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LCGT Project Status

LCGT Project Status. EGO-ICRR Meeting 4 October 2011 @ University of Tokyo Seiji Kawamura (ICRR). Objectives of LCGT. Detect gravitational waves together with Virgo and LIGO for the first time Establish Gravitational W ave Astronomy

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LCGT Project Status

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  1. LCGT Project Status EGO-ICRR Meeting 4 October 2011 @ University of Tokyo Seiji Kawamura (ICRR)

  2. Objectives of LCGT • Detect gravitational waves together with Virgo and LIGO for the first time • Establish Gravitational Wave Astronomy • Establish multi-messenger observations between GWs and Electromagnetic waves/Cosmic rays

  3. Expected GW sources • Neutron star binary coalescence • correlation with GRB • Black hole binary coalescence • Black hole ringdown • Supernovae • Correlation with Neutrino • Pulsar • Early universe • Unknown

  4. Key Features of LCGT Underground Cryogenic mirrors/ suspensions These are essential features for the 3rd GW detectors such as ET.

  5. Underground Site We are here.

  6. Ground motion inKamioka mine

  7. Advantage of Underground Site • Not only linear effect • But also nonlinear effect Smaller low-frequency motion of mirror  Lower gain of control system necessary  Lower in-band noise imposed by control system

  8. Sensitivity Comparison 20m prototype was moved from Tokyo to Kamiokain 1998. @ Tokyo Displacement spectrum m/RHz @ Kamioka Hz

  9. Cryogenics System Inner Wall (8K) Platform (14 K) Upper Mass (15 K) Mirror (20 K) Flexible Heat Link Baffles Thermal Shield Pulse Tube Cryocooler

  10. Sapphire Mirror Sapphire mirror at 20 K • Transparent at 1064 nm • Low thermal noise • High Quality factor at 20 K • Low thermoelastic noise • High thermal conductivity at 20 K • Low thermal expansion coefficient at 20 K

  11. Seismic Attenuation System (SAS) for LCGT Tunnel (2nd floor) Chamber Inverted Pendulum GAS Filter (invented by DeSalvo) Tunnel (1st floor) Chamber Mirror SAS was designed based on the Virgo SA.

  12. Goal Sensitivity of LCGT

  13. External Review • Feb. 28 – Mar. 4, 2011 @ICRR • Almost all the subsystems were reviewed • Review items: • Requirements • Design • Schedule • Prototype test plan • Etc.

  14. Reviewers

  15. Report • We obtained report on March 10, 2011 • 12 pages • Consists of: • Executive summary • Recommendations to management • Recommendations to each subsystem

  16. Executive Summary 1 focusing interferometer noise optimization (and corresponding astrophysics goals) to capitalize on the unique advantages of the underground site and cryogenic operation Bandwidth working group (led by K. Somiya) was convened to discuss this. It turned out that shifting the frequency band lower will not gain significant advantages.

  17. Executive Summary 2 establishing a strong Systems group to insure subsystem interfaces and design goals are properly distributed, and sufficient, but not excessive Systems Engineering Office has been created.

  18. Executive Summary 4 & 5 wherever feasible, employing (or at least starting with) established, tested component designs requiring minimal modification; proceeding rapidly toward integrated system testing (e.g., through enhanced scope for the iLCGT phase) to minimize the risk of late surprises Roadmap working group (led by M. Ando) was convened to discuss this. We decided to employ a simple isolation system for iLCGTand meanwhile to develop SAS at the site.

  19. Program Advisory Board • Jun. 21 – 22, 2011 @ICRR • Review items: • Management • Schedule • Design • Etc.

  20. Reviewers

  21. Report • We obtained report on August 30, 2011 • 6 pages • Consists of responses to the following points: • If the management and organization of the project are OK. • If the construction status & plan are OK. • If the scientific goals are reasonable. • What should be improved in the LCGT construction? • Whatever the advice for this project. • Actions: • We have started discussing possible actions to the report.

  22. Schedule of LCGT 2011 2012 2013 2014 2015 2016 2017 bLCGT Observation iLCGT

  23. Organization of LCGT LCGT Council Director (Kajita) Program Advisory Board Systems Engineering Office (Kawamura, Ando, Miyoki, Somiya) Executive Committee ( Nakatani (PM), Kuroda, Ohashi, Kawamura, Mio, Ando) Executive Support DATA Analysis Tunnel Facility Vacuum Vibration isolation Cryogenics Mirror Main interferometer Digital system Analog Electronics Input/Output Optics Laser Auxiliary optics Geophysics Interferometer Subsystem

  24. Joining the worldwide GW network GEO-HF Advanced LIGO LCGT Advanced Virgo LCGT will join the world network of gravitational wave detectors, with full reciprocal sharing of data with the Virgo collaboration, the LIGO Collaboration and the GEO600 Collaboration at a time determined by mutual agreement of all parties - LCGT, Virgo, LIGO, and GEO.

  25. L/H+L/L+V+LCGT 50% L/H+L/L+V 50% LCGT in network • LIGO(H)+LIGO(L)+Virgo+LCGT • Max sensitivity (M.S.): +13% • Coverage at 0.5 M.S.: 100% • 3 detector duty cycle: 82% • LIGO(H)+LIGO(L)+Virgo • Coverage at 0.5 M.S.: 72% • 3 detector duty cycle: 51% B. F. Schutz

  26. Dawning of Gravitational Wave Astronomy is near! Illustration: Sora

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