Andrew Faulkner

University of Manchester Jodrell Bank Observatory

• RadioNet has 20 partners: – major radio astronomy facilities

– technology development laboratories

• RadioNet was awarded €12.4M

• Based on 25 years of cooperation in the European VLBI Network.

• Coordinated by Univ. of Manchester, UK

Support and enhance European radio astronomy

RadioRadioNetNet Partners & Mission Partners & Mission

RadioRadioNetNet Objectives Objectives

• European access to world-class facilities

• Enhance facilities with an integrated R&D programme

• Greater collaboration in engineering, software and science

• Train & nurture next generation of astronomers and engineers

• A common and unified approach to user support

• Prepare for next generation of radio instruments:

• Strengthen European astronomy via close links with

ILIAS, OPTICON, EUROPLANET...

Europe has some of the largest, most sophisticated radio telescopes on Earth.

These facilities are working together very closely as part of RadioNet

The TelescopesThe Telescopes

In 2004: TNA programme delivered 4200 hours of access; 40% of time went to new users.

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection

Weisberg & Taylor (priv. comm)

Orbit shrinks 1cm every day

Confirmation of existence of gravitational waves

Hulse & Taylor (1974)

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection

0 0.5 1 1.5 2

Mass A (MSun)

002.0000.1exp

obs

s

sTesting GR:

Kramer et al.(2004)

Pb=2.4 hrs, d/dt=17 deg/yr

vel ~ 0.1% c

M

ass

B (

MS

un)

0

0

.5

1

1

.5

2

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection

2001 0.0003 – 0.25 2 – 1300 Kalogera et al. 2001

2002 0.001 – 0.03 4 – 140 Kim et al. 2002

2003 0.004 – 0.2 20 – 1000 Kalogera et al. 2003

Ligo I Ligo II ref.

Events per year (95% confidence)

Discovery of the Double Pulsar dramatically increasespredicted, observable coalescence rates:

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection

LIGO Consortium, Kramer & Lyne (2005)

Look for Gravity Waves of known ephemeris from solitary Pulsars

LISA should observe GW from the Double Pulsar directly: ~2x10-4 Hz

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection

B-mode signature of gravitational waves… ….. ‘smoking gun’ of inflation

Radio Astronomy & Gravity WavesRadio Astronomy & Gravity Waves

Verification

Sources

Detection-15 -10 -5 0 5 10 Log10 (f/Hz)

Lo

g 10 (

Ωg(f

)h2)

-16

-

14

-1

2

-1

0

-8

-6

Millisecond pulsarsact as arms ofhuge detector

Complementary in frequency with LISA and LIGO/VIRGO

Look for global spatial pattern in pulsar timing residuals

The Square Kilometre ArrayThe Square Kilometre Array

• Next generation radio telescope• Frequency range 0.15 - 25 GHz• Collecting area of 106 m2

• >50x sensitivity & >105 survey speed of today's best instruments

• A ‘discovery’ instrument

• Internationally co-ordinated• Europe in SKADS is developing:

– technology for 0.15 - 2 GHz – large field-of-view– multiple beams

The Square Kilometre ArrayThe Square Kilometre Array

Phased Arrays of receiversPhased Arrays of receivers

The revolution in radio telescopesThe revolution in radio telescopes

Aperture Arrays“electronic fish-eye lens”

Focal Plane Arrays“radio cameras”

SKA Demonstrators SKA Demonstrators KAT & xNTDKAT & xNTD

Description•20 x 15m Dishes•0.7 – 1.75 GHz•Fitted with phased FPAs•FOV 50 deg2

•Baselines <10Km•Completion 2009

KAT/xNTD Aims•Science delivery•Technology demonstration

Hardware & software

•Test possible SKA site•Attract the full SKA

Collaboration•2 teams building similar systems:

• Australia xNTD• South Africa KAT

•Test bed for phased array technology

SKA TimelineSKA Timeline

92 96 04 05 06 07 08 09 10 14 18 22

SKADSstart

SKADSreport

SKAconcept

WorkingGroup

Phase 2Build

50% SKA

Phase 3Build

100% SKA

SKAComplete

Now

Design & Build Demonstrators

KAT & xNTD1% SKA

Phase 1Build

10% SKA

‘10% SKA’Science

‘1% SKA’Science

……ISSCMoU

SiteSelection

ScienceCase pub.

Conceptexposition

‘Hydrogen Array’Wilkinson 1991

LegalEntity

Formed

2000

SKA systemdefined

SKADSMid-review

The SKA will….The SKA will….

• Improve timing of pulsars 100 fold

• Discover all the pulsars in the Galaxy

• Find the elusive Black hole-Pulsar binary

• Detect MBH-MBH binary GWs

• Hydrogen survey of all Galaxies to z ~2

• Fundamental neutrino research

• Detect inter-galactic magnetic fields

• Very high precision galaxy power spectrum

• ‘Cradle of life’ + planetary formation & SETI

Plus….

etc. etc….

SummarySummary

Radio Astronomy makes complementary GW observations

New technology will revolutionise Radio Astronomy

RadioRadioNetNet brings coherence to European RA teams

Opportunity for a joint FP7 funded science program?

ILIAS-GW and RadioRadioNet Net can make a great team in Fundamental Physics!

Developing future technologyand software for radioastronomy.

3 JRAs: all running on 3 JRAs: all running on time and on budget.time and on budget.

Networking ActivitiesNetworking Activities

• 8 NAs

• Range from management

to policy planning to

engineering workshops.

• In 2004 RadioNet funded

16 workshops on science,

engineering, interference,

operations and policy.

• Several hundred

astronomers and engineers

involved.

• 24 meetings planned for

next 18 months.

KKL - 1992 KKLB+ - 1993

180

8

Note KKLB+ model accounts for fainter pulsars – so rate increased by

~3.2x

The ‘Answer’*, again…

2001 0.0003 – 0.25 2 – 1300 KNST

2002 0.001 – 0.03 4 – 140 KKL

2003 0.004 – 0.2 20 – 1000 KKLB+

Ligo I Ligo II ref.

Events per year (95% confidence)

* Using model from KKL

0737 inc rate by 6-7 times

Daily!!1 per 13 years