The both field of view and sensitivity of a large radio telescope in MM band strongly depends on a number of independent receiver elements which give undistorted elements of a sky picture - pixels. Some ways also exist to expand the available focal zone in cross direction by using more narrow illumination angles and optimal turn of the plane from which the Secondary mirror may be illuminated but this would decrease aperture efficiency almost twice. Power aberration curves for Schmidt and Zenith modes are shown in Fig.1. Full identity of characteristics for MMIC LNAs made from one wafer. Cascaded MMIC LNAs do not require additional isolation.
Human factor is excluded in LNA performance and tuning.
It is cost effective alternative to hybrid assemblies. Very high technological and cost efficiency. The same factor 2-3 is lose in a bandwidth for dipole microstrip radiators but it is a rather difficult task to realize an effective high sensitive reception in the whole waveguide bandwidth even for a single horn not for an array. The input of each array element corresponds to a separate radiation pattern. We use Rogers Corp. ceramic filled composite materials with loss tangent 0.0013 and constant 3.02 for the dielectric substrate.