PJ Hall, Sept 2007

ISPO

The Square Kilometre ArrayA Plain Person’s Guide

Peter HallInternational SKA Project Engineer, ISPO

MCCT-SKADS Training SchoolBologna, September 24, 2007

www.skatelescope.org

PJ Hall, Sept 2007

ISPO

Overview� Radio telescopes, new & old� Introduction to SKA & science case (brief)� SKA design space

– Sensors (antennas) and other systems

� “Reference Design” technology development– Some enabling technologies– Pathfinders and Design Studies

� SKA specifications – 2007� Siting – brief� Project timelines & management� The SKA Preparatory Phase initiative

– International engineering, procurement, …, studies– Bright people needed!

� SKA progress and directions

PJ Hall, Sept 2007

ISPO

Radio telescopes

PJ Hall, Sept 2007

ISPO

Some current radio telescopes

J. Sarkissian

Parkes

Australia Telescope Compact Array

Very Large Array

AreciboAbout 10,000 sqmetres effectivearea

PJ Hall, Sept 2007

ISPO

Radio astronomy basicsTelescope as radiometer:

∆S=2k ∆Tant / AeffFor radiometer, ∆T ~ Tsys/(Bτ)1/2

Then, ∆S=2k Tsys/ { (Bτ)1/2 Aeff }

�For small ∆S, need big Aeff/Tsys

Telescope FoM:

Single field science: Aeff/TsysSurvey science: (Aeff/Tsys)2 . FoV

Different telescope designs for different frequencies and applications

Tsys ~ Tantenna + Treceiver

PJ Hall, Sept 2007

ISPO

Not just dishes….

BSA - Pushchino

Nancay

Molonglo

CoRE

PJ Hall, Sept 2007

ISPO

Sensitivity of radio telescopes

SquareKilometreArray

PJ Hall, Sept 2007

ISPO

New radio telescopes

� Exploit convergence of radio and ICT – Parameter space + flexibility = discovery

� Less metal, more ICT– Gains achieved via functionality/cost improvements

» Ride the “consumer wave”» Re-use expensive area, do more with photons

� Pose many challenges– New players can be as effective as old in key areas

» Architecture optimization, calibration, …� Collectively chart course to SKA and beyond

- New science and technology at each stage- SKA and Pathfinders (LOFAR, ATA etc) are

incubators for new astronomy & technology

Radio telescope arrays

Wide and/or multiple independent fields-of-view

Small field-of-view

Mass produced structures, drive and control elements

Precision structural and mechanical engineering

Interference mitigation integral to system design

No, or unsophisticated interference mitigation - as an afterthought

More DSP in signal path(possibly RF quantization below 2 GHz)

Analog signal path(quantization after IF)

Leading-edge un-cooled receivers (or “modestly cooled” receivers with miniature coolers)

Ultra-sensitive cryogenic receivers using massive coolers

Many “medium” or “small” antennasFew “large” antennas

SKA Pathfinders & BeyondNow

PJ Hall, Sept 2007

ISPO

SKA

PJ Hall, Sept 2007

ISPO

SKA at a glance

� Aperture synthesis radio telescope with “1 km 2 ” of effective collecting area by 2020

� Wide frequency range (25 GHz)

� Transformational science via new technologies– Huge survey sensitivity; wide

fields– High resolutions in time,

frequency & spatial domains– Addresses fundamental

physics questions� Innovative design� International funding: > € 1

billion� 2 short-listed sites: WA and

Southern Africa

Cordes et al, SKA Memo 85

x 10 000

Very wide field-of-View

PJ Hall, Sept 2007

ISPO

Wide field-of-view

Allen Telescope Array

Parkes

SKA

PJ Hall, Sept 2007

ISPOConnecting Quarks with the Cosmos: Eleven Science Questions for the New

CenturyUS National Academies Board on Physics & Astronomy (2003)

What Is the nature of the Dark Energy?

How did the Universe begin?Did Einstein have the last

word on gravity? What are the masses of the

neutrinos and how have they shaped the evolution of the Universe?

What is Dark Matter?How do cosmic accelerators

work and what are they accelerating?

Are protons unstable?What are the new states

of matter at exceedingly high density and temperature?

Are there additional space-time dimensions?

How were the elements from iron to uranium made?

Is a new theory of matter and light needed at the highest energies?

