With a 10 m large diameter the parabolic antenna reflector gives a theoretical gain of 40 dB on 1,4 GHz band. The parabola prime focus is located 5 metre distant from the grid reflector. The source cavity is handled by a mast boom and holding a dipole that is the receiving part of the antenna. Signals captured by the dipole are first amplified by a transistor MOSFET preamplifier that is at least 33 years old as it has been put there when the telescope was built. This preamplifier characteristics are the best that could be achieved in the 1980’s. For the present time we have no original document about it but we have been given a copy of a paper where it was described to have a 1.5 dB noise factor and a system temperature of 150° K. Then a 15 m long coaxial cable connects the preamplifier to an SDR receiver. Despite this cable is a low loss one, a certain level of signals could be lost and some noise added due to the length of the cable. Recently we have been extremely surprised that when applying 12-15 V to the coaxial cable via a Bias-Tee did awake the old preamplifier after 33 years ! Using a RIGOL DSA815 9KHz-1.5GHz spectrum analyzer we estimated the preamplifier gain at 1400 MHz to be around 20 dB.
It was necessary to add another preamplifier 15 m from the source in front of the SDR. (it is a KU LNA 133BH). Its characteristics are displayed on next figure (+28 dB and 0.6 dB noise factor around 1420 MHz).
Intrinsic preamplifier noise factor, important for overall radiotelescope receiving performances is displayed on the left scale. Gain is given on the right scale.
The first MOSFET preamplifier will be soon replaced by a better one dedicated to radioastronomy. HP LNA with CAVITY BAND PASS FILTER. Specifications: The filter section, will give the observer better selectivity (High Q) and will ward off some types of annoying interference, such as radar. The filter will pass the 1420 MHz signal and effectively attenuate unwanted signals. The LNA, N/F of 0.29 +/- 0.15 dB, gain of 35 dB +/- 3 dB. With N male connector.