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Five long and independent baselines: Better SNR and much better directional resolution

Proposal to extend current AIGO High Optical Power research facility to a 5km advanced interferometer. D G Blair on behalf of ACIGA LIGO-G060284-00-Z. Five long and independent baselines: Better SNR and much better directional resolution. Why is AIGO necessary. Increased angular resolution :

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Five long and independent baselines: Better SNR and much better directional resolution

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  1. Proposal to extend current AIGO High Optical Power research facility to a 5km advanced interferometer. D G Blair on behalf of ACIGA LIGO-G060284-00-Z

  2. Five long and independent baselines: Better SNR and much better directional resolution

  3. Why is AIGO necessary • Increased angular resolution : • average x 4 • sometimes much more • Coherent array analysis • increases the number of detectable sources x ~2 • Reduced Accidental coincidences • reduces as number of independent baselines to power N

  4. Improved angular resolution with AIGO • LIGO, VIRGO and AIGO • LIGO and VIRGO

  5. The Process So Far • Gingin facility development 2000-2005 • Western Australia funds Centre of Excellence for gravitational astronomy 2005 • AIGO Planning meeting Oct 2005: concept for reduced pipe diameter. • WA Govt forms Steering Committee for AIGO Nov 2005. • International Letter Writing Nov 2005…thanks!! • UWA and State Govt fund prospectus document Dec 2005 and planning process May 2006. • ACIGA costing and planning:(LIGO support through Adv LIGO review) May 2006.

  6. Gingin facility Investment • Clean rooms and assembly facilities • Vacuum system and vacuum automation • High optical power laser facilities • Seismic surveying demonstrating excellent seismic attenuation. • Roads and power infrastructure. • Total investment so far ~ $20M

  7. AIGO Concept • AIGO: I for International • An Advanced detector built using maximum knowhow, support and contribution from northern hemisphere detectors. • A detector planned and advised internationally. • Utilising the best aspects of all detectors built to date, combined with certain innovative features. • A detector that will feed data directly into the international data analysis grid.

  8. AIGO Realities • Funds ~ $40m thought to be possible in Australia • Funds ~$10m available soon for pipe infrastructure. • Substantial data analysis effort funded separately. • Can we build an advanced detector for such a small sum? • Not without international support • Control systems • Designs • Monitoring • Expertise in many areas • Advisory committees

  9. AIGO Preliminary Concept • 5km, 700mm diameter vacuum pipe (de Salvo) • keyhole welding, precision weld monitoring (CSIRO) • on site fabrication of pipe in long lengths (Duraduct) • spiral band saw baffle fabricated with pipe.(de Salvo,Duraduct) • Low mass enclosure, solar bakeout. (VACUUM 44: 2,151-154 ( 1993)).

  10. Light Scattering Noise (Takahashi) • Modelling based on R Takahashi et al PRD 70,06,2003 • Number of effective baffles N:h=height of baffle,d=baffle spacing Spiral baffle represents significant overkill

  11. Why 5km • Arm length dilutes test mass thermal noise. • Thermal noise penalty for parametric instability suppression by ring damping. • Adv LIGO proposed performance can be regained with extra arm length.

  12. Strong Thermal Lensing Observation and compensation (PRL accepted 2006)

  13. Parametric Instability (PRL2005) Stabilisation requires ring damping: extra thermal noise. (see Ju Li’s talk)

  14. Consortium About 70 people 7 AustralianUniversities 2 CSIRO Institutes 2 Companies

  15. Conclusion • AIGO offers significant benefit to existing terrestrial detectors. • Natural next step for world network. • Can be achieved over next 8 years with community support. • We would like to sign MOUs with organisations such as VESF

  16. Input Test Mass R1 =  Thermal compensation Cavity Waist Position Heat the compensation plate Thermal Gradient: Jerome Degallaix

  17. Demonstrated Thermal Compensation

  18. Gingin prediction, Fused Silica

  19. Gingin prediction, Sapphire

  20. Astro-ph/061275 Short GRB and binary black hole standard sirens as a probe of dark energy Authors: Neal Dalal (CITA), Daniel E. Holz (LANL and U. Chicago), Scott A. Hughes (MIT), Bhuvnesh Jain (U. Penn.) Comments: 8 pages, submitted to PRD Short gamma-ray bursts, if produced by merging neutron star binaries, would be standard sirens with known redshifts detectable by ground-based GW networks such as LIGO-II, Virgo, and AIGO. Depending upon the collimation of these GRBs, a single year of observation of their gravitational waves can measure the Hubble constant to about 2%. When combined with measurement of the absolute distance to the last scattering surface of the cosmic microwave background, this determines the dark energy equation of state parameter w to 9%.

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