Experimenters from four different argon dark matter searches have joined their forces in the “Global Argon Dark Matter Collaboration” to carry out a unified program for dark matter direct detection.  The participants are researchers currently working on the ArDM experiment at LSC; on the DarkSide-50 experiment at LNGS; on the DEAP-3600 experiment at SNOLab; and on the MiniCLEAN experiment at SNOLab.

In 2015/2016 the DarkSide-50 experiment at LNGS produced two zero-background science results, along with a comparison of the results obtained with both atmospheric and underground argon fills, demonstrating the ability of large experiments to eliminate background from betas/gammas at the tens of tonne-year exposure.  Early in 2018, the DarkSide Collaboration announced results from a 2-years campaign with DarkSide-50, resulting again in a zero-background, null observation of heavy (>50 GeV/c2) dark matter and in the best exclusion limits for light (<10 GeV/c2) dark matter.

The DEAP-3600 experiment at SNOLAB is the first tonne-scale experiment to achieve both stable operations and an extended physics run.  DEAP-3600 has been collecting physics data with over 3 tonnes of argon since late 2016 and published its first results in 2017.

Researchers from the four experiments will jointly carry out as the single next step at the scale of a few tens of tonnes the DarkSide-20k experiment.  DarkSide-20k was approved in 2017 by the Italian INFN, by the host laboratory LNGS, and by the US NSF.  DarkSide-20k is also officially and jointly supported by the three underground laboratories LNGS, LSC, and SNOLab.

DarkSide-20k is a 20-tonne fiducial volume dual-phase TPC to be operated at LNGS with an underground argon fill, designed to collect an exposure of 100 tonne×years, completely free of neutron-induced nuclear recoil background and all electron recoil background.  DarkSide-20k is set to start operating by 2021 and will have sensitivity to WIMP-nucleon spin-independent cross sections of 7.4×10−48 cm2 for WIMPs of 1 TeV/c2 mass, to be achieved during a 10 year run with an exposure of 200 tonne×years.  DarkSide-20k will explore the WIMP-nucleon cross-section down to the edge of the ’neutrino floor’, where coherent neutrino-nucleus scattering from environmental neutrinos induce nuclear recoils in the detector.

A second step in the program is the construction and operation of Argo, a detector with a fiducial mass of a few hundred tonnes, capable of collecting an exposure of several thousands of tonne×years, completely free of all backgrounds on top of CNNS.  This follow-up experiment would also be capable of performing a set of very high precision measurement of several solar neutrino sources (location and laboratory t.b.d.).  This includes exquisitely precise measurements of pep, CNO, as well as low energy 8B neutrinos, all in the region of transition between the vacuum- and matter-dominated regions of solar neutrino oscillations.

Ten years after the first detection of a gravitational-wave signal, the LIGO Observatories are the most sensitive detectors in the world. We’ll discuss the principles of gravitational wave detector technologies, the current limitations to the LIGO sensitivity and the LIGO Laboratory plans to improve the detectors over the next decade.

The Cosmic Microwave Background (CMB) is an amazing observable, which has unlocked many mysteries about the beginning and evolution of the universe.  Although discovered more than 60 years ago, what can still be learned from the CMB remains extremely exciting.  CMB measurement has been enabled by advances in cryogenic focal plane technology.  In this talk, I will give an overview of the detectors and readout technology used for precision measurements of CMB temperature and polarization.  I will overview the principle of detection for both transition-edge-sensor (TES) bolometers and microwave kinetic inductance detectors, as well as discuss sensitivity limits.  Recent and historic examples will be given throughout, and I will conclude with an outlook for the future.

The axion remains a compelling particle candidate for dark matter.  The Axion Dark Matter Experiment, ADMX, has explored a range of plausible axion models for dark matter over the last decade, but a comprehensive search of promising parameter space requires an improved detector.  I will discuss the QCD axion as a candidate for dark matter, the current progress of the ADMX search, and the emerging technologies that are being developed to improve the search: quantum sensing, superconducting resonators, and more.

In recent years, graph neural networks (GNNs) have shown tremendous promise in solving problems in high energy physics, materials science, and fluid dynamics. In this work, we introduce a new application for GNNs in the physical sciences: instrumentation design. As a case study, we apply GNNs to simulate models of the Laser Interferometer Gravitational-Wave Observatory (LIGO) and show that they are capable of accurately capturing the complex optical physics at play, while achieving runtimes 815 times faster than state of the art simulation packages. We discuss the unique challenges this problem provides for machine learning models. In addition, we provide a dataset of high-fidelity optical physics simulations for three interferometer topologies, which can be used as a benchmarking suite for future work in this direction.

