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