a high-pressure ice layer close to its melting point. This model also reproduces Titan's observed rotational state and static gravity field self-consistently, reconciling all available geophysical measurements. Efficient ice shell convection can prevent widespread melting and ocean formation, but a slushy high-pressure ice layer is consistent with expectations6, indicating that it probably hosts liquid water pockets. The forthcoming Dragonfly mission to Titan will provide a further test of whether a subsurface ocean exists.

Enceladus is among the most intriguing bodies in the solar system due to its astrobiological potential. Determining the extent and duration of habitability (i.e., sustained habitability ) requires characterizing the interior properties and the level and distribution of tidal heating in Enceladus. Inferring the intensity of geophysical activity in the core has direct implications for the potential hydrothermal activity and supply of chemical species important for habitability to the ocean. We build a statistical framework to constrain the interior using estimates of libration, shape, heat flux, gravity, and total mass. We use this framework to examine the extent that geodetic measurements can improve our understanding of the interior structure, with an emphasis on partitioning of dissipation between the shell and the core. We quantify plausible ranges of gravitational ( k _2 ) and displacement ( h _2 , l _2 ) tidal Love numbers consistent with existing observations. We demonstrate that measuring k _2 alone can only constrain the total tidally dissipated energy, not its radial distribution. However, measuring the amplitude and phase of h _2 or l _2 facilitates determining the extent of tidal dissipation in the shell and the core. We provide the precisions required for measuring k _2 , h _2 , and l _2 that enable distinguishing between the main tidal heating scenarios, i.e., in the shell versus the core. We also explore the effect of the structural heterogeneities of the shell on the tidal response. Lastly, we evaluate the efficacy of future geodetic measurements to constrain key interior properties essential to understand the present-day ( instantaneous ) and long-term ( sustained ) habitability at Enceladus.

The magnetometer investigation of the Galileo mission used the phenomenon of magnetic induction to produce the most compelling evidence that subsurface oceans exist within our solar system. Although there is high certainty that the induced field measured at Europa is attributed to a global-scale subsurface ocean, there is still uncertainty around the possibility that the induced field measured at Callisto is evidence of an ocean. This uncertainty is due to the presence of a conductive ionosphere, which will also produce an induction signal in response to Jupiter's strong time-varying magnetic field. Therefore, it is not yet known whether the observed induced field is attributable to the ionosphere, an ocean, or a combination of both. In this work, we use previously published simulations of Callisto's plasma interaction in combination with both an inverse and an ensemble forward modeling method to highlight the plausible range of interior properties of Callisto. We further constrain the ocean thickness and conductivity, ice shell thickness, and ionospheric conductivity that are required to explain the Galileo magnetometer observations. This is the first study to jointly consider all flybys to constrain the driving field and three flybys (C03, C09, and C10) to assess the induction response. Our results suggest that Callisto's response more likely arises from the combination of a thick conductive ocean and an ionosphere rather than from an ionosphere alone.

In order to improve our understanding of the interior structure of Saturn's small moon Enceladus, we reanalyze radiometric tracking and onboard imaging data acquired by the Cassini spacecraft during close encounters with the moon. We compute the global shape, gravity field, and rotational parameters of Enceladus in a reference frame consistent with the International Astronomical Union's definition, where the center of the Salih crater is located at -5 degrees East longitude. We recover a quadrupole gravity field with J3 and a forced libration amplitude of 0.091 degrees +/- 0.009 degrees (3-sigma). We also compute a global shape model using a stereo-photoclinometry technique with a global resolution of 500 m, although some local maps have higher resolutions ranging from 25 to 100 m. While our overall results are generally consistent with previous studies, we infer a thicker 27-33 km mean ice shell, a thinner 21-26 km mean ocean thickness, and a mean core density range of 2,270-2,330 kg/m3. Geodetic data, such as shape, gravity, and rotation, provide important constraints for probing a planetary body's interior structure. We analyze radiometric tracking and onboard imaging data acquired during close encounters of Enceladus by the Cassini spacecraft to compute geodetic products including topographic and gravitational fields in a common reference frame. The recovered Enceladus topography has a global resolution of 500 m, with some local regions having 25-100 m resolution. Our study suggests that Enceladus has a 27-33 km mean ice shell thickness, a 21-26 km mean ocean thickness, and a mean core density range of 2,270-2,330 kg/m3. A full quadrupole gravity field with J3 and the forced libration amplitude of 0.091 degrees +/- 0.009 degrees are recoveredA 500-m resolution global topography model was computed, with some local regions having 25-100 m resolutionThe results suggest that Enceladus has a 27-33 km mean ice shell thickness, a 21-26 km ocean thickness, and a mean core density range of 2,270-2,330 kg/m3