Cosmic microwave background (CMB) measurements are fundamentally limited by photon statistics. Therefore, ground-based CMB observatories have been increasing the number of detectors that are simultaneously observing the sky. Thanks to the advent of monolithically fabricated transition edge sensor (TES) arrays, the number of on-sky detectors has been increasing exponentially for over a decade. The next-generation experiment CMB-S4 will increase this detector count by more than an order of magnitude from the current state-of-the-art to 500,000. The readout of such a huge number of exquisitely precise sub-Kelvin sensors is feasible using an existing technology: frequency-domain multiplexing (fMux). To further optimize this system and reduce complexity and cost, we have recently made significant advances including the elimination of 4 K electronics, a massive decrease of parasitic in-series impedances, and a significant increase in multiplexing factor.
MotivationTransition edge sensors (TES) are a mature and extremely successful technology for calorimetric and bolometric measurements. Their low operating temperature (0.01 − 0.5 K), low (0.01 − 2 Ω) impedance, and stringent noise requirement ( 10 pA/ √ Hz) calls for a sophisticated multi-stage readout system. As the per-experiment number of detectors starts to approach O(10 6 ), 1 a highly multiplexed, simple to assemble, and cost-effective solution is required.Digital frequency-domain multiplexing 2,3 uses an LC resonator in series with each TES detector to select a frequency at which a voltage bias is applied. This voltage bias keeps the