�

�

��

�

�

Courtesy Brian Boyle

PJ Hall, Sept 2007

ISPO

A few key RA discoveries

� Quasars, radio galaxies– Jets and super-luminal motion

� Cosmic Microwave Background (3K)� Dark matter in spiral galaxies� Interstellar molecules

– Masers, megamasers (black hole dynamics)

� Pulsars– Gravitational radiation in binary systems

� Slow rotation of Venus� Spin-orbit locking of Mercury

� 4 of 7 Nobel Prizes in Astrophysics to RA

PJ Hall, Sept 2007

ISPO

Today –optical HST

Today -radio VLA

2020radio SKA

** Radio waveband advantage – unaffected by intervening dust **

HST WFPC2 2.5 arcmins FOV

Observing the Distant Universe

Telescopes look back in time

Early galaxies- stars light up

10m +light

CMB“Primordial soup”

- matter and energy

mm-wavesCOBE satellite

NASA

“Dark Ages”- before the stars ? SKAradio

PJ Hall, Sept 2007

ISPO

Dark Ages

Looking back to the Big BangSKA was originally the “hydrogen telescope” born in late 1980s & early 1990s

PJ Hall, Sept 2007

ISPO

SKA science priorities� The first stars and galaxies in the Universe

– Emergence of structure

� Large scale structure of the Universe– “Dark energy”

� Origin and evolution of cosmic magnetic fields– “The magnetic Universe”

� Gravity in the strong field case– Gravitational wave detection

� Planet formation– Including search for extra-terrestrial intelligence (SETI)

� EXPLORATION OF THE UNKNOWN

SKA is the radio member of a suite of next-generation telescopes

PJ Hall, Sept 2007

ISPO

11.5 < z < 5.2

redshift

The “Epoch of Re-ionisation”First stars & galaxies formed at this time

Radio quiet: A clear view to the early Universe

Detecting the first stars & galaxies

Courtesy Carole Jackson

PJ Hall, Sept 2007

ISPO

radio “fish-eye lens”

Inner core

Station

Digital radio camera+ stations to3000 km

Radio fish-eye lens

SKA: the big picture

PJ Hall, Sept 2007

ISPO

3 km

SKA is an “aperture synthesis”telescope

-

A large aperture radio telescope is ‘synthesized’by sampling the wave-front in the aperture plane

SKA needs angular and high dynamic range resolution – not just sensitivity

PJ Hall, Sept 2007

ISPO

SKA in general

� Exploits convergence of radio and ICT– Parameter space + flexibility = discovery

� Uses less metal, more ICT– Many gains via “consumer wave”

� Poses new challenges– New players effective in pivotal technologies

� Is an incubator for selected leading-edge technology– Radio astronomy is traditionally effective in this role– Astronomers are “sophisticated end users”

PJ Hall, Sept 2007

ISPO

Science & engineering exposition

New Astronomy Revs, 48, 2004 Experimental Astronomy, 17, 2004

(www.skatelescope.org for details)

PJ Hall, Sept 2007

ISPO

SKA: radio meets IT

PJ Hall, Sept 2007

ISPO

SKA concept – sensor distribution

(About 150 stations)

(About 2000 antennas)

PJ Hall, Sept 2007

ISPO

SKA as e-science

AntennaArray

DSP(“correlator”)

Post-processingHPC

(“imaging”)

Tier 0(SKA)

Tier 1(National)

Tier 2(Regional)

Tier 3(Institute)

Europe USA Australia South Africa

Pb/s

0.1 – 1 Tb/s

Gb/s

…………

Tier 4(Researcher)

E-science:Global collaboration in key areas of science, and the next generation of infrastructure that will enable it.More data, more computation, faster networks, more collaboration, exploration of data and models – in silicodiscovery, floods of public data, GRID computing, ..J. Taylor, OST.

PJ Hall, Sept 2007

ISPO

SKA technology topics

PJ Hall, Sept 2007

ISPO

Sensor (antenna) types

What defines the primary field-of-view?

(1st stage beam-former technology)

Optics

Electronics

Concentrator (dish)

Aperture phased array

Analog (RF)beamform

Digitalbeamfor

m

Technology choice depends on applications, frequency and delivery epoch

FOV expansion•Optical (multiple feed cluster)•Electronic (phased array feed)

continuum

ATA, meerKAT, APERTIF, ASKAP EMBRACE LOFAR 2-PADMWABEST, SKAMP

Extreme electronic beamforming

Processing of wavefront by“optical” beam-former

Processing of wavefront byelectronics and software

• cost decreases with time – Moore’s law• aperture re-use – many telescopes at once!• individual apertures can be part of much bigger

“aperture synthesis” correlation array

“Extreme” electronic beam-forming(< 1 GHz)

PJ Hall, Sept 2007

ISPO

Top-level SKA engineering� What is desired single FoV sensitivity, (Aeff/Tsys) ?

– What is the best A eff, Tsys trade-off?» Area is especially key to sensitivity at low freq w here Galactic

noise dominates» Receiver noise dominates at high frequencies

� Can Aeff/Tsys be traded for survey speed?– Often, but not always

� Consider survey speed FoM (SSFoM)– (Aeff/Tsys )2 * FoV– Wide FoV may be cheaper than better A/T but how do w e get

it?» What type of antenna?» What cost balance between receptors and downstream signal

processing/computing?

� How do we maintain tractable data volumes, rates and processing power?