Modern scientific instruments increasingly rely on image sensors and single-photon detectors to capture rare, fast, and data-rich events. As sensor arrays scale, moving raw data can become a central limitation in power, bandwidth, latency, and information preservation. This talk will introduce detector and image-sensor hardware foundations, relevant to experimental cosmology and dark matter detection. Challenges in large-scale photon sensing will motivate a broader question of what should be computed, compressed, protected, or filtered before data leaves the sensor front end. Rather than treating AI as a generic add-on, the talk will examine targeted on-sensor functions such as early multiply-and-accumulate operations, temporal frame filtering, security-aware image transformation, and compact event encoding. Advanced semiconductor integration, including 3D-stacked image sensors and near-pixel memory, will be discussed as a practical path toward closer coupling of sensing and computation.

The LIGO Scientific Collaboration is pursuing a major detector upgrade called A#. This is an upgrade in the current facilities with the joint goals of extracting the best possible science from our facilities and demonstrating the new technologies we plan to use in the next generation Cosmic Explorer detector. A key change to the LIGO detectors will be the deployment of many small interferometric sensors. The dramatic improvements to noise and calibration enable new opportunities for global optimization and control.

In 2019 a few of us proposed a far-future concept for an array of deeply quantum ~gram scale systems to search for dark matter purely via gravity. I will discuss some very recent/upcoming experiments representing the modern incarnation of this idea, with much more modest goals: arrays of mildly quantum ~femtogram scale systems to look for heavy sterile neutrinos and some non-gravitational dark matter interactions. Based on this I'll offer a few comments on the gravitational detection idea."

In the recent fourth astrophysical observing run of the Advanced LIGO detectors, major instrumentation upgrades have dramatically increased detector sensitivities to expand the observational horizons of the LIGO detectors. In particular, the filter cavity upgrade to frequency-dependent squeezing was implemented, resulting in broadband quantum noise reduction across much of LIGO's astrophysical detection band. This approach changes the squeezed quantum noise quadrature as a function of frequency to reduce both quantum radiation pressure noise at low frequencies and shot noise at high frequencies -- suppressing detector quantum noise below the Standard Quantum Limit while achieving up to 6 dB of shot noise reduction. Still, next generation detectors target 10-dB of robust quantum noise reduction measured across all observational frequencies, in interferometer facilities that circulate 2-5x higher laser powers, and may reach baselines up to 10x longer than today's 4 km facilities. Achieving 10 dB of usable squeezing in future detectors requires advances across the board, and I will describe some efforts and ideas towards reduced optical losses, improved diagnostics, and greater flexibility for quantum noise shaping and optimization.

What limits a superconducting-sensor experiment depends on the regime it operates in, and I will use that to frame a common set of challenges across cosmology, dark matter, neutrino physics, and quantum information. For background-limited measurements such as the CMB, the single sensor is already noise-limited, so sensitivity comes from operating and reading out ever-larger arrays. This is where multiplexed readout dominates. In next-generation CMB, microwave SQUID multiplexing and the SMuRF platform together now field of order 100,000 background-limited superconducting detectors at multiplexing factors around 1000. For the vast QCD axion dark matter search parameter space, for low-mass scattering/absorbing dark matter, and for coherent elastic neutrino-nucleus scattering, gains are to be made in the sensor or amplifier by lowering energy thresholds and noise, and pushing toward and past the standard quantum limit. As this happens, scaling soon follows. Superconducting qubit-based sensors for these applications blur the line further, with measurement protocols that motivate readout and control co-designed with the device. I will trace these regimes, the technologies they share, and the cross-field synergies I hope we can discuss.

Superconducting sensors are a cornerstone of modern frontier physics, driving discoveries from the early universe to the quantum world. In this talk, I will discuss the diverse applications and synergistic development of superconducting detector technologies, highlighting how advancements in one discipline frequently drive progress in others. The extensive R&D and vital industry partnerships established for CMB-S4 detector fabrication have resulted in new pathways for fabricating superconducting sensors. These advancements are now actively enabling highly sensitive new detector arrays for Line Intensity Mapping. The materials science necessitated by these cosmological observations has catalyzed innovation in dark matter detection and quantum computing. I will go over how exploring new materials, such as Hafnium, for the CMB sensors revealed exceptional properties of some superconducting metals for dark matter MKIDs and, subsequently, for novel superconducting qubit sensors. Similarly, our work on Aluminum-coupled Tungsten TESs for dark matter led to a collaboration with UC Berkeley and the Molecular Foundry to engineer large-grain aluminum—a material advancement that now holds tremendous promise for improving both dark matter sensors and qubit architectures. By exploring these interconnected pathways, this talk will illustrate the rich feedback loop between astrophysics, particle physics, and quantum science, demonstrating how detectors built to look at the sky simultaneously push the boundaries of quantum technology.

