Backends

Astronomy


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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.


The Wapp Correlators

The WAPP Correlators for pulsar and spectral line observations giving 100-MHz chunks of the full bandwidth of ALFA.

  • Also 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 Mock Spectrometers

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.


Puppi

The Puerto Rico Ultimate Pulsar Processing Instrument, for single-pixel pulsar observations.


GALFA Spectrometers

GALFA Spectrometers – for Galactic HI observations with ALFA


Mark5A & Mark5C

The Mark5A and Mark5C – backends for VLBI observations.


Interim Correlator

The Interim Correlator – an older single-pixel backend providing 4 boards with up-to 50 MHz bandwidth each.


Continuum Observing

Continuum Observing with the Radar Interface – it is normally recommended that for continuum observations one of the spectral-line backends is used. This system is used to provide a continuum total-power record for VLBI observations.