� How do we optimize system performance-cost ratio?� System design approach – See SKA Memo 91

– But will use technology snapshots for this talk

PJ Hall, Sept 2007

ISPO

Pre-Sept 07 SKA design numbers� At 1.4 GHz need A eff/Tsys ~ 20 000 m2K-1

– G/T ~ 68 dB K-1

� With T sys ~ 50 K……– (or if Tsys ~ Treceiver receiver noise figure ~ 0.7 dB)

� …Aeff = 106 m2

– Or 1 square kilometre

� FoV– 1 deg2 at 1.4 GHz– At least tens of deg2 below 1 GHz

� For A eff = 106 m2 and cost = €1 billion– SKA must cost < €1000 per m2

– cf present-day telescopes at €10,000 per m2

– Turn to convergence of radio and ICT engineering to develop new design paradigm

PJ Hall, Sept 2007

ISPO

SKA concepts - 2002

Large N,Small D(USA)

LuneburgLens(Aust)

ApertureArrayTiles(Europe)

KARST(China)

LAR(Canada)

CylindricalReflector(Aust)

Small-N Solutions Large-N Solutions

PJ Hall, Sept 2007

ISPO

Luneburg Lens Antenna

• A collimated beam is focussed onto the other side of the sphere

• Beam can come from any direction

• Spherical lens with variable permittivity

“Reference Design” antennas - 2006> 3 GHz: wide-band feed

< 0.3 GHz: sparse aperture array

0.3 – 3 GHz:dish + phased arrayfeed

Mid-band all-sky monitor: dense aperture array

Mid-Band

High-Band

Swinburne/CVA visualization

Low-Band

PJ Hall, Sept 2007

ISPO

SKA antenna applications

3-25

0.3-3

0.3-1

0.1-0.3

Frequency range(GHz)

ATA, TDP, meerKAT

ASKAP, APERTIF

SKADSLOFAR, MWA, LWA

Pathfinders or Design Studies

High-band array

(to ~1 GHz)(to ~0.5 GHz)

Imaging mid-band array

All-sky monitor

Low-band“EoR” array

Dish + Single-Pixel Feed

Dish + Focal Plane Array

Dense Aperture Array

Sparse Aperture Array

Mid-band SKA is the focus of intense Pathfinder act ivity

PJ Hall, Sept 2007

ISPO

Small Dish + Phased Array Feed

Digital beamformer

Phased array feed

Correlator & further processing

Multiple fields

10 m dish cost target:~ €30k exc. feed

FOV expansion factors ~30 maybe practical

~ λ/λ/λ/λ/D radian

D

Terminology: PAF is one type of Focal Plane Array

PJ Hall, Sept 2007

ISPOPhased Array Feed –

FOV Expansion

0 . 0 1

0 .1

1

1 0

1 0 0

1 0 0 0

1 1 0 1 0 0

7 0 0 M H z F O V f o r P a r a b o l i c D is h e s

FO

V (

deg

2 )

D is h D ia m e t e r ( m )

F O V E x p a n s io nF a c t o r

R e q u i r e d F O V

N a t u r a l F O V

P J H a ll , 4 / 0 6 , v 4

Expansion factors ~50 maybe feasible

PJ Hall, Sept 2007

ISPO

PAF Operation

Courtesy D. Hayman

Key question:

How calibratable arePAFs?

PJ Hall, Sept 2007

ISPODeveloping PAFs

Vivaldi array(ASTRON)

Checkerboard array(CSIRO)

PJ Hall, Sept 2007

ISPO

Plastic antennas?

Canada – 10 m carbon fibre mould

South Africa – 15 m composite antenna (KAT XDM)

SKA Receivers – Typical Requirements

25%, to 4 GHz max.~ 25% of centre freq.

Instantaneous bandwidth

> 4 bits> 8 bitsDynamic range

~ 7 K @ 10 GHz ~ 15 K @ 1.4 GHzRx noise equiv.

< 80 K (cooled)300 K (ambient)Physical temperature

RF packageFeed ���� optical O/PIntegration level

“Thousands”“Millions”Number of units

Single feeds(wideband)

Phased arrays(Aperture or focal plane)

Application

3 – 25 GHz(2 sub-bands)

0.1 – 3 GHz(2-3 sub-bands)

