1. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) Observation Runs of TAMA300 Gravitational Wave Detector Masaki Ando Dept. of Physics, University of Tokyo TAMA collaboration Coalescence of a binary neutron stars Illustration/ KAGAYA

2. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)2 Abstract Japanese activities for GW detection TAMA 7 year project (April 1995 – March 2002) Construct a 300m interferometric detector : TAMA300 Several data taking runs from 1999 Data analysis results Next project : LCGT 3km cryogenic interferometer at Kamioka mine Research and development tasks (April 2002 – March 2006)

3. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)3 Contents Introduction TAMA detector Data taking runs with TAMA Data analysis results Recent results (Data Taking 8) LCGT Overview Research and development tasks Summary

4. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)4 Introduction (1) - Gravitational-wave astronomy - Gravitational wave detectors Bar detectors - network observation Interferometric detector - finishing and starting observation Future projects on the ground and in the space

5. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)5 Gravitational waves (Coalescences of compact binaries, Stellar core collapses)  Change in distance between free masses (Strain about 10 -18 ) Introduction (2) - Detection method - Gravitational Waves Precise measurement by a laser interferometer (Mirrors behave as free masses) Michelson interferometer

6. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)6 Introduction (3) - Michelson interferometer - Michelson interferometer Detects optical-path difference caused by GWs Long arm length for higher sensitivity

7. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)7 Introduction (4) - Interferometer configuration - End mirror Photo detector Beamsplitter Some mirrors are added Sensitivity improvement Power-recycled Fabry-Perot-Michelson interferometer (LIGO, VIRGO, TAMA) Fabry-Perot cavity Effective arm length Power recycling Enhance power in the interferometer Front mirror Recycling mirror Fabry-Perot cavity Laser source

8. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)8 TAMA project (1) - overview - TAMA project Detect gravitational waves from local group of our galaxy Research and development for a large-scale detector Construct an interferometer named TAMA300 Fabry-Perot-Michelson interferometer with 300m arms (with power recycling) Target sensitivity h : 3x10 -21 Aerial photograph of the TAMA site (NAOJ, Mitaka, Tokyo, JAPAN) 300m

9. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)9 TAMA project (2) - Noise budget of TAMA300 - Target sensitivity

10. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)10 TAMA project (3) - Photos - Fused silica mirror Mirror suspension 300m vacuum duct Laser RMMCBS FM2 FM1 Center room

11. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)11 Data taking runs (1) - Data taking runs with TAMA300 - Data TakingObjective Observation time Typical strain noise level Total data (Longest lock) DT1August, 1999Calibration test1 night3x10 -19 /Hz 1/2 10 hours (7.7 hours) DT2 September, 1999 First Observation run3 nights3x10 -20 /Hz 1/2 31 hours DT3April, 2000 Observation with improved sensitivity 3 nights1x10 -20 /Hz 1/2 13 hours DT4 Aug.-Sept., 2000 100 hours' observation data 2 weeks (night-time operation) 1x10 -20 /Hz 1/2 (typical) 167 hours (12.8 hours) DT5March, 2001 100 hours' observation with high duty cycle 1 week (whole-day operation) 1.7x10 -20 /Hz 1/2 (LF improvement) 111 hours DT6 Aug.-Sept., 2001 1000 hours' observation 50 days5x10 -21 /Hz 1/2 1038 hours (22.0 hours) DT7 Aug.-Sept., 2002 Full operation with Power recycling 2 days25 hours DT8 Feb.-April., 2003 1000 hours Coincidence 2 months3x10 -21 /Hz 1/2 1157 hours (20.5 hours)

12. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)12 Data taking runs (2) - DT6 observation summary - TAMA data taking 6 (DT6) 50 days’ observation (August 1 – September 20, 2001) Phase I configuration (without power recycling) Sufficient sensitivity and stability for GW events in our Galaxy SNR of 30 for 1.4-1.4 M solar inspirals Observation : 1038 hours (86.5%) Well-organized observation Automatic lock of the detector Online monitor and diagnosis 65 shift participants (2 person / 8 hours’ shift)

13. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)13 Data taking runs (3) - Detector operation status in DT6 - Operation status calendar Total observation : 1038 hours Typhoon Laser instability Measurement+adjustment Human error

14. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)14 Data Analysis results (1) - TAMA data analysis - GW search Binary inspiral search Two step search Binary inspiral search using Wavelet TAMA-LISM coincidence Continuous wave from known pulsar Burst wave search BH ringdown search, Stochastic background search, etc. Detector characterization analysis Calibration Noise veto analysis Interferometer diagnosis

15. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)15 Data Analysis results (2) - Binary inspiral search - Binary inspiral event search Matched filtering Prepare templates (predicted waveform) Expected SNR for binary mergers Distance: 10kpc (Galactic center) DT6 noise spectrum SNR : about 30 (1.4/1.4 M solar binaries)

16. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)16 Data Analysis results (3) - Search results - Matched filtering analysis DT6 1038 hours’ data 1.0-2.0 M solar events (200-1000 templates)  2 event selection No GW event Simulation Assumed Galactic source distribution DT6 detector direction Detection efficiency: 23% Upper limit Galactic event rate: 0.0095 events/hour (C.L. 90%)  10 -6 events/year (prediction)

17. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)17 Data taking 8 (1) -Data taking runs with TAMA300 - Data TakingObjective Observation time Typical strain noise level Total data (Longest lock) DT1August, 1999Calibration test1 night3x10 -19 /Hz 1/2 10 hours (7.7 hours) DT2 September, 1999 First Observation run3 nights3x10 -20 /Hz 1/2 31 hours DT3April, 2000 Observation with improved sensitivity 3 nights1x10 -20 /Hz 1/2 13 hours DT4 Aug.-Sept., 2000 100 hours' observation data 2 weeks (night-time operation) 1x10 -20 /Hz 1/2 (typical) 167 hours (12.8 hours) DT5March, 2001 100 hours' observation with high duty cycle 1 week (whole-day operation) 1.7x10 -20 /Hz 1/2 (LF improvement) 111 hours DT6 Aug.-Sept., 2001 1000 hours' observation 50 days5x10 -21 /Hz 1/2 1038 hours (22.0 hours) DT7 Aug.-Sept., 2002 Full operation with Power recycling 2 days25 hours DT8 Feb.-April., 2003 1000 hours Coincidence 2 months3x10 -21 /Hz ½ 1157 hours (20.5 hours)

18. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)18 Data taking 8 (2) - DT8 observation summary - TAMA data taking 8 (DT8) 2 month’ observation (February 14 – April 15, 2003) Full configuration (with power recycling) Sufficient sensitivity and stability for GW events in our Galaxy SNR of 40 for 1.4-1.4 M solar inspirals Observation : 1157 hours (81.3%) 94 shift participant Coincidence run LIGO (4km detector x2, 2km detector)

19. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)19 Data taking 8 (3) - Detector operation status in DT8 - Operation status calendar Total operation : 1157 hours

20. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)20 Data taking 8 (4) - Sensitivity in DT8 - Sensitivity for binary inspiral events Better than DT6 Longer obs. Time Better results Coincidence Analysis with other detectors

21. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)21 LCGT project (1) - Overview - For gravitational wave astronomy Higher sensitivity (seeing further away) More than a few events in a year 10 0 10 1 10 2 10 3 10 4 10 -19 10 -20 10 -21 10 -22 10 -23 10 -24 10 -25 Frequency [Hz] Strain sensitivity [1/Hz 1/2 ] Illustration / S.Miyoki LCGT project SNR : 10 for 230Mpc events (NS-NS inspiral)

22. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)22 LCGT project (2) - LCGT parameters - LCGT Baseline length : 3km Site: Kamioka mine Cryogenic interferometer Laser : 100W 50kg Sapphire mirror (20K, Q=10 8 ) Broadband RSE Seismic isolator : SAS (300K) Cryogenic SUS (10K, Q=2x10 8 ) Suspension point interferometer

23. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)23 LCGT project (3) - CLIO100 - CLIO100 : LCGT prototype at Kamioka mine 100m cryogenic interferometer R&D for … Mirror Suspension Cryogenics Tunnel digging finished (July 2002) Installing IFO for geo-phys

24. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)24 LCGT project (4) - Site for CLIO100 - Super Kamiokande CLIO100 Entrance

25. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)25 Summary TAMA300 Data taking runs 8 data taking runs (August 1999- ), over 2000 hours of data Data analysis Upper limit for Galactic binary inspirals : 0.0095 /hour Coincidence analysis, burst wave, continuous wave Data taking 8 : February 14 - April 15, 2003 just finished Better results will be obtained Collaboration with other detectors For LCGT R&D tasks --- TAMA300 and CLIO100 Design document

26. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)26

27. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)27 Introduction (2) - Gravitational-wave astronomy - Gravitational waves (Ripples of space time) Gravitational-wave astronomy New window for astronomy and cosmology A.Einstein Predicted by General Relativity --- Strain of space-time which propagates at the speed of the light (A.Einstein, 1916) Existence was proved by observation of a binary pulsar (J.H.Taylor, et.al, 1979) Generated by acceraration of masses (  Electro-Magnetic waves ： acceraration of charges) High transmissivity (Small cross section with matters) Accumulated shift [s] Time [year]

28. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)28 TAMA project (1) - Optical and control configuration -

29. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)29 TAMA project (1) - Data acquisition and analysis -

30. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)30 TAMA project (1) - Basic design of TAMA300 - Main interferometer Fabry-Perot-Michelson with power recycling Arm cavity length :300m Finesse of arm cavities :516 Light sourceLD-pumped Nd:YAG laser Output power : Wavelength : 10W 1064 nm Mode cleanerTriangle ring cavity Baseline length : Finesse : 9.75m 1700 Vibration isolation Three-stage stack + Double pendulum + Active isolation system Vibration isolation ratio :< -165 dB Data acquisition16 bit, 20 kHz sample, 8 channels, 160 low-freqency channels Vacuum system< 10 -6 Pa

31. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)31 Data Analysis results (3) --- Burst wave search --- Burst GW event search (M.Ando, et.al. ） Poorly predicted waveform Cannot use matched-filtering scheme Masked with non-Gaussian noises Excess power detection Time-scale selection Gaussianity Excess power Reject non-Gaussian noise without rejecting GW candidates Event rate : 10 -2 /hour (1.2x10 -20 /Hz)

32. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)32 Data Analysis results (4) --- Continuous wave search --- Continuous wave search (K.Soida, M.Ando, et.al. ） Target : pulsar at SN1987A remnant (935 0.1 Hz) DT6 1038 hours’ data Threshold : 14P 0 (False alarm: 2.6%) No GW signal, h upperlimit : 3.4x10 -23 (Preliminary: fixed spindown param.)

33. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)33 Data taking 8 (4) - Noise level at DT8 -

34. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)34 TAMA current status (1) --- Improvements after DT6 --- Power recycling (TAMA Phase II) Mirror installation : November, 2001 First lock : Dec. 24, 2001 Harmonic demodulation for RM control Longest lock : 4 hours Recycling gain : 4 (Low gain configuration) Improved noise level Shot noise Detector noise level Scattered light noise Frequency stabilization (K.Arai, R.Takahashi S.Sato, et.al.)

35. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)35 TAMA current status (2) --- Current noise level --- Latest noise level Improved with power recycling (and the other efforts) h : 4x10 -21 /Hz 1/2 around 1kHz DT7 (Aug.31-Sept.1) Improvement factor of 3

36. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)36 Data taking runs (1) --- Noise level at DT6 --- DT6 noise level h : 5x10 -21 /Hz 1/2 at 1kHz Noise sources are identified Alignment control noise Michelson phase noise Detector noise Shot noise etc. (K.Arai, R.Takahashi, et.al.)

37. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)37 Data Analysis results (5) --- Coincidence search --- TAMA-LISM coincidence analysis for binary events (paper in preparation) (H.Takahashi, H.Tagoshi, N.Kanda, D.Tatsumi, T.Tanaka) LISM 20m detector at Kamioka mine Locked Fabry-Perot configuration Sensitivity h : 8x10 -20 /Hz 1/2 Simultaneous operation with TAMA DT6: 709 hours Compare candidate event list 244 hours of commonly lock data. Check parameter consistency 1. Significant reduction of fake event rate. 2. Number of survived events : Consistent with the accidental coincident rate. 3. Upper limit to the Galactic event rate within 1kpc : 0.064/hours (1.0-2.0 M solar )

38. XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)38 Data taking 8 (5) - Stability of sensitivity in DT8 - Sensitivity distribution