In 1957 July the two-dimensional intensity distribution of radio emission over the solar disk was determined at 3.2- and 10-cm wavelengths. The observations were carried out on the radio telescope 31 m in diameter at the Crimean Radio Astronomical Station of the Physical Institute of the Academy of Sciences of the U.S.S.R. The radio telescope was an immovable parabolic reflector with the axis set in the meridian plane on 22-degrees declination [1]. Scanning the pattern of the radio telescope in the declination range ±32 minutes of arc to obtain the intensity distribution was done by setting the feed and preamplifier on a movable carriage reciprocating near the focal plane. In combination with the sun's daily movement it provided the two-dimensional solar distribution along a zigzag line. These sections gave the radio picture.