Frequency range

High BandLow Band

Low band receivers – one approachLNA

20dB Gain50K Noise Temp-10dBm Comp. Point

HIGHPASS

500MHz~3rd Order2dB Ins. Loss

LOWPASS

1700MHz~3rd Order3dB Ins. Loss

RF AMP

15dB Gain200K Noise Temp0dBm Comp. Point

MIXER

0dB Conv. Loss0dB Comp. Point800K Noise Temp

MIXER

LOWPASS

250MHz5th Order Active0dB Ins. Loss800K Noise Temp

LOWPASS

RF AMP

15dB Gain400K Noise Temp5dBm Comp. Point

VGA

SAMPLER

512Msps8 bit

SAMPLER

LO AMP

LO AMP

VGA

20-25-30dB Gain800K Noise Temp0dBm Comp. Point

D

Q

Q

D Q

Q

QUADRATURE LO

LOCAL OSCILLATOR3000 - 5800 MHz

A POL RF IN500 - 1700 MHz

SAMPLE CLOCK512 MHz

PASSIVE PASSIVE ACTIVE

ACTIVE

GILBERT CELL

GILBERT CELL

SERIALISER

E

E

E

O

O

O

0.18 um RF-CMOS

INTEGRATED RECEIVERHIGH DYNAMIC RANGE

500-1700 MHz RF Band512 MHz IF (Direct IQ Conversion)8 bit Digitiser50 K Noise Temperature (0.7 dB NF)

E

O

B POL RF IN500 - 1700 MHz

0.18 um RF-CMOS

INTEGRATED RECEIVERHIGH DYNAMIC RANGE

A POL DATA8.192 Gbps

B POL DATA8.192 Gbps

RECEIVER ELEMENT (1 OF 64)

DUAL POLARISATIONWIDEBAND TAPEREDSLOT ANTENNA

850nm FIBRE TOCONTROL ROOM

0

50

100

150

200

250

300

350

400

1994 1996 1998 2000 2002 2004 2006 2008Year

Tra

nsis

tor f

T (G

Hz)

0

0.05

0.1

0.15

0.2

0.25

0.3

0.35

0.4

Gat

e Le

ngth

(µm

)

Transistor Speed

Gate Length

Length Trend

Speed TrendRF CMOS Integrated Receiver500 – 1700 MHz

S. Jackson, J. Harrison, P. Hall

PJ Hall, Sept 2007

ISPO

“Cheap as chips” receiver

Low-band CMOS receiver: 3.5 x 2.5 mm, I-Q baseband architecture0.3 – 1.7 GHz, RF���� digital solution

Jackson, Hall, Harrison

“Jelly bean” receiversare enabling technologyfor phased arrays

PJ Hall, Sept 2007

ISPO

SKA – not just antennas

� High speed data transport– Tb/s from EACH station on scales of hundreds of km – 100 Gb/s trans-continental and trans-oceanic links– Longest links will rely on telcos and research networks– Need government support for economical access

� Signal processing– Peta-ops per second– Need highly scaleable solutions

� Post-processing, information management– New super-computer architectures– Archive and sharing of data will be a major challenge

� Infrastructure– Civil, electrical (power, …), communications

� Operations and support

PJ Hall, Sept 2007

ISPO

Technology growth rates

0 1 2 3 4 5 6

Number of years

Performance per Dollar Spent Optical fibre

(bits/sec double every 9 months)

Data Storage(bits per square inch

double every 12 months)

Silicon Computer Chips(Number of transistorsdouble every 18 months)

Source: Scientific American

0 1 2 3 4 5 6

Number of years

Performance per Dollar Spent Optical fibre

(bits/sec double every 9 months)

Data Storage(bits per square inch

double every 12 months)

Silicon Computer Chips(Number of transistorsdouble every 18 months)

Source: Scientific American

PJ Hall, Sept 2007

ISPO

High Performance Computing

� “Starving in an era of plenty” (Dally et al 2001)– Raw GFLOP, memory, bandwidth costs all down– Still supercomputers cost much more per GFLOP & GByte than

low-end machines» Scalability is the issue

� Scalability removes barriers in key applications– Signal processing & analysis, protein folds, fluid flow in machinery,

…

� Streaming promises scalability to PFLOPS– Involves stream architectures, high-speed signaling, efficient

interconnection

� New HPC architectures and implementations are enabling technology for next-generation telescopes– Calibration, imaging and visualization– Real-time signal processing – HPC in data stream– Electromagnetic synthesis and simulation– …

PJ Hall, Sept 2007

ISPO

HPC in signal path� Replace DSP environment with

supercomputer– e.g. LOFAR and BlueGene/L– Enormous flexibility and upgrade potential

� Augment CPU with FPGA “engines”– E.g. improved FFT

� Design new processors suited to streaming/DSP– e.g. integer arithmetic– More attractive “total cost of ownership”

� Excellent current opportunities for radio astronomers to have major impact on new-generation supercomputers

PJ Hall, Sept 2007

ISPO

DSP or HPC?

