"This animated gif shows observations of the Moon from MWA survey data taken at 72-103 MHz. The Moon is visible because it reflects radio waves from transmitters on Earth, including the FM radio band. The Moon can easily be seen progressing across the sky in individual snapshots taken about 10 minutes apart. Note that the Moon only reflects radio waves to Earth from its center (specular reflection) and that extragalactic sources close the Moon disappear as its disk occults them."
Credit: N. Hurley-Walker, N. Seymour
The MWA consists of 4096 dual-polarization dipole antennas optimized for the 70-300 MHz frequency range, arranged as "tiles", each a 4x4 array of dipoles. A complete technical description of the Phase I telescope is given in the journal article: The Murchison Widefield Array: The SKA Low Frequency Precursor by Tingay et al. (2013), and a Phase II description can be found in the article The Phase II Murchison Widefield Array: Design Overview by Wayth et al (2018).
The array has no moving parts, and all telescope functions including pointing are performed by electronic manipulation of dipole signals, each of which contains information from nearly four steradians of sky centered on the zenith. Each tile performs an analog beamforming operation, narrowing the field of view to a fully steerable 25 degrees at 150 MHz.
The majority of the tiles are scattered across a roughly 1.5 km core region, forming an array with very high imaging quality, and a field of view of several hundred square degrees at a resolution of several arcminutes. The remaining tiles are placed at locations outside the core, yielding baseline distances of up to 6km to allow higher angular resolution for solar burst measurements.