Nikolai Oukhanski presented below 100 quanta sensitivity resonant PHEMT readout for quantum devices, and proposed to employ its for frequency domain multiplexing of Could Electron Bolometers (CEB) array by applying bias modulation technique. By using series connection of bolometers it is possible to realise voltage-, current-, and power- biasing mode for 10-40 channels (if resonant tank quality factor in the range of 200-1000) by means of one PHEMT amplifier, and one common biasing line (at the best case) for bolometers. In this case amplifier power consumption is in the range of 500 nW-1000 nW per one bolometer channel, and amplifier can be placed at the stable working temperature between 300 mK and 300 K (depending optimum read-out configuration and allowable power consumption).
Leonid Kuzmin suggested to choice a power-biasing mode as a most promising (and most simple in realisation) approach for the basic idea of Could Electron Bolometer. L. K. suggested to build and test (with participation of Michail Tarasov) one (and several) channel PHEMT readout system with CHALMERS made CEB, with further implementation of this technique for the CHALMERS CEB multiplexing in the frame of common project with CESR (Toulouse)-laboratory, represented in workshop by Damien Rambaud.
Damien Rambaud support this PHEMT CEB multiplexing idea and idea to collaborate CESR, CHALMERS, and IPHT in the frame of common project following after PLANK (probably ELISA or Research and Technology program leading by CNES (Space french agency)) for building of 10000 channel CEB multiplexed array for usable in future astronomical observation with balloons, satelites or telescopes. And CESR can to take oneself the front-end part of read-out, which is included generation of CEB ac-bias signals, demodulation of output signals from PHEMT amplifiers, and its inferencing.
SUMMARY
It is very promising to use resonant PHEMT readout technique for CEB frequency domain multiplexing.
IPHT, CESR, and CHALMERS will try to integrate the work to realise a bolometer array usable in future astronomical observation (balloons, satelites or telescopes).