� Line between DSP and general purpose computers will be blurred

DZB/Jive

SKA

LOFAR

Courtesy ASTRON

PJ Hall, Sept 2007

ISPO

Data transmission realities

� Total costs > €200 M– Even with advances in f/o sources etc

� High trenching costs – must share with power etc

� Need careful optimization between WDM and multiple fibre approaches

� Fibre management (incl. connectors etc) is a major issue

� Different technology optimizations for different distances

� Longest links will rely on telcos and research networks– Need government cooperation for

economical access

PJ Hall, Sept 2007

ISPO

Global connectivity

Source: Simon Olawo, EASSy

Up to 640 Gb/scapacity

PJ Hall, Sept 2007

ISPO

SKA development

PJ Hall, Sept 2007

ISPO

SKA challenges - summary

� Technology

� Project Management

� Wideband, efficient antennas

� Sensitive, low-cost receivers

� Fast, long-distance, data transport

� High performance DSP & computing hardware

� New data processing and visualization techniques

� Large-scale software engineering

� Evolving science goals� High levels of technical

risk� International politics

– Possible funding phase slips

� Ambitious delivery timescale

� Industry liaison

Performance + Cost

PJ Hall, Sept 2007

ISPO

SKA development approach� Astronomy &

engineering iteration to refine specs– Rapid convergence

� International system design effort

� Strong emphasis on technology demonstration– Retire risk as early as

possible– Regional pathfinders are

crucial» > €200M investment

� Focus on:– Aggressive cost reduction

strategies– Industry engagement

» To deliver SKA on required timescales

Reference Designtechnologies

1% (pathfinders) ���� 10% (SKA Phase 1) ���� 100% (SKA)

PJ Hall, Sept 2007

ISPO

Two large pathfinders

LOFAR ATA

+ meeKAT, ASKAP, SKADS, TDP, …..

Multiple fields-of-view

(350 x 6.1m)

PJ Hall, Sept 2007

ISPO

Recent ATA-42 result

HI image

Technology Readiness Level (TRL)

NASA/DoDPrepSKA + Pathfinders

Desirable SKA performance - 2007KSP ID

KSP Description Frequency Range GHz

FoV Sens-itivity

Survey Speed

Resn. Base-line

Dyn. Range

Poln.

0.1

0.3 1.0 3.0 10 30 deg2 m2/K deg2m 4K - 2 mas Km L M H L M H

1 The Dark Ages

1a* EoR >~3x107 1 L H

1b First Metals 0.003 15,000 50 125 L L

1c First Galaxies & BHs 20,000 10 4500 H H

2 Galaxy Evolution, Cosmology & Dark Energy

2a* Dark Energy 6x109 5 L L

2b* Galaxy Evolution 1x109 10 L L

2c Local Cosmic Web 2x107 0.5 L L

3 Cosmic Magnetism

3a* Rotation Measure Sky

2x108 10-30 M H

3b Cosmic Web 1x108 5 M H

4 GR using Pulsars & Black Holes

Search 1x108 ~5 - L

4a* Gravitational Waves - >15,000 1 200 M H

4b BH Spin 1 10,000 - M H

4c* Theories of Gravity >15,000 1 200 M H

5 Cradle of Life

5a* Protoplanetary Disks <10-5 10,000 2 1000 L L

5b Prebiotic Molecules 0.5-1 10,000 100 60 L L

5c SETI 1

6 Exploration of the Unknown

Large Large

PJ Hall, Sept 2007

ISPO

SKA performance-cost optimization

� What are the specification trade-offs?

� What specs enable transformational science within a given budget?

� Draft specs now available

� Design your SKA at: http://www.atnf.csiro.au/projects/ska/cost/

PAF v WBSPF for constant SSFoM

0100200300400500600700800900

1000

0 10 20 30 40diameter

cost

€M PAF 1x10 9̂

PAF 3x10 8̂

WBSPF 3x10^8

Ae/Tsys=10000 m^2/K, Fmax=3 GHz, Tsys=35K, Eff=65%

0

500,000,000

1,000,000,000

1,500,000,000

2,000,000,000

2,500,000,000

6 10 12 15 20

Dish Diameter [m]

Computing

Correlator

Long Haul Links

Station Electronics

Short Haul Links

Antenna Electronics

Antennas

PJ Hall, Sept 2007

ISPO

SKA draft specifications – 2007� Upper frequency limit for phase two ~8

GHz– Higher frequencies as part of “Phase 3” (post-2020)

� Lower frequency limit ~ 0.07 GHz– But should 0.07 – 0.3 GHz array should stay as part of

SKA?

� Survey science emphasis– Survey speed as primary spec– Includes explicit recognition of transient surveys

� Narrower band antenna solutions– 3:1 for phased arrays; 6:1 for single-pixel feeds– Likely more pronounced performance-to-cost peaks than

10:1 designs– More “sub-classes” of aperture array & dish feeds

» Greater role for sparse aperture arrays < 0.6 GHz

� Wide-field (~30 deg 2) synthesis imaging limited to baselines below ~5 km – Mitigates huge spectral line computing burden

Lorimer et al.

