WP2.2 CoDR PAF introduction · 2011. 10. 24. · 4 K −2 deg 2 0.3 1.0 3.0 10.0 Frequency GHz 0.1...
Transcript of WP2.2 CoDR PAF introduction · 2011. 10. 24. · 4 K −2 deg 2 0.3 1.0 3.0 10.0 Frequency GHz 0.1...
AA-mid
Jan Geralt Bij de Vaate
Outline
• EMBRACE • AA-mid • PEP: AA verification systems
EMBRACE System Architecture
Pulsar Detection Setup
Dual Beam demonstration
EMBRACE@Nançay
EMBRACE@Nancay
Pulsar B0329+54
EMBRACE connected to ARTEMIS backend (courtesy U. Oxford)
See poster!
AA noise temp measurement
• APERTIF Front end • 50K noise temp
ORA
• New design • Will be tested with
EMBRACE beamformer
0.4 0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5-35
-30
-25
-20
-15
-10
-5
0
Frequency (GHz)R
efle
ctio
n co
effic
ient
(dB
)
Infinite arrayThe centre element for the finite ORA array tile
SKA2 Receptor Technologies
250 Dense Aperture Arrays 1-3000 Dishes
AA-low - 250 Arrays
3-Core Central Region
Artist renditions from Swinburne Astronomy Productions
SKA2 Receptor Technologies
250 Dense Aperture Arrays 1-3000 Dishes
AA-low - 250 Arrays
3-Core Central Region
Artist renditions from Swinburne Astronomy Productions
Science requirements
0
2,500
5,000
7,500
10,000
Sen
sitiv
ity A
eff/T
sys
m2
K−1
0.3 1.0 3.0 10.0
Frequency GHz
0.1 0.14 1.4
2. Resolving AGN and Star Formation in Galaxies
39,000 5. Wide Field Polarimetry - 2
11. Galaxy Evolution via H I Absorption
12. HI BAO
25,0000 3. Protoplanetary disks
20,0000 6. Continuum deep field
7. Deep HI Field
9. Galactic centre pulsars
10a, 13a. Pulsar search
10b, 13b. Pulsar timing
4. Cosmic Magnetism
8. HI EoR
Sensitivity Requirements
12,500
15,000
Specified sensitivity
Derived survey speed
5. Wide Field Polarimetry - 1
Huge....
ProposedDish Envelope3,000 @ 15m
ProposedAA system
envelope
1e2
1e4
1e6
1e8
1e10
Surv
ey S
peed
m4
K−2
deg2
0.3 1.0 3.0 10.0
Frequency GHz
0.1 0.14 1.4
5. Wide Field Polarimetry
11. Galaxy Ev. via HI Abs’n
7. Deep HI Field
4. Cosmic Magnetism8. HI EoR
Survey SpeedRequirements
1e1
Specified survey speed
Derived from sensitivity
ProposedDish Envelope3,000 @ 15m
ProposedAA system
envelope
13a. Pulsar search
1.4 GHz hydrogen line
Positioning AA-mid
Sky dominated
noise Receiver dominated noise1
10
100
1000
10000
0 200 400 600 800 1,000 1,200 1,400 1,600 1,800 2,000
Sky
Tem
pera
ture
, Tsk
y, K
Frequency MHz
Sky Noise TemperatureDense AA
Optimize in case AA-low requires two bands?
AA-mid station
• Station diameter 56m • Limited analogue beamforming • ~110.000 elements • Distributed or central processing
• Crucial:
– Calibration – Dynamic range – Cost /power
PEP AAVS-mid
• Part of AIP • Aperture Array Verification Systems
– AAVS0, small antenna test tiles – AAVS1, small test station (~100m2) – AAVS2, ~2000m2
– On the SKA site!
– Processing and site infrastructure to be shared with AA-low
AAVS2 AA-mid -> EMMA
• Science capable system
Parameter Conditions Value
Sensitivity Aeff/Tsys Broad sight 20 m2 / K
Number of ‘stations’ 14
Frequency range Instantaneous 450 – 1450MHz
Field-of-View (FoV) @ 1450 MHz 78 deg2
Scan range ±45°
Baseline <1km in 2D
Ilse van Bemmel
AAVS2 AA-mid -> EMMA
• Dual pol • Designed for SKA site
– RFI / Climate etc.
• Modular design • Low cost / Low power
Antenna development
Truncation simulations
Beam former design
¼ EMMA tile Combi board RF board
Tile in lab tests
Integrated Receiver
French National Funding Nançay (coordinator),Bordeaux, NXP, ASTRON Beamformer chip with time delay instead of phase
shifting for wide bandwidth System-in-Package:
ADC with Serializer LNA with filter
Goal AAmid tile with digital output Reduce power consumption, and
data transport/command complexity
Receiver design
• Ready for production Q1 2012
Down converter sub rack Down converter card Down converter Layout
Conclusion
• AA-mid has huge scientific benefits • Lots of electronics, but on the ICT development path • AA depend on high speed comms and processing • Upgradable • SKA2 is realistic
EMBRACE RFI mitigation 15th July 2011, local TV tower