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Post-Correlation Interference Mitigation. M. Kesteven & R. Sault Australia Telescope National Facility [email protected] IUCAF – Bonn, March, 2001. Post-Correlation RFI excision. Overview of the scheme Application 1 - Single Dish Application 2 - Synthesis Array Problems/Limitations

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post correlation interference mitigation

Post-Correlation Interference Mitigation

M. Kesteven & R. Sault

Australia Telescope National Facility

[email protected]

IUCAF – Bonn, March, 2001

post correlation rfi excision
Post-Correlation RFI excision
  • Overview of the scheme
  • Application 1 - Single Dish
  • Application 2 - Synthesis Array
  • Problems/Limitations
  • Comparison with Adaptive Filters
  • Parametric Filter - Glonass excision
features
Features
  • A Post-Correlation equivalent to an Adaptive Filter
  • Applicable to Single Dish observations
  • Applicable to Synthesis Array observations
  • Performance comparable to the Adaptive Filter
  • Can be implemented with current hardware
slide6

Single Dish - Autocorrelation

Reference antenna

Parkes 64m

post correlation features
Post-Correlation - Features
  • Tolerant to small number of sampler bits
  • Tolerant to multi-pathing interference
  • Tolerant to significant delays between the reference and the astronomy antenna
  • Tolerant to offset between the array tracking centre and the interference location
  • Only one reference antenna required even for an array filter
array notes
ARRAY - notes
  • Require one Reference Antenna + conversion chain
  • Require Additional Correlator resources. Equivalent to adding one extra antenna to the array.
  • Enjoys all the flexibility of the observatory correlator
  • Makes no assumption as to similarity between antennas of the array. Interference may enter via different sidelobes in different antennas.
  • The corrections are based on the correlator output – therefore works with few-bit samplers.
post correlation theory
Post-Correlation - Theory

The correction spectrum Vc(f) is given by:

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