30 Jy peak, ms duration

PJ Hall, Sept 2007

ISPO

Draft top-level SKA specs - 2007Parameter

Phase 1 10% SKA

Phase 2 Full SKA at low & mid

bands

Phase 3 Full SKA

Frequency range: Low (GHz) High (GHz)

0.200 3

0.070 3 (8)

0.070 25 (35)

Survey speed (m4K-2deg2) * 70 - 200 MHz

200 - 500 MHz 0.7 GHz 1.4 GHz

3 GHz 8 GHz

25 GHz

- 1.2 x 106 (1 x 107) 3 x 105 (1 x 107) - -

3 x 109 (2 x 1010) 1.3 x 107 (2 x 1010) 1.2 x 108 (2 x 1010) 6 x 107 (6 x 108) (2.6 x 106) 1.4 x 107

(4 x 105) 2 x 106

3 x 109 (2 x 1010) 1.3 x 107 (2 x 1010) 2.4 x 108 (2 x 1010) 1 x 109 (6 x 109) 1.4 x 107

8 x 106

Min. sensitivity at 45o (Aeff/Tsys) (m2K-1) *

70 - 200 MHz

200 - 500 MHz 0.5 - 3 GHz

8 GHz 25 GHz

700 250

4 000 - 10 000 10 000 (4 500) - 10 000 (2 500) - 5 000

4000 - 10 000 10 000 10 000 10 000 5 000

Configuration core (< 1km) inner (< 5 km)

mid (< 180 km) outer (up to at least 3000 km)

5 % 7.5 % 10 % 10%

20 % 50 % 75 % 100 %

20 % 50 % 75 % 100 %

Signal processing Spectral image size/time domain

(max baseline) channels

sample rate

5 km 16 384 0.1 ms

10 km 16 384 (32 768) 0.1 ms

20 (50) 16 384 (32 768) 0.1 ms

NB: no explicit field-of-view specification

PJ Hall, Sept 2007

ISPO

SKA project matters

PJ Hall, Sept 2007

ISPO

SKA site selection� Physical characteristics required

– Very quiet radio frequency environment, particularly for the core region

– Large physical extent (> 3000 km)– Low ionospheric turbulence– Low troposphere turbulence

� Not many suitable sites in the world

� Site selection process started in 2003– Request for full proposals issued 1 September 2004– Four proposals received on 31 December 2005– Short-list of two acceptable sites 30 August 2006– Likely final selection ~2011

PJ Hall, Sept 2007

ISPO

Telescope siting - clues

PJ Hall, Sept 2007

ISPO

Terrestrial RFI

FORTÉ satelliteForte Satellite

PJ Hall, Sept 2007

ISPO

Industry interaction in host country(possible)

€ 200M

Host nation has to be smart in reaping hi-tech returns.Example: universities (or similar) can be incubators of collaborations.

� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � �

� � � � � � �� � � � � � �

� � �� � � �

� � �� � � � � � � � � � � � � � �� � � � � � � � �! � � " �

PJ Hall, Sept 2007

ISPO

SKA timeline

98 06 07 08 09 10 11 12 13 14 18 22200

2

Concept DemosConcept Demos Concept DesignConcept Design System DesignSystem Design Phase 1 (10%) Phase 1 (10%) ConstConst ’’nn Full Full ConstConst ’’nn

Europe: SKADS

US: Technology Dev Programme - TDP

US: Allen Telescope Array - ATA

Aust.: Australian SKA Pathfinder - ASKAP

South Africa: Karoo Array Telescope - MeerKAT

Netherlands: Low Frequency Array - LOFAR

ISSCMoAs

ScienceCase

published

Referencedesign selected

Site short-list

‘‘1% SKA1% SKA’’ScienceScience

EC-FP7: PrepSKASystem design Funding Governance Site Selection

‘‘10% SKA10% SKA’’ScienceScience

SKASKACompleteComplete

Concept Desgn. Ext.Review

Initial specs:10% & full

SKA

PJ Hall, Sept 2007

ISPO

SKA timeline

98 06 07 08 09 10 11 12 13 14 18 22200

2

Concept DemosConcept Demos Concept DesignConcept Design System DesignSystem Design Phase 1 (10%) Phase 1 (10%) ConstConst ’’nn Full Full ConstConst ’’nn

Europe: SKADS

US: Technology Dev Programme - TDP

US: Allen Telescope Array - ATA

Aust.: Australian SKA Pathfinder - ASKAP

South Africa: Karoo Array Telescope - MeerKAT

Netherlands: Low Frequency Array - LOFAR

ISSCMoAs

ScienceCase

published

Referencedesign selected

Site short-list

‘‘1% SKA1% SKA’’ScienceScience

EC-FP7: PrepSKASystem design Funding Governance Site Selection

‘‘10% SKA10% SKA’’ScienceScience

SKASKACompleteComplete

Concept Desgn. Ext.Review

Initial specs:10% & full

SKA

€18M ($25M)

Pathfinders:

€65M (AU$100M)

€105M (1Bn Rand)

