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Receiver Systems
Alex Dunning
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The Basic Structure of a typical Radio Telescope
CSIRO. Receiver Systems for Radio Astronomy
Receiver
Conversion
Digitiser
Signal Processing / Correlator
Captures and amplifies the incoming radiation
Filters and reduces the frequency of the microwave signal
Converts the analog signal to a digital bit stream
Divides signal into frequency bins and forms correlation products between
signals
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They are much the same
CSIRO. Receiver Systems for Radio Astronomy
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Radiotelescope Receivers
CSIRO. Receiver Systems for Radio Astronomy
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The Receiver
CSIRO. Receiver Systems for Radio Astronomy
On the outside...
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The Receiver
CSIRO. Receiver Systems for Radio Astronomy
On the inside...
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The Australia Telescope Receivers
CSIRO. Receiver Systems for Radio Astronomy
10
cm-2
5cm
12
mm
-18
.7m
m
6m
m-1
0m
m
O2
ab
sorp
tion
2.8
mm
-3.5
mm
4.6
cm-6
.7cm
3.2c
m-3
.7cm
2.5
cm-7
cm
Future upgrade
L/SC/X
K Q W
1:1.25 bandwidth1:1.65 bandwidth1:2.5 bandwidth
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Where do they go?
CSIRO. Receiver Systems for Radio Astronomy
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CSIRO. Receiver Systems for Radio Astronomy
At the focus of course
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Waveguides
CSIRO. Receiver Systems for Radio Astronomy
• Replace cables at high frequencies
• Operate like optical fibres for microwaves
• Only work over a limited frequency range
• Can support signals with two polarisations
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Receiving the signal – Feed horns
CSIRO. Receiver Systems for Radio Astronomy
Feed
Signal
Waveguide output
Captures the focused microwaves into a waveguide output
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Feed Horns
CSIRO. Receiver Systems for Radio Astronomy
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Coupling noise into the System
CSIRO. Receiver Systems for Radio Astronomy
Feed
Signal
Noise source
Coupler
7mm waveguide coupler
Noise coupled in through
small holes
Noise coupled in through vane
21cm waveguide coupler 12mm noise source
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Separating Polarisations – Orthomode Transducers (OMTs)
CSIRO. Receiver Systems for Radio Astronomy
PolariserFeed
Signal
Noise source
Coupler
Pol B
Pol A
Separates incoming signal into two linear or circular polarisations
Linear OMTs are more effective over broad frequency bands (usually)
12mm Orthomode transducer
4cm Orthomode transducer
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Separating Polarisations – Orthomode Transducers (OMTs)
CSIRO. Receiver Systems for Radio Astronomy
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Low Noise Amplifiers (LNA)
CSIRO. Receiver Systems for Radio Astronomy
PolariserFeed
Signal
Noise source
Coupler LNA
LNA
To conversion System
Pol B
Pol A
High Electron Mobility Transistor
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CSIRO. Receiver Systems for Radio Astronomy
….so though receiver topologies can be quite varied I am saying that this is a pretty typical structure of our receivers
…………and the 3/7/12 mm systems reflect this.
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CSIRO. Receiver Systems for Radio Astronomy
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What is the rest of the stuff?
CSIRO. Receiver Systems for Radio Astronomy
What’s this?
What’s this?
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Electronics
CSIRO. Receiver Systems for Radio Astronomy
• Supplies and monitors all amplifier voltages and currents
• Monitors system temperatures and pressures
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Cryogenics
CSIRO. Receiver Systems for Radio Astronomy
15K section
80K section
Helium Lines
Helium Compressor
Helium Refrigerator
Refrigerator in the Parkes 12mm receiver
Cold finger
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CSIRO. Receiver Systems for Radio Astronomy
Copper Radiation Shield 80K
Helium Refrigerator cold
finger
Vacuum Dewar
Thermal Isolation waveguide
15K section
Low Noise Amplifiers
Gap
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CSIRO. Receiver Systems for Radio Astronomy
….but why do we need to cool our receivers at all?
…………well first
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How weak is the signal?
