The front-end outputs are connected to the back-ends either by coaxial cables or optical fibers depending whether the back-end is located in the apparatus box (500 m away from the antenna) or within the radio telescope. For the first operations of the radio telescope, the following four back-ends designed for specific scientific activities are available at the site:
- Total power: this is formed by 14 voltage-tofrequency converters to digitize the detected signals. Different IF inputs can be selected from three focal points. The system can be adjusted to select different bandwidths (maximum bandwidth: 0.1 - 2.1 GHz) and to modify the attenuation level.
- Digital Filter Bank mark 3: this is a FX correlator developed by the Australia Telescope National Facility, allowing full-Stokes observations. It has four inputs with 1024 MHz maximum bandwidth each and 8-bit sampling for high dynamic range. The DFB3 is suitable for precise pulsar timing and search, spectral line and continuum observations with high time resolution. It allows up to 8192 spectral channels, to counter the effects of interstellar dispersion when it is operated in pulsar mode, and for power spectrum measurements in spectrometer mode
- Xarcos: this is a narrow band spectropolarimeter with 8x2 input channels. The working band is 135-240 MHz and the maximum number of spectral channels is 2x2048 per polarization, per output channel. The instantaneous bandwidth ranges between 0.488 and 62.5 MHz and the maximum effective spectral resolution is ~500 Hz.
- Digital Base Band Converter: this is a digital platform based on a flexible architecture, composed by four ADC boards 1 GHz bandwidth each and four Xilinx FPGA boards for data-processing. The platform is designed mainly for VLBI experiments; however, a wideband spectrometer has been developed for different purposes.