€104M

PJ Hall, Sept 2007

ISPO

SKA timeline

98 06 07 08 09 10 11 12 13 14 18 22200

2

Concept DemosConcept Demos Concept DesignConcept Design System DesignSystem Design Phase 1 (10%) Phase 1 (10%) ConstConst ’’nn Full Full ConstConst ’’nn

Europe: SKADS

US: Technology Dev Programme - TDP

US: Allen Telescope Array - ATA

Aust.: Australian SKA Pathfinder - ASKAP

South Africa: Karoo Array Telescope - MeerKAT

Netherlands: Low Frequency Array - LOFAR

ISSCMoAs

ScienceCase

published

Referencedesign selected

Site short-list

‘‘1% SKA1% SKA’’ScienceScience

EC-FP7: PrepSKASystem design Funding Governance Site Selection

‘‘10% SKA10% SKA’’ScienceScience

SKASKACompleteComplete

Concept Desgn. Ext.Review

Initial specs:10% & full

SKA

€38M

Design Studies

€9M ($12M)

PJ Hall, Sept 2007

ISPO

SKA timeline

98 06 07 08 09 10 11 12 13 14 18 22200

2

Concept DemosConcept Demos Concept DesignConcept Design System DesignSystem Design Phase 1 (10%) Phase 1 (10%) ConstConst ’’nn Full Full ConstConst ’’nn

Europe: SKADS

US: Technology Dev Programme - TDP

US: Allen Telescope Array - ATA

Aust.: Australian SKA Pathfinder - ASKAP

South Africa: Karoo Array Telescope - MeerKAT

Netherlands: Low Frequency Array - LOFAR

ISSCMoAs

ScienceCase

published

Referencedesign selected

Site short-list

‘‘1% SKA1% SKA’’ScienceScience

EC-FP7: PrepSKASystem design Funding Governance Site Selection

‘‘10% SKA10% SKA’’ScienceScience

SKASKACompleteComplete

Concept Desgn. Ext.Review

Initial specs:10% & full

SKA

€22M (€7.6M EC FP7)

€250M€250M€1.5B€1.5B

Anticipated

SKAFundingDecison

Anticipated

SKASKAFundingFundingDecisonDecison

SKA management structureInternational SKA

Steering Committee

Executive Committee

International Science Advisory

Committee

International Engineering

Advisory Committee

International Site Selection Advisory

Committee

Outreach Committee

Engineering Working Group

Site Evaluation Working Group

Simulations Working Group

Science Working Group

International SKA Project Office

OperationsWorkingGroup

International CollaborationWorking Group

8 task forces 2 task forces 1 task force6 task forces

Current SKA management structure

PJ Hall, Sept 2007

ISPO

SKA preparatory phase: PrepSKA(2008 – 2011)

� WP1: PrepSKA management� WP2: SKA system design

– Includes hardware & software Initial Verification System – Establishes ISPO Central Design Integration Team (CDIT)

» 15 engineers» Located Manchester UK

� WP3: Continuing site selection process– Regional, international, joint projects

� WP4: Governance� WP5: Industry and procurement policy� WP6: Funding model� WP7: Implementation strategy

€ 22M Eu program with strong international collaborati on (including US Technology Development Project)

PJ Hall, Sept 2007

ISPO

CentralDesign

IntegrationTeam

Canada(ASKAP)

Europe(LOFAR,SKADS)

SouthAfrica

(MeerKAT)

Australia(ASKAP)

USA(ATA,TDP)

Other(via ISPOworkinggroups)

Technology innovation& prototyping

System design& integration

WP2 SKA design

PJ Hall, Sept 2007

ISPO

WP2: SKA design� Recognizes primary role of Pathfinders &

Design Studies in technology development

� Leverages current programs to generate coherent SKA design– Brings the best technologies together into complete program– Emphasizes “fit for manufacture” design

� Delivers– Overall SKA concept design, with costing– Detailed SKA Phase 1 design– Initial Verification System for SKA Phase 1 design

� Demonstrates functional central team, plus strong working links to regional engineering

� ~180 p*yr effort� Many shared central and regional projects

for 4 -year duration of WP2

PJ Hall, Sept 2007

ISPO

WP5: Procurement� Recognizes that industry is crucial to SKA developme nt,

delivery & operations� Coordinated by INAF� Procurement Working Group to be formed

– Funding agencies, consultants, industry, …

� PWG looks at:– Potential for global industry in development & construction– Possible procurement models

» Maximize added-value for participating nations (recognize different ambitions)– Risks attached to various models

� PWG outputs:– Procurement options paper for discussion by funding agencies etc., then– Draft policies on industry engagement, procurement, protocols for research

institute involvement, ….

