Field Trials of an RFI Adaptive Filter for Pulsar Observations M. Kesteven, R.N. Manchester, G. Hampson & A. Brown Australia Telescope National Facility

Field Trials of an RFI Adaptive Filter for Pulsar Observations

M. Kesteven, R.N. Manchester, G. Hampson & A. Brown

Australia Telescope National Facility

Groningen, 28 March 2010

RFI mitigation. Groningen, 2010

Outline

• Introduction

• Adaptive Filter details

• Results

• Conclusions


Introduction

• The RFI mitigation work at the Parkes Observatory was given greater emphasis when one of the Parkes Pulsar observing bands became heavily polluted with RFI (digital TV).

• The prospects were favourable:• The levels were substantial, but not so large as to overload the

system.

• Some of the critical hardware needed was already in place.

• A new digital backend with reserve capacity came on-line.

• An adaptive filter works well with pulsar observing.


Introduction (II)

• The Parkes Observatory recently commissioned a new pulsar processing machine. This a digital polyphase filterbank that is capable of 8-bit sampling at a rate of 2GHz for an observational bandwidth of up to 1GHz. It supports a range of configurations including an online-folding mode with up to 2048 pulse phase and radio frequency bins.

• For observations in the 50cm (~700 MHz) band there is spare capacity which could readily be deployed for RFI mitigation.

• This takes the form of an adaptive filter in conjunction with a reference antenna directed towards a TV tower, the source of RFI for the receiver’s band.


The basic narrow-band adaptive filter


Filter details

)1(

1.

.

2

2

64

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64646464

INRnattenuatiofilter

INR

gainfilter

VVV

VVVV

sysref

rfiref

ref

rfiref

rfim

V

V

P

VV

sysref

rfirefref

sysm

rfim

astmm

= residual RFI / unfiltered RFI


The broad band filter, as implemented


PDFB3: Real-time RFI Mitigation

Filter outputRef ant

RFI Mitigation Off

Cross-Correlation

• Reference antenna pointed at RFI source

• 2048 channels across band

• Signal*reference cross-correlation subtracted from data

• Filter updates at 1ms intervals to follow tropospheric multi-path propagation

• Single reference can be applied to both polarisations of telescope signal

• Main application (so far): Digital TV signals in 50cm band

• 4-m reference antenna pointed toward Mt Ulandra, 200 km south of Parkes

RFI Mitigation On!

64 MHz at 50 cm (655 – 717 MHz)


PSR J0437-4715 at 50cm

RFI Mitigation Off

RFI Mitigation On

S/N ~ 1040 in 4 min

S/N ~ 1710!

• Pulsar signal under RFI is recovered with no (evident) perturbation

• Improvement in S/N will be greater with weaker pulsars

• Expect to apply to regular 50cm observations with APSR soon

Stokes I


Filter OFF Filter ON


(operational details)


Operational details

dtVVgg ref

t

t

filtnn*

1

1

determines the speed of the filter in responding to changing conditions. In effect it sets the rate at which gn converges on the optimum setting. A value of[0.1/(mean IF power)] works well for us

needs to be smaller than time scale of the changing conditions in the propagation path. We use 1 msec.

The filter gain is computed as :

Propagation Issues - movie


How well does the filter work?

1. Compare the observed and predicted attenuation of the RFI at the filter output.

There is a good match – the filter is working as designed.

2. Relate the residual RFI to the science requirements:

The rms in the pulse /phase plot has dropped to close to the rms of the RFI-free condition. The residual RFI after filtering is less than 10% of the receiver bandpass.

3. The pulse shape is not affected by the filter, neither inside nor outside the bands affected by RFI.


Filter performance (1)

RFI at the filter output

RED : filter OFF BLUE : filter ONBLACK : 10% of the receiver bandpass

RFI in the reference antenna


Filter performance(2) : the RFI attenuation

RED : the measured attenuationBLUE : the attenuation predicted from the INR in each channel

Adaptive Filter Performance (1)

Adopting the RA-769 criteria we can estimate the limitations of the adaptive filter.

1. The ratio of the RFI powers in the main and reference antennas is given by :

= (Area of 0 dBi antenna) / (Area of the reference antenna)

= (R)2 [= 0.0016 at 600 MHz, 4m ref antenna]

2. The residual power (due to the RFI) in the filtered output :

resid = * Tsys * INR / (1 + INR)

3. resid tends to *Tsys for large INR. (~0.0016*Tsys)

4. The filter starts to fade out at INR ~ 1, with resid ~ *Tsys/2

5. Thereafter resid falls gracefully to 0 as the INR decreases.

NOTE : Tsys is the system temperature of the reference antenna


Current Status

• The filter is embedded in the pulsar processor, and is available for on-line operations.

• However, the receiver has been tuned to a new frequency –

Planned nearby transmitters would violate the linearity requirements, so for continuity in the pulsar timing, prudence dictated a re-tune.

• We still have RFI to contend with, from a different direction, and with less RFI.


New 50 cm environment : Peak Hill

WHITE: Unfiltered RED: Reference


Peak Hill: unfiltered filtered

Conclusions

0. The filter works well.

1. The filter meets RA.769 in that the residual RFI is below the 10%Tsys.

2. It would satisfy RA.769 for VLBI, and for most pulsar work.

3. It is not so clear for a pulsar blind search mode : low frequency modulation in the range 1 ms to 5 sec could compromise the period search machine.

4. It would probably not work for spectroscopy.


Contact UsPhone: 1300 363 400 or +61 3 9545 2176

Email: [email protected] Web: www.csiro.au

Thank you

Australia Telescope National FacilityMichael Kesteven

Phone: 61 2 9372 4544Email: [email protected]: www.csiro.au/group

Documents

Field Trials of an RFI Adaptive Filter for Pulsar Observations M. Kesteven, R.N. Manchester, G. Hampson & A. Brown Australia Telescope National Facility