Towards Ne

Peter

A iArtisanJan 2

w Horizons

Hekman

B lfn, Belfast 8, 2014

Agen

I d i Introduction Scopep Technology Trends

R di T l Radio Telescopes Summaryy

nda

Introdu Peter Hekman Formerly Work Package Formerly Work Package

AIV in Oxford at STFC-R Currently Project Manage Currently Project Manage Background experiences

Semiconductors and WireSemiconductors and Wire Worked in Research, Pro

Volume Production linesVolume Production lines. Companies: SKA, ESO, A

Astron and Thales NetheAstron and Thales Nethe

uction

manager ALMA Front Endmanager ALMA Front End RALer AIV for SKA Telescopeer AIV for SKA Telescope.s in Radar, Radio Astronomy, eless communicationseless communications.

oduct development and high

Alu BLI, MaCom, NXP, T3G, erlandserlands.

Sco

The scope of this presapplication of radio anppin Radio Astronomy.

Trends in Radio Astro Trends in Radio Astro New RA Flag ships

ope

sentation will be the nd microwave technology gy

nomy Telescopesnomy Telescopes

New TechNew Tech With the cheap and powerfu

are now Software driven wit Download-able ”Apps” to in

fi blreconfigurable Examples

– Smart Car, Phone, Radiocomputing

– Medical and safety equip– Wireless and remote sen– Robots and Drones

hnologyhnologyul micro processors , products th the support of Hardware.crease functionality and

o, TV, base stations, mobile

mentsors

SMART AntenSMART Anten Cellular and Wireless N Radar systems

El t i W f Electronic Warfare cou Satellite systemsy Radio Astronomy

Maximize antenna Minimize the gain

Interference Reuse array, MIM

nna Systemsnna SystemsNetworks

t

Desired User

untermeasures

Interfering User

a gain is a desired directionAntenna Array

User

in directions of

MO

1st Radio T

1930, Karl. Jansky, 31 ft operating at 20.5 MHz

Discovered Radio waves from MilkyDiscovered Radio waves from Milky way

Telescope

1940,Grote Reber 31ft diameter Primary focusGrote Reber, 31ft diameter, Primary focus parabolic reflector (150 – 3000MHz)

RequireRequire Key Parameters

Collecting area Low Noise

receivers Band width High Dynamic

rangeFigure of Merit Figure of Merit

Aeff/Tsys

Single beam > Slow survey sp Use Interferometry to increase Use Interferometry to increase Reached Practical limits

ementsements

Make bigger antennas

Cryogenic cooled LNA

Double side band

Dual Polarization Dual Polarization

Very High Linearity

peed, sensitive to interferencese Aeff and higher selectivitye Aeff and higher selectivity

When is bigWhen is big

Green Bank TeleGreen Bank TeleWest Virg

Nov. 18

g too big?g, too big?

escope 300ft dishescope 300ft dishginia, USA8, 1988

New Green Ba(GB

Larg

Tto

Ituaththra

BOO

W

ank Telescope BT)

est Fully-Steerable Telescope

The Green Bank Telescope operates at meter o millimeter wavelengths.

s 100-meter diameter collecting area, nblocked aperture, and excellent surface ccuracy provide excellent sensitivity across

he telescope's full 0 1–116 GHz operatinghe telescope s full 0.1 116 GHz operating ange.

Build start: 1991Operation: 2002Operation: 2002

West Virginia, US

Radio TelRadio Tel

Arecibo Observatory, Porto Rico, 305m

Westerbork Array, Netherlands 14x25m, fixed baseline 2700m

escopesescopes

Jodrell Bank Observatory, UK, 76m diam

Very Large Array, US. Max. baseline 22 miles, 27x 25m diam

Next GeneratioObserva

ALMA mm/sub mmALMA mm/sub-mm

SJWST far-infra red

on Astronomy atories

E ELT opticalE-ELT optical

SKA radio

E EE-EEuropean Extremely

Very Large Telescope

ELTELTy Large Telescope

Optical and near IROptical and near IRAltitude: 3060m asl789 hexagonal mirrors with adaptive opticsOptical reflector: 39 m diameterOptical reflector: 39 m diameterSecondary optical mirror: 4 m diameterOperational: 2020CCosts 1.3 B Euro

Largest Optical Telescope in the world: Collects 13x more light than gthe largest optical Telescope today.

James Webb SpJames Webb Sp

Optical Telescope Element diffraction limited at 2 micron w25 m2 6 35 m average diameter aperture 25 m2 , 6.35 m average diameter aperture.