Optical interferometer observatories such as LIGO have begun a new era of astrophysics by measuring the length of their vast arms to such precision that gravitational waves from distant collisions of black holes and neutron stars are now regularly observed. This past run, the global gravitational wave network itself entered a new era, whereby every detector has enhanced sensitivity using quantum squeezed states of light, limited by measurement back-action and optical loss. In its latest observing run, LIGO is now operating with its advanced, "Frequency-dependent squeezing" upgrade to now surpass two limitations to its quantum-limited sensitivity. Given the proven and maturing effectiveness of squeezing, we should now explore what are future avenues to utilize quantum mechanics to improve Gravitational-Wave observatories, interferometers, and physics experiments in general. This talk will outline the information theoretic basis of squeezing's effectiveness, it's fundamental limitations, and outline how emerging technologies such as atomic quantum memories can implement alternate non-Gaussian quantum enhancements that surpass squeezing for certain astrophysics and fundamental physics science goals.

Cryogenic solid-state detectors on the gram to kilogram scale, with very low energy thresholds and precise energy resolution, are among the most promising technologies for multiple types of rare event searches -- including low-mass DM direct detection, CEvNS, and neutrinoless double beta decay. I will introduce three such R&D projects currently underway in the University of Toronto astroparticle physics research group. The first, HONEYCOMB, will conduct DM searches and CEvNS studies using arrays of gram-sized Ge crystals with Transition Edge Sensors (TESs) on their faces, essentially scaling up the "HVeV" (High Voltage eV-resolution") technology of SuperCDMS prototypes. The second, LiMo, will employ TESs on wafers of lithium molybdate to search for 0vBB events in the isotope Mo-100. The third will pair anisotropic scintillators, in the form of crystals of organic molecules such as stillbene, with Charge Coupled Devices for "directional" DM searches probing below the neutrino fog.

Spectroscopy at millimeter wavelengths is sensitive to far-infrared emission lines from high-redshift dusty galaxies that are often optically faint. Next-generation surveys have the potential to push measurements of large-scale structure to the first billion years of the universe, providing unprecedented constraints on the physics of inflation, dark energy, and dark matter. Recent advances in superconducting millimeter-wave detector technology have enabled an order-of-magnitude decrease in spectrometer size, and we can now envision large arrays of spectrometers-on-a-chip with the sensitivity for these science goals. I will review the state of the field and present SPT-SLIM and SuperSpec, on-chip filter-bank spectrometers using kinetic inductance detectors which both saw first light in 2025. I will discuss our understanding of device performance on sky and future steps towards large, background-limited arrays that could constrain cosmological physics beyond the reach of optical galaxy surveys.

Magnons, the quanta of collective spin excitations in magnetically ordered media, has been recently predicted to interact with axion dark matter via spin-dependent dark matter coupling to electron spins. This requires magnon quantum detection for detecting incoming low-energy dark matter. The first approach is to couple magnons to a 3D cavity, and use quantum-limit amplifiers to readout single microwave photons from the cavity. The second approach is to use magnon-qubit entanglement and perform quantum non-demolition (QNL) readout of magnon states. This talk will discuss the general idea of magnon quantum sensing using cavity magnonics and compare the two different approaches. In particular, we will focus on the second approach and propose a circuit-scalable on-chip quantum magnonic platform for dark matter detection [1]. The architecture is based on our recently developed superconducting cavity magnonic circuit system [2], which allows for coherent control of magnons with state-of-the-art coherence time and phase coherence in real time [3]. We will discuss the fundamental limit in QNL magnon quantum detection and the potential solutions, such as increasing the target mass, circuit multiplexing, and dark-count reduction ideas.