� Opportunities for national industry input to PrepSKA WP5– Via national funding agencies, national research bodies, ISPO engineering

task forces » Ideal routes for industry clusters, peak bodies, …

CDIT project managementCDIT

WP2 design study management

P10

Science post –proc.CSIRO

CalibrationASTRON

Data products & VO planUK:cam

Software engineeringASTRON

Computing hardwareCDIT

SKA computing & software spec.CDIT

Computing specification & prototyping

P9

Non-imaging processorsUK:man

RF interference mitigationASTRON

CorrelatorDRAO

Station DSPUK:oxf

Signal processing prototyping

P8

Monitor & controlUK:cam

LO and timingUK:man

Station-core data linksUK:man

Intra-station data linksUK:man

Intra-antenna data linksCSIRO

Signal transport prototyping

P7

New-gen. cryo solutionsTDP

Integrated receiversCSIRO

Low-noise amplifiersASTRON

Receiver prototyping

P6

WFoV –Multiple-feed clustersKAT

WFoV -Phased array feedsCSIRO

WFoV –Aperture array tilesUK:man

Wideband single-pixel feedsTDP

Feed prototypingP5

Dish design 4(hi perf. metal)TDP

Dish design 3(carbon fibre)DRAO

Dish design 2(composite)KAT

Dish design 1(basic metal)CSIRO

Dish design & optimization

P4

IVS integration & testCDIT

IVS constructionUK

IVS specificationCDIT

Initial Verification System

P3

SKA-P1 sub-systems spec. & evaluationCDIT

SKA-P1 sub-system spec & evaluation

P2

SKA system designCDIT

SKA technicaldoc.CDIT

SKA manu-facturingstudiesUK:man

SKA cost opt’nCDIT

SKA support planCDIT

SKA operations planASTRON

SKA life-cycle studyKAT

SKA specificationCDIT

SKA concept delineationCDIT

SKA designP1

T 9T 8T 7T 6T 5T4T3T2T1

FP7 Preparatory Phase: Elements of Work Package 2 ( WP2)

CDIT project managementCDIT

WP2 design study management

P10

Science post –proc.CSIRO

CalibrationASTRON

Data products & VO planUK:cam

Software engineeringASTRON

Computing hardwareCDIT

SKA computing & software spec.CDIT

Computing specification & prototyping

P9

Non-imaging processorsUK:man

RF interference mitigationASTRON

CorrelatorDRAO

Station DSPUK:oxf

Signal processing prototyping

P8

Monitor & controlUK:cam

LO and timingUK:man

Station-core data linksUK:man

Intra-station data linksUK:man

Intra-antenna data linksCSIRO

Signal transport prototyping

P7

New-gen. cryo solutionsTDP

Integrated receiversCSIRO

Low-noise amplifiersASTRON

Receiver prototyping

P6

WFoV –Multiple-feed clustersKAT

WFoV -Phased array feedsCSIRO

WFoV –Aperture array tilesUK:man

Wideband single-pixel feedsTDP

Feed prototypingP5

Dish design 4(hi perf. metal)TDP

Dish design 3(carbon fibre)DRAO

Dish design 2(composite)KAT

Dish design 1(basic metal)CSIRO

Dish design & optimization

P4

IVS integration & testCDIT

IVS constructionUK

IVS specificationCDIT

Initial Verification System

P3

SKA-P1 sub-systems spec. & evaluationCDIT

SKA-P1 sub-system spec & evaluation

P2

SKA system designCDIT

SKA technicaldoc.CDIT

SKA manu-facturingstudiesUK:man

SKA cost opt’nCDIT

SKA support planCDIT

SKA operations planASTRON

SKA life-cycle studyKAT

SKA specificationCDIT

SKA concept delineationCDIT

SKA designP1

T 9T 8T 7T 6T 5T4T3T2T1

FP7 Preparatory Phase: Elements of Work Package 2 ( WP2)

PJ Hall, Sept 2007

ISPO

SKA - recent progress� Reference Design selected

– Key development technologies identified– Initial emphasis on bands <10 GHz endorsed

� Sites short-listed� Major progress in Pathfinders: meerKAT, ASKAP,

SKADS, ATA, LOFAR, …� Funding Agencies Working Group formed

– International SKA Forum proposal

� “Directed” science-engineering interaction –a.k.a. tough talking– Updated science case, detailed engineering system studies, new

performance vs cost analysis– More emphasis on SKA Phase 1 – Initial specifications (and SKA evolution) to be set by early 2008

� First-round infrastructure study complete� Successful PrepSKA European 7 th framework

submission

PJ Hall, Sept 2007

ISPO

International SKA – coming milestones

� Late 2008: Major engineering specs agreed– Includes “base” (dish) technology option

� Early 2009: External engineering review� 2010,11: Reviews of pathfinder technologies

– Can “base” technology be extended to wide fields-of-view?

� ~ 2011: Possible site selection� End 2011: SKA system design

– Top-level SKA

– Detailed SKA Phase 1

� 2012-20: Progressive SKA rollout