Demonstrating Large Low Noise Transition Edge Sensor Arrays for Future FIR Space Missions

The 2020 Decadal report explicitly recommends two potential FIR missions. One of those will be a competed FIR Probe that, according to the report, could be launched as early as 2030. This probe mission requires a very fast and focused detector development program to mature current detector technologies that potentially can meet the sensitivity and pixel number requirements of such a mission- from currently TRL level 3 to level 6 not later than in 2025. It is evident that it is mandatory for the technology development for such a mission to begin now rather than only once the mission formulation has begun. While not yet defined, the detector requirements for the Probe mission can be expected to be close to the parameters required for the FIR Probe GEP, which is the FIR Probe proposed to the Decadal survey. In terms of detector noise requirements, this translates into detector NEPs just below 10^-18 W/sqrt(Hz) for the low spectral resolution imaging instrument GEP-I. In terms of pixel numbers, both GEP instruments require a few times 10^4 pixels, but with individual detector arrays with ~1,400 pixels each for GPI-I, and ~ 6,000 pixels each for GPI-S. Here we propose to build and demonstrate tileable individual kilopixel arrays with an architecture that can meet the few 10^4 pixel requirements for both GEP instruments, and which can meet the noise requirements for GEP-I with slightly modified optical parameters. These arrays will be based on an architecture we have developed and demonstrated in a prior SAT. The architecture demonstrated there is optimized for the use of the latest 2-D time domain SQUID multiplexers developed and produced at NIST, together with a high density fanout scheme developed by our team for a separate SAT. The noise requirements will be achieved by using a pixel design our group has successfully developed and demonstrated for the HIRMES Transition Edge Sensor (TES) based high resolution spectrometer arrays, but with a potential minor reduction of the transition temperature Tc that will be be enabled by the available cooling power provided by space certified ADRs, such as the one flown on HITOMI. Our array design will also be compatible with future lower NEP TES designs that are currently investigated by members of this team and other groups. In summary, we propose to use a combination of an already demonstrated array architecture with an existing TES pixel design plus high-density readout schemes designed to read out those arrays with 2-D SQUID multiplexers designed by NIST. This will be an end-to-end demonstration of large TES-based arrays capable of meeting the requirements for the low spectral resolution imaging instrument of the FIR probe mission GEP, which can be considered as a template for the actual low-resolution instrument expected to be proposed for a future FIR probe, which is called for in the Decadal report.

The Strategic Astrophysics Technology program (SAT) supports focused development efforts for key technologies to the point at which they are ready to feed into major missions in the three science themes of the Astrophysics Division: Exoplanet Exploration, Cosmic Origins, and the Physics of the Cosmos. This program is specifically designed to address middle technology readiness level (TRL) "gaps" between levels 3 and 6: the maturation of technologies that have been established as feasible, but which are not yet sufficiently mature to incorporate into flight missions without introducing an unacceptable level of risk. NASA does not require a data management plan for proposals to SAT.

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