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Direct spectroscopic biosignature characterization (hereafter "biosignaturecharacterization") will be a major focus for future space observatoriesequipped with coronagraphs or starshades. Our aim in this article is to providean introduction to potential detector and cooling technologies for biosignaturecharacterization. We begin by reviewing the needs. These include nearlynoiseless photon detection at flux levels as low as$<0.001~\textrm{photons}~s^{-1}~\textrm{pixel}^{-1}$ in the visible andnear-IR. We then discuss potential areas for further testing and/or developmentto meet these needs using non-cryogenic detectors (EMCCD, HgCdTe array, HgCdTeAPD array), and cryogenic single photon detectors (MKID arrays and TESmicrocalorimeter arrays). Non-cryogenic detectors are compatible with thepassive cooling that is strongly preferred by coronagraphic missions, but wouldadd non-negligible noise. Cryogenic detectors would require active cooling, butin return deliver nearly quantum limited performance. Based on the flightdynamics of past NASA missions, we discuss reasonable vibration expectationsfor a large UV-Optical-IR space telescope (LUVOIR) and preliminary coolingconcepts that could potentially fit into a vibration budget without being thelargest element. We believe that a cooler that meets the stringent vibrationneeds of a LUVOIR is also likely to meet those of a starshade-based HabitableExoplanet Imaging Mission.

Detectors and cooling technology for direct spectroscopic biosignature characterization