References

[1] Clarence Chang, et al. ""Searching for axion dark matter with array-scalable single magnon detectors"" Phys. Rev. D 113, 015016 (2026)

[2] Yi Li, et al. ""Coherent coupling of two remote magnonic resonators mediated by superconducting circuits"" Phys. Rev. Lett. 128, 047701 (2022)

[3] Moojune Song, et al. Single-shot magnon interference in a magnon-superconducting-resonator hybrid circuit, Nature Communi. 16, 3649 (2025)

Kinetic Inductance Detectors have emerged as a cornerstone technology for next-generation physics experiments. With high multiplexing factors enabled by superconducting microresonators, large arrays resolve photon energy and arrival-time. The presentation highlights how these advancements drive major scientific frontiers in physics. First, for the PRIMA (PRobe far-Infrared Mission for Astrophysics) concept, ultra-sensitive arrays probe the obscured universe. High-throughput far-infrared spectroscopy will trace early cosmic dust and galaxy evolution. Second, for the LIFE (Large Interferometer for Exoplanets) mission, high-dynamic-range photon counting enables advanced nulling interferometry. This interferometer architecture allows direct characterization of terrestrial exoplanet atmospheres. Third, the discussion covers how THz KIDs empower the innovative QUALIPHIDE (QUAntum LImited PHotons In the Dark Experiment) for dark matter searches. Finally, the presentation highlights newer kinetic inductance enabled quantum sensing projects at JPL and Caltech.

A wide number of physics and cosmology applications are demanding greater and greater numbers of low temperature superconductor-based sensors.  However, scaling up the sensor count is often a significant challenge given the practical realities of cryogenics, complexity, and cost.  In this talk, I will give an overview of a key scaling technology which is often the principal limiter - multiplexed sensor readout – with a focus on some of the most common energy- and power-resolving superconducting sensors (TESs, MKIDs, and MMCs).  I will highlight some recent advances and successes in mm-wave cosmology, where we have recently fielded 105 background-limited sensors and achieved multiplexing factors above 103.  I will also describe ongoing R&D in our group to adapt highly multiplexed readout technology to phonon detectors for dark matter experiments.  Finally, I will briefly showcase a new simulation tool our group has developed to predict and optimize the cool-down time of large cryostats early in the design stage, an increasingly common concern as low temperature sensor arrays continue to grow in size.

Fermilab is actively developing and testing a novel digital Silicon Photomultiplier (dSiPM) tailored to cryogenic environments, a project being carried out in collaboration with EPFL and GlobalFoundries (GF) utilizing Single-Photon Avalanche Diodes (SPADs) implemented in the GF 55nm CMOS process. While the primary focus of this project is to support the next-generation Deep Underground Neutrino Experiment (DUNE) photon detector system, the architecture is highly versatile, making other applications possible. The monolithic design transitions away from conventional analog frameworks to achieve simple, low-cost, low-power photon counting at MSPS rates. Comprehensive testing of these integrated devices is currently ongoing and preliminary results will be presented. These results include the behavior of the SPAD breakdown voltage down to 60K and the distinctive temperature dependence of after-pulsing lifetimes between 87K and 165K. This initiative is taking place in the context of a wider research portfolio at Fermilab dedicated to advanced single-photon photodetectors of various types, including ultra-low-noise Skipper CCDs and SNSPDs.

Liquid xenon (LXe) time projection chambers (TPCs) are a leading technology for rare-event searches, including neutrinoless double-beta decay and dark matter experiments. Realizing the full potential of these detectors requires low-noise and low-power electronics capable of operating directly in the cryogenic environment. 

The CRYO ASIC was developed as a cryogenic-compatible readout solution for large-scale noble liquid detectors. Fabricated in 130 nm CMOS technology, CRYO is a highly integrated System-on-Chip that combines configurable front-end amplification and shaping, waveform digitization at up to 2 MSPS, and high-speed digital serialization.

This talk will present the design and performance of the CRYO ASIC, including characterization results obtained under cryogenic conditions and in liquid xenon. Measurements of noise, gain stability, and overall system performance will be discussed. Results for both ionization-charge readout and large-area silicon photomultiplier readout will be presented, demonstrating the versatility of the ASIC and its potential for next-generation liquid xenon detectors.

Photon to Digital Converters (3D-PDCs) are next-generation digital silicon photomultipliers (SiPMs) that vertically integrate a sensing layer of Single Photon Avalanche Diodes (SPADs) with a custom CMOS active quenching circuit and processing electronics. This design enables individual-SPAD control, reducing system noise and offering ~100 ps single-photon timing resolution. The 'fully digital' philosophy avoids the analog-to-digital conversions used in SiPMs, decreasing power consumption while supporting customizability. The project aims to be a drop-in replacement for SiPMs in a wide range of applications from quantum measurements to radiation detection, fundamental nuclear and high-energy physics, and medical devices. This talk will cover 3D-PDC design, current performance status, the outlook for future systems utilizing the device, and remaining R&D challenges.

