We use Rogers Corp. ceramic filled composite materials with loss tangent 0.0013 and constant 3.02 for the dielectric substrate. Input mutual radiator isolation is provided at -20 dB level. Super low noise HP Schottky square low detectors complete VHF parts. Output mutual channel isolation is provided at -70 dB level. One loaded LMA-422 is used as a noise oscillator for a communal input channel calibration.
Noise injection is produced through special radiators fed by a distributing microstrip line.
We hope to reach a factor 2 in sensitivity in this mode. Another exciting possible field of applications for multi-pixel MMIC reception at radio telescopes is millimeter wave antenna technologies including holographic antenna measurement techniques. MMIC receiving systems may be used to get moment holographic surface maps with a high resolution on strong cosmic or beacon satellite sources that gives a chance to correct surface errors practically in real time. It may give a powerful impulse to develop an active and adaptive optics technique at radio telescopes including wave front correction but requires at least one more order in MMIC cost reduction. This seems possible to build 500-1000 beam MMIC focal array for the radio telescope in the nearest future.