Setting the stage GWADW2010, Kyoto

1. Setting the stageGWADW2010, Kyoto Francesco Fidecaro Pisa GWADW2010 - Kyoto

2. Recent progress in gravitational wave research • With input from • Rana Adhikari • Matt Evans • Hartmut Grote • Kazuaki Kuroda • David Shoemaker • Didier Verkindt • Stefano Vitale • Work of many • Data taking by current detectors (S6/VSR2) and analysis of large datasets • Network of interferometers in coincidence <-> em and n observatories • Theoretical study of sources • A new promising entry: Pulsar timing (not covered this time) • Ongoing projects for Advanced Detectors and space • Cryogeny, thermal noise, mechanical noise, underground-> third generation • Endless spiral: Research, development, construction, tests, measurements, models, simulation GWADW2010 - Kyoto

3. Analysis of 6 months of coincidence data between LHO, LLO and Virgo • Data quality: the noise curve is the beginning of the story, not the end! Virgo Omega triggers in 107 seconds 1 s coincidence -> 10 ev Triples? -> 0.01 ev GWADW2010 - Kyoto O(104) SNR>8 triggers

4. 10 nrad rms https://pub3.ego-gw.it/itf/tds/file.php?callFile=VIR-0123A-10.pdf GWADW2010 - Kyoto

5. GWADW2010 - Kyoto

6. Signalled by Jay Marx GWADW2010 - Kyoto

7. Direct and indirect origins for strong contributions to noise • In random order: • Large beams • High intensity • Thermal effects • Position, angular noise (rms) • Optical design • Poor or missing error signals • Beam halo, stray, diffused light • Creep and the like • End up in different approaches (all will be working, with trade offs) • It is a little bit like having to choose between… GWADW2010 - Kyoto

8. GWADW2010 - Kyoto

9. GWADW2010 - Kyoto

10. ALIA ASTROD-GW DECIGO Current launch date 2012 Q1 GWADW2010 - Kyoto

11. Light and heat • Compensation of thermal distortions: significant complication introduced (TCS, managing higher modes) • Can we go around high light intensity? • Warm mirrors and suspensions have thermal noise • The direct way: cool them (CLIO, LCGT, …) • Or reduce internal dissipation • Or both • In any case, need to address material properties • New ideas? GWADW2010 - Kyoto

12. Alignment • Longitudinal noise is not the end of the story • Angular control comes in, becomes more difficult with high power and broad beams • Engineered-in since the beginning? GWADW2010 - Kyoto

13. Simulation after first generation • Now is a Must have • Optical, frequency domain, time domain • We know better how to ask questions aiming at lock acquisition, noise coupling • Need to introduce imperfections, which ones? • How to simulate non stationarity? GWADW2010 - Kyoto

14. Entering the advanced detector era • Long run • Not only knowledge but also skills to be acquired and maintained: • Teaching the art • Managing these bright minds • Thinking • Built-in reliability: • hw and core sw at the same level • Cleanliness • QC • Prototype and test as much as possible • Manage centrifugal forces: • Missing real astrophysical data • New detector instead of routine construction and debugging GWADW2010 - Kyoto

15. Squeezed states of light • “As a positive thing one might see that squeezing may arrive earlier than anticipated in the past” Hartmut Grote • Be prepared... GWADW2010 - Kyoto

16. Photo Courtesy H. Grote GWADW2010 - Kyoto

17. A stimulating program • Expertise is building, experience accumulates • Experiments are made • Codes are run • Third generation takes shape • Progress is made on all fronts, our detectors will be better than ever • Thank you Syd and convenors for putting it together, and our warmest wishes! • But there was a starter: Kamioka mountain GWADW2010 - Kyoto

18. CLIO/KS tour: very interesting Location of ＣＬＩＯ／LCGT LCGT is planned to be built underground at Kamioka, where the prototype CLIO detector is placed. Effort headed by the Director of ICRR Takaaki Kajita. GWADW2010 - Kyoto