CSIRO. Receiver Systems for Radio Astronomy
Your Hand → 1.38× 10-23 W Hz-1K-1 × 300K × 2 × 109 Hz
= 8 × 10-12 W
10Jy radio source → 10 × 10-26 W m-2Hz-1 × 300m2 × 2 × 109 Hz
= 6 × 10-14 W
Mobile Phone → ≈ 1W
Mobile Phone on the moon→ ≈ 1W ÷ 4π (3.8×108m)2 ÷ 5×106Hz≈ 10Jy
Effective area of an Australia telescope dish
Bandwidth of an Australia telescope digitiser
Boltzmann's constant
Lunar Distance
3G transmit bandwidth
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Like your hand all the components in the receiver system contribute a thermal noise signal which masks the astronomical signal we are trying to observe
By cooling the receiver we reduce these thermal sources of noise and improve the sensitivity of the receiver by 7-10 times
CSIRO. Receiver Systems for Radio Astronomy
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Reduce noise by cooling
CSIRO. Receiver Systems for Radio Astronomy
Electronic device
generates a signal
Cold stuff (liquid nitrogen)
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The Conversion System
CSIRO. Receiver Systems for Radio Astronomy
Contains:• more amplification• band defining filters• frequency conversion• level adjustment• signal detection• band shaping
Frequency Convertion
Signal
Filter
To Digitiser
AmplifierLevel
Adjustment
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Filters
CSIRO. Receiver Systems for Radio Astronomy
High Pass Filter Low Pass Filter Band Pass Filter
21cm band filter
Slow roll off where possible so you can push the band edges
Hard roll off where necessary to stop strong interference
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Mixing it down – Frequency Conversion
CSIRO. Receiver Systems for Radio Astronomy
Signal 1
Signal 2
Signal 1 × Signal 2
Mixer (Multiplier)
Frequency
Pow
er
Frequency
Pow
er
cos(ω1t)cos(ω2t)=½[cos((ω1+ω2)t)+ cos((ω1-ω2)t)]
Δf Δf
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Mixing it down – Frequency Conversion
CSIRO. Receiver Systems for Radio Astronomy
Signal 1
Signal 2
Mixer (Multiplier)
Frequency
Pow
er
Frequency
Pow
er
cos(ω1t)cos(ω2t)=½[cos((ω1+ω2)t)+ cos((ω1-ω2)t)]
Δf Δf
Low pass filter
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Mixing it down – Frequency Conversion
CSIRO. Receiver Systems for Radio Astronomy
Signal 1
Mixer (Multiplier)
Frequency
Pow
er
Frequency
Pow
er
Δf Δf
Local Oscillator
flo
cos(ω1t)cos(ωLOt) → ½cos[(ω1-ωLO)t]
Upper Side Band (USB)
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Mixing it down – Frequency Conversion
CSIRO. Receiver Systems for Radio Astronomy
Signal 1
Mixer (Multiplier)
Frequency
Pow
er
Frequency
Pow
er
Δf Δf
Local Oscillator
flo
cos(ω1t)cos(ωLOt) → ½cos[(ωLO-ω1)t]
Lower Side Band (LSB)
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Mixing it down – Frequency Conversion
CSIRO. Receiver Systems for Radio Astronomy
Signal 1
Mixer (Multiplier)
Frequency
Pow
er
Frequency
Pow
er
Δf Δf
Local Oscillator
flo
Band pass filter
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Single Sideband Mixers
CSIRO. Receiver Systems for Radio Astronomy
Signal
2√2cos(ω1t)
2cos(ω1t)
2sin(ω1t)sin[(ω1- ωLO)t] (USB)-sin[(ωLO- ω1)t] (LSB)
cos[(ω1- ωLO)t] (USB)cos[(ωLO- ω1)t] (LSB)
-cos[(ω1- ωLO)t] (USB)cos[(ωLO- ω1)t] (LSB)
0 (USB) √2cos[(ω1- ωLO)t] (LSB)
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Single Sideband Mixers
CSIRO. Receiver Systems for Radio Astronomy
Signal
2√2cos(ω1t) √2cos[(ωLO- ω1)t] (USB) 0 (LSB)
SignalLocal Oscillator
Lower sideband
Upper sideband
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Attenuators – The Volume Knob
CSIRO. Receiver Systems for Radio Astronomy
• Allow the signal level to be varied
• May be several in the system• Usually set automatically
Just like some other systems if you turn the signal down too far all you get is noise and if you turn it up to far you get distortion!
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CSIRO. Receiver Systems for Radio Astronomy
Of course real systems are a little more complicated.....
They usually contain multiple conversions and many amplification and filter stages....
But that’s the gist of it.
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Things to remember
CSIRO. Receiver Systems for Radio Astronomy
• Sometimes local oscillators leak if you look deep enough you might find one!
• Single sideband mixers can result in signals turning up at the wrong frequency, albeit at a very low level.
• Make sure your attenuators are set right. Too high and the system noise increases. Too low and you may distort your signal.
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Contact UsPhone: 1300 363 400 or +61 3 9545 2176
Email: [email protected] Web: www.csiro.au
Thank you
CSIRO Astronomy and Space ScienceAlex DunningRF Engineer
Phone: 02 9372 4346Email: [email protected]: www.csiro.au/org/CASS