Traditionally employed in digital cameras, pixelated CCD and CMOS sensors have evolved into powerful tools for fundamental physics. CCDs now provide world-leading sensitivity to sub-GeV dark matter, with the 104-CCD DAMIC-M experiment entering commissioning this year. Recent advances have enabled the identification of atomic recoils by the stimulation of crystal defects, opening new opportunities for dark matter and neutrino detection. Meanwhile, CMOS charge sensors offer unprecedented spatial resolution for imaging electrons in an amorphous selenium target, with applications ranging from searches for neutrinoless double-beta decay to hard X-ray detection. This talk will review the status and future prospects of these technologies in astroparticle and nuclear physics.

Astroparticle physics in the MeV regime, such as neutrinos produced by core-collapse supernovae and MeV-scale γ-rays, is rich and fascinating; however, owing to the difficulties of detection, it has barely been explored.  Liquid-argon time-projection chambers (LArTPCs) offer unique opportunities for physics in the MeV regime based on their millimeter resolution and potential on calorimetric capabilities, allowing reconstruction of both directionality and calorimetry for MeV-scale particles. The Deep Underground Neutrino Experiment (DUNE) places detection of supernova neutrinos as one of its primary physics goals with its LArTPC far detector, and a space-borne MeV γ-ray detector based on the LArTPC technology has been recently proposed by a SLAC group.

In this talk, I will discuss R&D projects optimized to MeV physics in LArTPCs, and its application in COHERENT, DUNE Phase II far detector, and GammaTPC in space.

Xenon and argon have historically been among the most successful target materials for dark matter searches using direct‑detection experiments in underground laboratories. Xenon benefits from its larger atomic size, while the lighter argon nucleus allows for larger recoil energies when struck by a GeV‑scale dark matter particle, particularly in experiments that measure charge, as in a dual-phase Time Projection Chamber (TPC), or nucleation. To extend dark matter searches further into the sub‑GeV mass range, xenon‑doped argon has emerged as an ideal target material. It has already been tested in ProtoDUNE, is currently under validation in the Scintillating Bubble Chamber experiment, and is a potential candidate for the DarkSide‑LowMass program. In this talk, we review the current challenges facing the xenon‑doped argon research program and discuss its potential impact on the dark matter and neutrino physics communities, if the technology is successfully scaled to multi‑tonne detectors.

The HydroX concept seeks to provide the LUX-ZEPLIN (LZ) experiment with sensitivity to sub-GeV dark matter by introducing light nuclei such as protons into the liquid xenon target. Unlike xenon nuclei, where sub-GeV dark matter scattering does not produce detectable signals, protons are kinematically well-matched targets and generate larger signal yields when stopped in liquid xenon. The challenge is loading hydrogen compounds into detectors like LZ without impacting their low backgrounds and high signal yields, factors that enable their sensitive searches. I will describe our measurements of the solubility of various gases in liquid xenon and the ongoing studies of simple hydrocarbons as candidates for the HydroX upgrade.

Liquid argon time projection chambers (LArTPCs) require extremely high argon purity because electronegative contaminants capture drifting electrons and degrade detector performance. Electron lifetime measurements are therefore essential for detector calibration and operation.

This talk will present purity monitor development and testing for the Deep Underground Neutrino Experiment (DUNE). Purity monitors are miniature TPCs that measure electron lifetime by comparing the charge emitted from an electron source with the charge collected after a known drift distance. Two complementary designs are being prepared for deployment in the DUNE far detectors. UV-illuminated gold photocathode purity monitors provides high-precision electron lifetime measurements, while bismuth-207 source purity monitors enable continuous operation without an external light-delivery system. Together, these devices provide both precise calibration measurements and continuous monitoring of liquid argon purity. The talk will also describe a dedicated liquid argon facility at UC Irvine that supports the DUNE purity monitor program through a high-flow argon recirculation and purification system.

Understanding detector response at low energies is essential for current and future rare-event searches, including dark matter and neutrino experiments. To support these efforts, the CALIX detector, a small dual-phase xenon time projection chamber (TPC) developed at UCLA, has been constructed to study and calibrate the microscopic processes governing electron-recoil signals in xenon TPCs.

