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LCGT Collaborators ICRR, Univ. of Tokyo ERI, Univ. of Tokyo KEK AIST NAOJ ECU GSFS, Univ. of Tokyo

CLIO Introduction and Overview Masatake Ohashi, Shinji Miyoki & CLIO, LCGT Collaborators (ICRR Univ. of Tokyo, Japan Science and Technology Association) GWADW 2010, Kyoto Hearton Hotel, Kyoto, Japan May 17th 2010. LCGT Collaborators ICRR, Univ. of Tokyo ERI, Univ. of Tokyo KEK AIST

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LCGT Collaborators ICRR, Univ. of Tokyo ERI, Univ. of Tokyo KEK AIST NAOJ ECU GSFS, Univ. of Tokyo

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  1. CLIOIntroduction and Overview Masatake Ohashi, Shinji Miyoki & CLIO, LCGT Collaborators (ICRR Univ. of Tokyo, Japan Science and Technology Association) GWADW 2010, Kyoto Hearton Hotel, Kyoto, Japan May 17th 2010 LCGT Collaborators ICRR, Univ. of Tokyo ERI, Univ. of Tokyo KEK AIST NAOJ ECU GSFS, Univ. of Tokyo Phys, Kyoto Univ. Yukawa, Kyoto Univ. DPRI, Kyoto Univ. Phys. Univ. of Tokyo Osaka Univ. Nagaoka TS Univ. Osaka City Univ. Hiroshima Univ. Tohoku Univ. Hirosaki Univ. Hosei Univ. NICT Japan Ochanomizu Woman Univ. Nihon Univ. Niigata Univ. Rikkyo Univ. Waseda Univ. Ryukyu Univ. MPQ, Germany AEI, Germany Caltech, USA Univ. of Western Australia Louisiana State Univ. USA Rochester, USA BNU, China IHEP, China UST, China PMO, China IUCAA, Moscow Univ. EGO/LAPP China Science Technology Univ. NRMN, Taiwan Maryland Univ. USA Univ. of Birmingham, UK

  2. GW Development in JAPAN GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  3. CLIO Features • 100m base-line Unrecombined Fabry-Perot Michelson Proto-Type for LCGTset in the Kamioka mine. • Technical combination of products of • - CLIK(2000-02) for cryogenic system development • - LISM(1999-2002) forUnderground IFO characterization • - Ultra low vibration PT • refrigerator developments • at KEK(2004-2006) • Demonstrate an improvement • of sensitivity by reduction • of the mirror and suspension • thermal noise • using mirror cooling technique. GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  4. CLIO Site • 220km away from Tokyo • 1000m underground from the top of the mountain. (Near Super Kamiokande) • 360m altitude • Hard rock of Hida gneiss • (5 [km/sec] sound speed) Landsat photo data NASA altitude data Cashmir 3D GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  5. Tour to CLIO GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  6. Underground for GW Detectors- stable environment - GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  7. Continuous operation of LISM(2002) and CLIO MC (2006) Observation period : 8/1-8/23, 9/3-9/17 Total observation time : 862h Total lock : 786h Longest stretch of lock : 72h Record:170h in 2001spring Live rate : 91% (99.8% for last 1week) Without Wave Front Sensing CLIO one of steering mirrors alignment noise. GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  8. Thermal Noise Reduction by Cooling- sapphire substrate and fibers for cooling, CLIK - • The first cryostat prototype using GM refrigerators and two radiation shields structure with holes exposed to 300K area for thermal radiation estimation check. • 7m base-line cryogenic Fabry-Perot Cavity : CLIK • ,where f10cm x t6cm sapphire mirrors produced by Crystal Systems, polished by Canon, and coated by Japan Aviation Electronics. - Sapphire substrate Q check at 20 K - Temperature distribution check. Sapphire fiber heat transfer check. Later, the thermal radiation estimation miss-understanding was revised through CLIO and CLIK experiment. GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  9. Thermal Noise Reduction by Cooling- refrigerators, cryostat, magnet problems, etc - Refrigerator structure Refrigerator outlook Cooling Power Vibration reduction GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  10. Thermal Noise Reduction by Cooling- refrigerators, cryostat, magnet problems, etc - GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  11. Displacement in November 2008- Almost thermal noise limited at 300K condition- CLIO displacement touched the predicted thermal noise levels. - Sapphire mirror thermoelastic noise (80Hz~250Hz) Green Line - Suspension thermal noise (20Hz-80Hz) Blue Line GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  12. Noise Budget GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  13. Suspension thermal noise reduction- detailed in Miyakawa’s talk- ♦Suspension wires are pure aluminum, not sapphire fibers. ♦ “Suspension thermal noise” was decreased, as the aluminum wires were cooled (251K -> 225K ->91K) (Green, Black, Red ) GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

  14. Mirror Thermo-elastic Noise Reduction- detailed in Uchiyama’s Talk - • ♦Only two input mirrors were cooled, accounting for smaller spot size on these mirrors. • ♦ According to noise budget verification, main noise contributions are … • Shot noise • Suspension thermal noise • Mirror thermo-elastic noise • ♦Sapphire mirror thermo-elastic noise reduction seems to contribute the displacement noise improvement around 200Hz. Estimated mirror thermal noise (300K) Estimated mirror thermal noise (~15K) GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010) 14

  15. Summary • The CLIO has finally demonstrated the sapphire mirrors thermo-elastic noise and Al wires’ suspension thermal noise reduction at around 10-19 [m/rHz] displacement lever around 100Hz. • Please see Uchiyama’s, Miyakawa’s and Siaito’s talk today and tomorrow for details. GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

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