This page describes the backends available for passive radio astronomy observations. Back-ends for the planetary radar and for the atmospheric science instruments are not described here.
PUPPI – The Puerto Rico Ultimate Pulsar Processing Instrument, for single-pixel pulsar observations.
The Mock Spectrometers for spectral line and pulsar observing using the full 300-MHz bandwidth of ALFA and
- single-pixel observing with 7 × 164-MHz boards or 14 boards with a bandwidth of 82 MHz or less in 7 independently steerable groups.
The WAPP Correlators for pulsar and spectral line observations giving 100-MHz chunks of the full bandwidth of ALFA.
- Allows 4 boards of up to 100-MHz each in single-board mode and 8 boards of up to 100-MHz each in dual-board mode for single-pixel observing. (Note: there are 4 WAPP machines: ‘single-board’ and ‘dual-board’ refer to the number of boards employed per machine.)
- Pulsar capabilities are described here
The GALFA Spectrometers – for Galactic HI observations with ALFA.
The Mark5A and Mark5C – backends for VLBI observations.
The Interim Correlator – an older single-pixel backend providing 4 boards with up-to 50-MHz bandwidth each.
Continuum Observing with the Radar Interface – it is normally recommended that for continuum observations one of the spectral-line backends is used. However, this system is used to provide a continuum total-power record for VLBI observations.