In this talk, I will present the CALIX detector design and commissioning program, including photomultiplier tube (PMT) gain measurements at various operating voltages, optimization of detector operating conditions, liquid xenon filling and operation, xenon purity monitoring through electron-lifetime measurements using a Cs-137 calibration source, and the development of pulse-identification algorithms for scintillation (S1) and electroluminescence (S2) signals. Stable dual-phase operation has been achieved, and the detector is now successfully operating at UC San Diego, where it will be used to perform detailed studies of low-energy detector response in liquid xenon

Cosmic muons in a uniform magnetic field generate broadband radiation. Such events can potentially bring backgrounds to the axion dark matter searches. We simulate the muon tracks with GEANT4 in a cylindrical region of interest with an 8T solenoid magnetic field applied. We further develop an analytical estimation of the angular-frequency-differential synchrotron radiation power spectra in this work as the cosmic muons span a wide range of Lorentz factor γ and pitch angle α. We verify that the natural charged particles are not the dominant noise backgrounds for the current axion dark matter experiments on the μeV scale because of the high quality factor Q and fine energy resolution in the readout. However, without sufficient energy resolution in the detector readout, future broadband axion dark matter experiments might be vulnerable to the synchrotron radiation of these charged particles.

The QCD axion is a well-motivated solution to the strong CP problem and a candidate for the dark matter in the universe. The DMRadio suite of experiments uses a resonant, lumped-element design to search for low-mass axions below 1 μeV. Reaching the required sensitivity is primarily an R&D challenge, driving development of high-field DC magnets in multiple geometries, tunable high-Q resonators, and low-noise quantum sensors operating near—and ultimately beyond—the standard quantum limit (SQL). In this talk, I will present the design and commissioning of DMRadio-50L, the first stage of the program, and outline the hardware scaling and key technical milestones for next-generation detectors targeting GUT-scale axions.

As the LIGO detectors undergo hardware upgrades and continue to reach greater sensitivities, it becomes increasingly important to better understand how our existing approaches for noise mitigation and detector stabilization must evolve. I will overview of several projects currently underway in the Richardson lab toward this goal. We are developing machine learning-based tools to model and subtract transient seismic noise from the data, as well as computer vision-based algorithms capable of distinguishing transient noise artifacts from true astrophysical signals. In parallel, future gravitational-wave detectors must operate at significantly higher laser power, making precise correction of thermally-induced wavefront distortions critical for maintaining detector sensitivity. I will also discuss ongoing efforts toward the development of next-generation solutions such as FROSTI, designed to provide high-resolution, low-noise control of optical aberrations.

We present the Crystal Xenon Time Projection Chamber (CXe TPC), a novel particle detector technology as a proposed upgrade to existing LXe TPCs, or as a standalone next-generation particle detector. The dominant background in current LXe dark matter searches is beta decays from radon contamination, which has proven to be ubiquitous, long-lived, and soluble in liquid xenon. Foundational tests at the sub-kg scale have shown that CXe offers a factor 500x mitigation of Rn progeny, allowing for a dark matter search with neutrino interactions as the leading background, while preserving the benefits of LXe as a detection medium. CXe has other benefits as well, such as increased electron drift speed - which can reduce instrumental backgrounds and improve resolution of multiple scatters - and increased electron extraction into the vapor phase. This presentation will present the status of CXe particle detection and growth studies at the O(10) kg scale as well as prospects for future CXe applications.

Next generation kilotonne-scale underground LArTPCs provide a unique opportunity for broadband sensitivity for rare-event searches, imaging ionization signals with millimeter-scale granularity. This talk will highlight two complimentary approaches --- self-triggered zero-suppressed pixelated readout and fixed-trigger-window projective readout --- to achieve the same end: full acquisition of bonafide physics charge induction signals from the keV to GeV regime.

Particle collision data are traditionally processed through a sequence of event reconstruction steps, including charged-particle tracking, calorimeter clustering, and particle-flow reconstruction, to transform detector signals into physics objects suitable for analysis. Relatedly, there is growing interest in developing foundation models for high-energy physics: general-purpose models that learn transferable representations and can be adapted to a wide range of downstream tasks. In this talk, I will present an alternative approach based on supervised event reconstruction. Specifically, we use a machine-learning model trained for particle-flow reconstruction (MLPF) and investigate whether its learned latent particle representations transfer to downstream analysis tasks. By augmenting standard kinematic inputs with latent features learned during reconstruction, we achieve improvements over models trained using kinematic inputs alone. These results demonstrate that the latent representations learned during reconstruction encode essential physics information, suggesting a promising route toward building foundation models for collider physics.