Instantaneous Field of View (FOV) ~ 9’ X 18’. Deployable Primary Mirror (PM) and Secondary Mirro Integrated Science Instrument Module (ISIM) contain

instrumentsinstruments.Deployable sunshield for passive cooling.Power Generation: 2000 Watts Solar Array.Data Capabilities: 471 Gbits on-board storageScience Data Downlink: 28 MbpsScience Data Downlink: 28 Mbps.Life: Designed for 11 years (goal) of operation.Orbit at 1.5 million miles from earthLaunch date 2018

pace Telescopepace Telescope

wavelength.

or (SM)ing near and mid infrared cryogenic science

ALMALMAtacama Large mm and

Project start: 1990, Operational:

Radio Astronomy Telescope:

66x 12 meter dishes, max Basel

Angular resolution at 300GHz is g

100x times more sensitive that c

Frequency range: 30 – 960 GHzq y g

Cryogenic Cooling

Dual Polarization Dual Polarization

5000 m above sea level in Chile

Costs: 1200 M Euro Costs: 1200 M Euro

Consortia: North America, Europ

MAMAd sub mm ArrayMarch 2013

ine 16km

0.015 arc Sec

current mm Interferometers

z in 10 bands

pe and Far East.

ALMALMAtacama Large mm a

Power & Comms

ALMA Antenna Transporter

A t D kiAntenna Docking Pad (192x) Dowels 3x

MAMAand sub mm Array

OSF (2900m asl)OSF (2900m asl)

Array Operating Site (AOS) 5000m asl

Eu Front End IntEu Front End Int

Near Field Beam and Phase measurements

Cryostat IF Elect

tegration Centretegration Centre

FE#26 R d fFE#26, Ready for Shipping to Chile.STFC-RAL Jan 2013

ronics Rack

ALMA mm waALMA mm wa

Co

ALMA Front End Receiver

ave Front Endave Front End

old Cartridge

Warm IF Band 5 : 163 - 211 GHz

SKA TelSKA Tel Square Kilometer Array.

Over 1.000.000m2 antenna

50x more sensitive than wo50x more sensitive than wo

Up to 10.000 faster in surve

B li t 3000 k Base lines up to 3000+ km.

Frequency range: 50 MHz –

Clear-aperture, offset-Greg

Real time signal processing Real time signal processing

Estimated costs: 1.2 B Euro

Consortia: Canada, Europe, SChina

escopeescope

a collecting area

orlds best Interferometerorlds best Interferometer

ey speed

.

– 10 GHz

orian optics design for Dish

g (very high data rate)g (very high data rate)

o

South Africa, Australia, India,

SKA sumSKA sumThe SKA will have: – up to 3000 dishes, with:

– wide band single pixel feeds

h d f d– phased array feeds

– ~1 GHz to >10 GHz

– up to 250 dense Aperture Array statio(56m diameter), with:– ~70,000 dual pol elements, so ~150,000 

receiver chains, total 40 M elements

– ~400‐~1400 MHz

– up to 250 sparse Aperture Array statio(180m diameter) with:(180m diameter), with:– ~10,000 dual pol elements, so ~20,000 

receiver chains, total 5 M elements  

~50 ~400 MHz– ~50‐~400 MHz

mmarymmary

ons 

ons 

SKA SSKA SSouth Africa (Cape Town)

Karoo

Home to: 64x Meerkat and 190x SKA Dish Mid and 250x

Karoo

190x SKA Dish-Mid and 250x MFAA

SitesSitesPrecursors

Single Point Feed Wideband

Meerkat13.5m diam

South AfricaSouth AfricaKaro

Great Karookm2

a Core Sitea Core Siteoo

o has an area of more than 400,000 ,

SKA SSKA SAustralia (Perth)

Boolardy

Home to: 36x ASKAP, 60x SKA Dish-Survey and 2.500.000x LFAA y

Murchison Widefield Array128 x 16, 80 – 300 MHz

SitesSitesPrecursors

Phased Array Feed

ASKAP 12m diamASKAP 12m diam

Western AustrWestern AustrBoolardy

ralia Core Siteralia Core Site3500 square kilometres

♦ PAF technology electronic“beams” from the same pbeams  from the same p

♦ Used in radar systems forybut new challenges arise 

♦ Need large bandwidths fo

cally generates multiplephysical antennaphysical antenna 

r years, y ,in astronomy

or best science

SKA PreSKA PreSouth Africa;Meerkat 13.5m diameter13.5m diameter

64 dishes

Wideband single pixel feed Wideband single pixel feed

Dual polarization

C i C l d LNA Cryogenic Cooled LNA

Can carry 5 cooled FE's

Goal is high sensitivity

ecursorsecursorsAustralia;ASKAP

12m diameter dish 12m diameter dish

38 dishes

L band (1420 MHz) L-band (1420 MHz)

Phased Array Feed

94 x 94 elements (188)

Dual polarization

Ambient temperature LNA

Capable of 36 beams

Goal is high Survey speed

SKA Dish (aSKA Dish (a

Up

a prototype)a prototype)

Using composite carbon fibre, single piece mold prototype (Canada)

SKA Low (SKA-Low (

LPDA by Cambridge, SiteAustralia

Frequency range: 50 – 60Frequency range: 50 60Dual polarizationDense/ Sparse transitionSKA goal: 2.5 M dipole e

prototype)prototype)

e test array 16 elements,

00 MHz00 MHz

at 111 MHzlements.

