1. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) Observation run of TAMA GW detector Masaki Ando Department of Science, University of Tokyo and the TAMA Collaboration

2. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 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 Operation with final configuration Data analysis results Next project : LCGT 3km cryogenic interferometer at Kamioka mine Research and development tasks (April 2002 – March 2006)

3. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 3 Contents TAMA Overview Data taking runs Data analysis results Current status LCGT Overview Research and development tasks

4. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 4 TAMA project (1) --- Targets of TAMA --- 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 Target sensitivity h : 3x10 -21 Aerial photograph of the TAMA site (NAOJ, Mitaka, Tokyo, JAPAN) 300m

5. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 5 TAMA project (2) --- Noise budget of TAMA300 --- Target sensitivity

6. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 6 TAMA project (3) --- 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

7. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 7 TAMA project (4) --- Photos --- Fused silica mirror Mirror suspension 300m vacuum duct Laser RMMCBS FM2 FM1 Center room

8. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 8 TAMA project (5) --- Optical and control configuration ---

9. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 9 TAMA project (6) --- Data acquisition and analysis ---

10. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 10 Data taking runs (1) --- Data taking runs with TAMA300 --- Data TakingObjective Observation time Typical strain noise level Total data (Longest lock) DT1 August, 1999 Calibration test1 night3x10 -19 /Hz 1/2 10 hours (7.7 hours) DT2 September, 1999 First Observation run 3 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 (TR1) June, 20012 days(24.8 hours) DT6 Aug.-Sept., 2001 1000 hours' observation 50 days5x10 -21 /Hz 1/2 1038 hours (22.0 hours)

11. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 11 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 Operation : 1107 hours (92.3%), longest cont. operation : 22 hours 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) Coincidence run LISM (20m detector at Kamioka mine) Simultaneous operation : 709 hours

12. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 12 Data taking runs (3) --- Detector operation status in DT6 --- Operation status calendar Total operation : 1107 hours Typhoon Laser instability Measurement+adjustment Human error

13. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 13 Data taking runs (4) --- 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.)

14. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 14 Data Analysis results (1) --- TAMA data analysis --- GW event search Binary inspiral search One step search (H.Tagoshi, D.Tatsumi, H.Takahashi) Two step search (H.Tagoshi, T.Tanaka) Binary inspiral search using Wavelet (N.Kanda) TAMA-LISM coincidence (H.Takahashi, H.Tagoshi, D.Tatsumi,…) Continuous wave from known pulsar (K.Soida, M.Ando,…) Burst wave search (M.Ando,…) BH ringdown search, Stochastic background search, etc. Detecor characterization analysis Calibration (D.Tatsumi, S.Telada,…) Noise veto analysis (Y.Watanabe, N.Kanda,…) Interferometer diagnosis (M.Ando,…)

15. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 15 Data Analysis results (2) --- Inspiral search --- Binary inspiral event search (H.Tagoshi, D.Tatsumi, N.Kanda, H.Takahashi, T.Tanaka, M.Sasaki) Expected SNR for binary mergers Distance: 10kpc (Galactic center) DT6 noise spectrum SNR : about 30 (1.4/1.4 M solar binaries)

16. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 16 --- Inspiral search (contd.) --- Matched filtering analysis (paper in preparation) DT6 1038 hours’ data 1.0-2.0 M solar events (200-1000 templates) c 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%)

17. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 17 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)

18. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 18 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.)

19. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 19 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 )

20. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 20 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.)

21. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 21 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

22. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 22 Current and future tasks --- LCGT project --- TAMA project 7years’ project (April 1995 – March 2002) 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. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 23 Current and future tasks --- Status --- Research and development for LCGT Observation runs with TAMA detector Development of cryogenic techniques 100m cryogenic interferometer : CLIO Seismic isolation system : SAS Thermal noise investigation Resonant sideband extraction, Suspension point interferometer Design document will be finished in this year DECIGO (Interferometer in space) Working group

24. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 24 R&D tasks (1) --- CLIO100 --- CLIO100 : 100m cryogenic interferometer Development and test of … Mirror Suspension Cryogenics Tunnel digging finished (July 2002) (S.Miyoki, M.Ohashi, et. al.)

25. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 25 R&D tasks (2) --- TAMA SAS --- TAMA SAS Low-freq. seismic attenuation system To be installed in TAMA300 Pre-isolator of LCGT Full Scale Prototype Test Two Test Towers For a 3m Prototype Interferometer Established Local Control Characterization of Attenuation Performance Introducing New Control Method Commissioning a Fabry-Perot Cavity 2 SAS Prototypes Completed Acquired lock of the cavity (A.Takamori, et. al.)

26. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 26 --- TAMA SAS (contd.) --- (A.Takamori, et. al.)

27. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 27 --- TAMA SAS (contd.) --- (A.Takamori, et. al.)

28. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 28 R&D tasks (3) --- Direct measurement of TN --- Reference Cavity Rigid cavity (suspended) Frequency stabilization Length : 11cm Finesse : 19000 Test Cavity Displacement sensor Independent mirror Length : 1cm Finesse : 500 Spot size : 50um Material : BK7 (K.Numata, et. al.)

29. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 29 --- contd. --- Approaching TN …or looking at TN Unidentified noise : f -1/2 10 -16 m/rtHz@~100Hz ~TAMA Could be updated by Low noise driver Stack Future works Alignment Shot noise New mirror CaF2/Sapphire/Silica… Differential measurement Frequency/seismic noise Electric noise Ground loop Low noise filter (K.Numata, et. al.)

30. Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 30 Summary TAMA300 Data taking runs 6 data taking runs (August 1999- ), over 1000 hours of data Data analysis Upper limit for Galactic binary inspirals : 0.0095 /hour Coincidence analysis, burst wave, continuous wave Data taking 7 : August 31 - September 1 Detector updates Power recycling Recycling gain : 4 Longest cont. lock : 4 hours (over 24 hours without power recycling) Improved sensitivity : h : 4x10 -21 /Hz 1/2 For LCGT R&D tasks Design document in this year