Andrew Faulkner University of Manchester Jodrell Bank Observatory

1. Andrew Faulkner University of Manchester Jodrell Bank Observatory

2. RadioNet Partners & Mission Support and enhance European radio astronomy • RadioNethas 20 partners: • major radio astronomy facilities • technology development laboratories • RadioNetwas awarded €12.4M • Based on 25 years of cooperation in the European VLBI Network. • Coordinated by Univ. of Manchester, UK

3. RadioNet 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...

4. The Telescopes Europe has some of the largest, most sophisticated radio telescopes on Earth. These facilities are working together very closely as part of RadioNet In 2004: TNA programme delivered 4200 hours of access; 40% of time went to new users.

5. Radio Astronomy & Gravity Waves Verification Sources Detection

6. Hulse & Taylor (1974) Radio Astronomy & Gravity Waves Double neutron star binaries Verification Sources Detection Weisberg & Taylor (priv. comm) Orbit shrinks 1cm every day Confirmation of existence of gravitational waves

7. Testing GR: Kramer et al.(2004) Radio Astronomy & Gravity Waves The Double Pulsar Verification Sources Detection Pb=2.4 hrs, d/dt=17 deg/yr vel ~ 0.1% c Mass B (MSun) 0 0.5 1 1.5 2 0 0.5 1 1.5 2 Mass A (MSun)

8. Radio Astronomy & Gravity Waves Coalescence Rate of NS binaries Verification Sources Detection Discovery of the Double Pulsar dramatically increases predicted, observable coalescence rates: Ligo I Ligo II ref. 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 Events per year (95% confidence)

9. LIGO Consortium, Kramer & Lyne (2005) Radio Astronomy & Gravity Waves See solitary & binary Neutron Stars Verification Sources Detection Look for Gravity Waves of known ephemeris from solitary Pulsars LISA should observe GW from the Double Pulsar directly: ~2x10-4 Hz

10. Radio Astronomy & Gravity Waves Polarisation in the CMB Verification Sources Detection B-mode signature of gravitational waves… ….. ‘smoking gun’ of inflation

11. Log10 (Ωg(f)h2) -16 -14 -12 -10 -8 -6 -15 -10 -5 0 5 10 Log10 (f/Hz) Radio Astronomy & Gravity Waves PTA Verification Sources Detection Pulsar Timing Array Look for global spatial pattern in pulsar timing residuals Millisecond pulsars act as arms of huge detector Complementary in frequency with LISA and LIGO/VIRGO

12. The Square Kilometre Array

13. The 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

14. Phased Arrays of receivers Aperture Arrays “electronic fish-eye lens” Focal Plane Arrays “radio cameras” The revolution in radio telescopes

15. SKA Demonstrators KAT & xNTD • Collaboration • 2 teams building similar systems: • Australia xNTD • South Africa KAT • Test bed for phased arraytechnology • KAT/xNTDAims • Science delivery • Technology demonstrationHardware & software • Test possible SKA site • Attract the full SKA • Description • 20 x 15m Dishes • 0.7 – 1.75 GHz • Fitted with phased FPAs • FOV 50 deg2 • Baselines <10Km • Completion 2009

16. ‘1% SKA’ Science Legal Entity Formed ‘Hydrogen Array’ Wilkinson 1991 { SKA Complete SKADS start SKADS report ‘10% SKA’ Science SKADS Mid-review Working Group ISSC MoU Science Case pub. Site Selection …… { { 92 96 0405 06 07 08 09 1014 18 22 { { 2000 { { { SKA system defined Phase 2 Build 50% SKA SKA concept Concept exposition Design & Build Demonstrators KAT & xNTD 1% SKA Phase 1 Build 10% SKA Phase 3 Build 100% SKA Now SKA Timeline

17. 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….

18. Summary Radio Astronomy makes complementary GW observations New technology will revolutionise Radio Astronomy RadioNetbrings coherence to European RA teams Opportunity for a joint FP7 funded science program? ILIAS-GW and RadioNet can make a great team in Fundamental Physics!

20. 3 JRAs: all running on time and on budget. Developing future technology and software for radio astronomy.

21. Networking 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.

22. KKL - 1992 KKLB+ - 1993 8 180 Note KKLB+ model accounts for fainter pulsars – so rate increased by ~3.2x

23. 0737inc rate by 6-7 times 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) 1 per 13 years Daily!! * Using model from KKL