LCGTCollaborators

ICRR, Univ. of TokyoERI, Univ. of TokyoKEKAISTNAOJECUGSFS, Univ. of TokyoPhys, Kyoto Univ.Yukawa, Kyoto Univ.DPRI, Kyoto Univ.Phys. Univ. of TokyoOsaka Univ.Nagaoka TS Univ.Osaka City Univ.Hiroshima Univ.Tohoku Univ.Hirosaki Univ.Hosei Univ.NICT JapanOchanomizu Woman Univ.Nihon Univ.Niigata Univ.Rikkyo Univ.Waseda Univ.Ryukyu Univ.MPQ, GermanyAEI, GermanyCaltech, USAUniv. of Western AustraliaLouisiana State Univ. USARochester, USABNU, ChinaIHEP, ChinaUST, ChinaPMO, ChinaIUCAA, Moscow Univ.EGO/LAPPChina Science Technology Univ.NRMN, TaiwanMaryland Univ. USAUniv. of Birmingham, UK

CLIO Introduction and OverviewMasatake Ohashi, Shinji Miyoki & CLIO, LCGT Masatake Ohashi, Shinji Miyoki & CLIO, LCGT CollaboratorsCollaborators(ICRR Univ. of Tokyo, Japan Science and Technology Association)(ICRR Univ. of Tokyo, Japan Science and Technology Association)GWADW 2010, Kyoto Hearton Hotel,Kyoto, JapanMay 17th 2010May 17th 2010

GW Development in JAPAN

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

CLIO Features 100m base-line Unrecombined Fabry-Perot Michelson Proto-Type for LCGT set in the Kamioka mine.

Technical combination of products of- CLIK(2000-02) for cryogenic system development- LISM(1999-2002) for Underground 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)

Frequency [Hz]100 1K10 10K

10-21

10-20

10-19

10-18

10-17

10-16

Shot Noise

Suspension Thermal Noise@300KMirror Thermal Noise@300K

SQL

Total@300K

Total@20K

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

CLIO Site220km 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 dataNASA altitude dataCashmir 3D

Tour to CLIO

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

Underground for GW Detectors- stable environment -

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

Continuous operation of LISM(2002) and CLIO MC (2006)

Observation period : 8/1-8/23, 9/3-9/17Total observation time : 862hTotal lock : 786hLongest stretch of lock : 72h

Record:170h in 2001springLive rate : 91% (99.8% for last 1week)Without Wave Front Sensing

CLIO one of steering mirrors alignment noise.

Thermal Noise Reduction by Cooling

- sapphire substrate and fibers for cooling, CLIK -

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

- Sapphire substrate Q check at 20 K- Temperature distribution check.

Sapphire fiber heat transfer check.

-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 10cm x t6cm sapphire mirrors produced by Crystal Systems, polished by Canon, and coated by Japan Aviation Electronics.

Later, the thermal radiation estimation miss-understanding was revised through CLIO and CLIK experiment.

Thermal Noise Reduction by Cooling

- refrigerators, cryostat, magnet problems, etc -

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

1st Stage 2nd Stage

Reduction Stage

41.2K 4.15K

43.7K 4.43K@15W @0.5W

Original Cooling Head

Refrigerator structure

Refrigerator outlook

Cooling Power

Vibration reduction

Thermal Noise Reduction by Cooling

- refrigerators, cryostat, magnet problems, etc -

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

Displacement in November 2008

- Almost thermal noise limited at 300K condition-

CLIO displacement touched thepredicted 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)

Noise Budget

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

Suspension thermal noise reduction

- detailed in Miyakawa’s talk-

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

♦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 )

Mirror Thermo-elastic Noise Reduction- detailed in Uchiyama’s Talk -

GWADW2010, Kyoto Hearton Hotel, Kyoto, (May 16th 2010)

Estimated mirror thermal noise (300K)Estimated mirror thermal noise (~15K)

♦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.

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)