A Robust, Efficient Architecture to Produce Scalable, Superconducting Kilopixel Far-IR Detector Arrays

The far-infrared (FIR) band is uniquely suited to study the physical conditions in the interstellar medium and star formation out to the highest redshifts. Robust, high sensitivity detector arrays that operate over the entire FIR regime with up to several 10 4 pixels, large focal plane filling factors and compatibility with low noise detector designs and low cosmic ray cross sections, are required for future (F)IR missions, such as Origins . The arrays could consist of smaller sub-arrays, since they can be tiled. The GSFC-designed Backshort Under Grid (BUG) array architecture and its precursor architectures have been fielded in several FIR cameras, including GISMO at the IRAM 30 m telescope (the array used in this instrument was strictly speaking a precursor to the final BUG array) and HAWC + on SOFIA. The BUG array used in the latter instruments has an integrated termination board and SQUID readout multiplexer. The array was fabricated in collaboration between NASA/GSFC and NIST and meets these requirements. However, the BUG fabrication has many low throughput processing steps, with the consequence of long production times and sub-optimal yields. To meet the requirements for robustness and production efficiency for future arrays, we have developed, and by now partially demonstrated, a new architecture to provide the superconducting connection of transition edge sensor detectors to the readout multiplexers or readout boards behind the array. This approach will allow us to reach the goal to produce reliable, large low noise detector arrays for future space-based and suborbital instrumentation.