MFAA (prMFAA (pr

Vivaldi Array (Dense)Dual polarisationEMBRACE500 – 1500 MHz

rototype)rototype)

Prototype Tile

SKA ChaSKA Cha Technical

– Wide bandwidth, SensMitigation, Calibration,

P liti l ( ti l i Political (national science prog

Financial (1.3 B Euro)

Fast and low cost deployment

Environmental (sites are natio

Need innovative designs to red

High growth of Wireless techng gapproach of Single beam teles

– Urgent need to more foT lTelescopes.

allengesallenges

sitivity, Cost, Interference Upgrade path, Operations

)grams)

(~30min/LFAA, fully AIV-ed)

nal heritage sites, RFI)

duce cost

ology expected: Current gy pscopes has hit the limits.

or multi beam and SMART

SKA PSKA P

Power Supply Options Power Supply Options Diesel LPG Grid Electricity

Dominate Operations cost budget ~50%

50Mega Watt per site Costs ~130M USD/year High Capital Costs High Maintenance costs High Maintenance costs

PowerPower

Potential Opportunities Potential Opportunities Solar Power

High W/m2 Low Transmission

lossesBut High Capital costs Need Storage for nightg g Cleaning of Collectors

Micro-dust Micro dust

RFI ChaRFI ChaSKA-Low (IBW)

MFAA

Air coms & Navi.Shortwave

Mil. Sats

Terr Broadc

Terr. BroadcMob comms

Airborne

70MHz

Terr. Broadc

Satellites

Wireless

Short wave Propagation

Over the Horizon Radar

allengeallengeSKA-mid

SKA s r eIridium, Glonass, Sat. Broadc

SKA-survey

Test Equi. Noise floor

H2 line

Equipment made RFI

Frequency and time domain interferences

LNA d iti ti IMD LNA de-sensitization, IMD

Critical TecCritical Tec Antennas and Feeds

Wideband and multi beeasy to deployPhased Array Feeds Phased Array Feeds

RF Front EndsLo noise req ires hig Low noise, requires hig

GaAs or InP MMIC recRF over Fibre RF over Fibre

Signal Transmission and DisDi it l Si l i Digital Signal processing

Software SKA will largely be a S

chnologieschnologies

eaming, low cost manufacturing,

gh integrationgh integrationceivers

stribution

Software Radio Telescope.

Telescope Ae/TTelescope Ae/T

DSN 70m Tsys=18Arecibo 305m Tsys=25VLA 27x25m Tsys=32VLA 27x25m Tsys=32

GBT 100m Tsys=20ALMA 64 12 T 50ALMA 64x12m Tsys=50SKA 1km2 Tsys=50

Tsys summaryTsys summary

Ae/Ts= 145 year 1965Ae/Ts= 1414 1970Ae/Ts= 280 1982Ae/Ts= 280 1982

Ae/Ts= 285 2000A /T 98 2013Ae/Ts= 98 2013Ae/Ts= 20.000 2024

SummSumm Radio is un-missable in to

P d t bi d Products are bigger and ccooperation and multi discall in-house.all in house.

Big projects are sensitive tSchedule and Politics.

Products are SMART drivefly reconfigurability.

S ft f t di t t– Software features dictate Radio Astronomy is going

Multi Beam and SW reco– Multi Beam and SW reco There are plenty interestin

engineers in the years aheengineers in the years ahe

marymaryday’s technology and life.

l i i i t ti lcomplex requiring international ciplinary companies rather than

to Funding, Resourcing,

en: high emphasis on on-the-

H d l tie Hardware solutions.SMART too.

onfigurableonfigurableng challenges for RF ead.ead.

ThankThankk Youk You.

Back upBack upp slidesp slides

SKA InternatioSKA Internatio

SiteSelection

2012

20162016

2013-15 2016-19

Phase 1 Construction

(10% )

Detailed Design and Pre-Construction Phase

( )

onal Time Lineonal Time Line

Full science operations with

Full science operations with

Phase 1 Phase 2

2020 2024

2019-24

Phase 2 Construction

(100% )n

( )

SKA BaselineSKA BaselineCove

e Frequencye Frequency rage

SKA1_low911 stations911 stationsX  289 elements

SKA1 mid arraySKA1_mid array190 SKA dishes (15m) +64 Meerkat (13.5m)dishes

SKA1_survey60 SKA dishes (15m) +38 ASKAP (12m)dishes

SKA-Low FunSKA-Low Fundiagram (p

Depicted for 1 polarizationDepicted for 1 polarization

nctional blocknctional block proposal)

CoolingCooling

SKA Key ScieSKA Key Scie•Hydrogen survey – dark ener•Pulsar survey – strong field tof gravity

•Cosmic magnetism – origin ofields

•Cradle of Life• Epoch of Re‐ionization• Exploration of the Unknown

ence Driversence Driversrgyests 

of B 

n

ALMA SkyALMA Skyy by Nighty by Night

SKA- DDishes