High-resolution spectroscopy is essential for resolving fine spectral features that reveal important physical processes in planetary, astrophysical, and heliophysical environments. However, traditional high-R instruments are large, complex, and incompatible with compact or distributed space platforms. We present a new generation of Spatial Heterodyne Spectroscopy (SHS) systems that overcome these limitations through a fully integrated, all-reflective, and monolithic design. Optimized for the FUV/EUV regime (10–200 nm), our SHS architecture delivers resolving powers of R ~20,000–100,000 in a compact form factor (<2U volume, <10 kg), making it ideal for CubeSats, SmallSats, and deep-space missions. We highlight critical system-level innovations, including thermal, optomechanical, and detector interfacing, as well as a validated performance model that includes sensor and electronics noise, optomechancial alignment tolerance, calibration and operation stability. These developments establish SHS as a scalable, high-fidelity spectroscopic solution for the next generation of space science missions.

Astrophotonics is the application of versatile photonic technologies to channel, manipulate, and disperse guided light from one or more telescopes to achieve scientific objectives in astronomy in an efficient and cost-effective way. The photonic platform of guided light in fibers and waveguides has opened the doors to next-generation instrumentation for both ground- and space-based telescopes. Utilizing the photonic advantage is a promising approach to massively miniaturize the next generation of spectrographs for ground- and space-based telescopes. I will discuss some of our recent results from our efforts to design and fabricate high-throughput on-chip astrophotonic spectrographs. These devices are ideally suited for enabling exciting science cases, such as measuring exoplanet masses and characterizing exoplanet atmospheres. I will also discuss specific approaches to make this technology science-ready and qualified for the next generation of space missions and potentially, planetary missions.

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 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 is 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: uplift of the domes could have occurred early in Titan’s history, a billion years ago, or could have uplifted within the last 100 Myr during a recent phase of orbital excitation.

In this talk I will share our recently published results on the detection of potential biosignatures within the Neretva Vallis ancient riverbed on Mars, and then extend outward to our efforts to characterize and explore worlds of the outer solar system that harbor contemporary liquid water oceans beneath lithospheres of ice. At least six ice-covered moons of the outer solar system present compelling evidence for subsurface oceans, and thus provide highly compelling targets in our search for life beyond Earth. I will focus on Jupiter’s moon Europa, and detail experiments conducted in my lab that help us better understand Europa’s ocean chemistry and surface morphology. If time permits, I will also provide an overview of missions that will explore these worlds in the coming decades, and describe how exploration of Earth’s ocean and cryosphere is helping to guide our understanding of the potential habitability of these alien oceans.

Martian meteorites provide key information about the geological history of Mars. However, our collection is biased by geologically young samples that are not representative of Mars’ exposed surface, which is dominated by ancient rocks. This generates gaps in our knowledge of Mars’ early evolution. Recently, we discovered that a Martian meteorite, Teghaza 001, is a gabbroic diorite with a crystallization age > 4.1 Ga. In this presentation, I will describe this unique sample, how it compares to other Martian meteorites and igneous rocks studied by rovers, what results imply to our understanding of early Mars differentiation.