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Observation run of TAMA GW detector

Observation run of TAMA GW detector. Masaki Ando Department of Science, University of Tokyo and the TAMA Collaboration. Abstract. Japanese activities for GW detection TAMA 7 year project (April 1995 – March 2002) Construct a 300m interferometric detector : TAMA300

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Observation run of TAMA GW detector

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

  4. 300m 300m 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) Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

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

  6. TAMA project (3)--- Basic design of TAMA300 --- Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

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

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

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

  10. Data taking runs (1)--- Data taking runs with TAMA300 --- 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 30for 1.4-1.4 Msolar inspirals • Operation :1107 hours (92.3%), longest cont. operation : 22 hours • Observation :1038 hours (86.5%) • Well-organized observation • Automatic lockof 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 Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

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

  13. Data taking runs (4)--- Noise level at DT6 --- • DT6 noise level • h : 5x10-21 /Hz1/2 at 1kHz • Noise sources are identified Alignment control noise Michelson phase noise Detector noise Shot noise etc. (K.Arai, R.Takahashi, et.al.) 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,…) 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 Msolar binaries) 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 Msolarevents (200-1000 templates) • c2 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%) Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

  17. Excess power Gaussianity 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 • Reject non-Gaussian noise without rejecting GW candidates • Event rate : 10-2 /hour (1.2x10-20 /Hz) 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 : 14P0(False alarm: 2.6%) No GW signal, hupperlimit : 3.4x10-23(Preliminary: fixed spindown param.) 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 /Hz1/2 • 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 Msolar) 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.) Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

  21. Improvement factor of 3 TAMA current status (2)--- Current noise level --- • Latest noise level Improved with power recycling (and the other efforts) h : 4x10-21 /Hz1/2 around 1kHz DT7 (Aug.31-Sept.1) 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=108) • Broadband RSE • Seismic isolator : SAS (300K) Cryogenic SUS (10K, Q=2x108) Suspension point interferometer 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 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.) 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.) Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

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

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

  29. --- contd. --- • Approaching TN • …or looking at TN • Unidentified noise : f-1/2 • 10-16m/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.) 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 /Hz1/2 • For LCGT • R&D tasks • Design document in this year Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

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