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Results of the search for burst gravitational waves with the TAMA300 detector

Results of the search for burst gravitational waves with the TAMA300 detector. Masaki Ando (Department of Physics, University of Tokyo) and The TAMA Collaboration. Upper limit for Galactic events Galactic event rate GW energy rate. Introduction.

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Results of the search for burst gravitational waves with the TAMA300 detector

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  1. Results of the search for burst gravitational waves with the TAMA300 detector Masaki Ando (Department of Physics, University of Tokyo) and The TAMA Collaboration The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  2. Upper limit for Galactic events Galactic event rate GW energy rate Introduction • Target of this work … Burst gravitational waves Predicted waveforms of stellar-core collapse TAMA300 data Data Taking 9 Data analysis Excess power filter Fake reduction Galactic simulation Signal injection simulation The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  3. Outline • Target waveform • TAMA300 data Overview, Observation runs, Noise level • Analysis scheme Burst filter, Fake reduction • Analysis results Event-trigger rate • Galactic simulation • Summary and Conclusion The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  4. Reference waveforms Relativistic, axisymmetric simulation byDimmelmeier et al. 26 waveforms H.Dimmelmeier et al, Astron. Astrophys. 393 (2002) 523. Amplitude : h rss : 4 x 10-22 /Hz1/2 (at Galactic center: 8.5kpc) Energy : E tot : 9 x 10-8 Moc2 Analysis target- Target waveforms - • Targets : Burst waves from stellar-core collapse Numerical simulations … ~100 waveforms are obtained Not cover all initial conditions Common characteristics Short burst waves Spike wave ~1msec Duration time <30msec Not suitable for templates (matched filtering: not available) The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  5. First obs. run in 1999 (DT1) Upgrade and observation runs Sufficient sensitivity for Galactic binary inspirals Automated crewless operation 9 observation runs (Data : ~3000 hours) TAMA300 (1)- Overview - • Data : Observation data by TAMA300 TAMA300, an interferometric GW detector in Japan Baseline length : 300m Fabry-Perot-Michelson interferometer with power recycling Placed at National Astronomical Observatory in Japan Baseline 300m National Astronomical Observatory at Mitaka, Japan The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  6. TAMA300 (2)- Observation runs - • TAMA observation runs The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  7. TAMA300 (3)- Data Taking 9 - • TAMA DT9 Data Taking 9 Nov. 28, 2003 – Jan. 10, 2004 558 hours of data Noise level : 2x10-21 /Hz1/2 This analysis … DT6 Noise floor level drift DT8 2nd half : 200 hours (Christmas, new-year Holiday terms) Better noise level Stable environment DT9 The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  8. TAMA300 (4)- Noise spectrum - • Noise spectrum TAMA noise spectrum withDimmelmeier waveforms Detectable range : ~ 300 pc (optimal direction, polarization) The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  9. Raw Data (time series) Total power in given T-F region Burst-wave analysis (1) - Excess power filter - • Burst filter : Excess power filter Evaluate signal power in given time-freqency regions Spectrogram Time- Frequency plane (spectrogram) Freq. sum Signal !! Few assumptions for signal … time-frequency bands Robust for waveform uncertainties The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  10. Burst-wave analysis (2) - Filter parameters - • Filter parameters (time-frequency window) Burst GW → Short duration, wide frequency band (c.f. Cont. waves: long duration, narrow freq. band) For higher SNR … Short time window ~Signal duration Requires line removal Wide frequency window Limited by worse noise level at low and high freq. Dt = 12.8 [msec] Df = 2300 [Hz] The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  11. Burst-wave analysis (3) - Data conditioning - • Data conditioning Line removal Filter freq. resolution : ~80Hz line removal is required (AC line, Violin mode peak, Calibration peak) Without Line Removal With Line Removal Method FFT 72sec data Reject line freq. components Inverse FFT Normalization Track the drift of noise level Each spectrum is normalized by averaged noise spectrum 30min (5.6x10-4 Hz) Use 30min-averaged spectrum The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  12. Hardware and software injections Safety check : not to reject real signals Confirm that monitor channel bursts were not caused by real GW signal Event threshold DT8 analysis results (before veto) veto threshold False-dismissal rate estimation Less than 2% Hardware injection results Calibration : SNR (filter output)hrss Burst-wave analysis (4)- Fake reduction - • Fake reduction, Injection test Two veto methods Time-scale selection Veto with monitor channels Burst signal < 100 msec Most detector noises > a few seconds Correlated bursts in intensity monitor channel Effective to long-duration noises Effective to short spikes The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  13. TAMA burst analysis- Analysis results - • Analysis results Trigger rate with vetoes Improvement in rates with veto analyses Better in DT9 than DT8 Fake rate : 30 –100 times Sensitivity : 3-6 times DT8 DT9 (before veto) Much larger than results with Gaussian noise DT9 DT6 Still many fake events The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  14. Position : Somewhere in Galaxy Exponential Disk model Galactic-event distribution R = (x 2+y 2) 1/2 Rd : 3.5 kpc, hd : 325 pc Time ： Somewhere in DT9 (200hr) Detector angular depend. Source : 26 Dimmelmeier waveforms Random angle Source angular depend. Effective distance Galactic simulation (1)- Simulation method - • Galactic simulation Monte-Carlo simulation Random events Inject signal to real data Analyze data with same codes Investigate ‘what happens with real signals’  compare with obs. results The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  15. Upper limit Assume a Poisson distribution for the observed event number N obs N ul Galactic event rate 6 x 103 events/sec GW energy rate 6 x 10–4Moc 2/sec (90% C.L.) Galactic simulation (2)- Results - • Results of Galactic injection test Event-selection threshold : SNR>2.9 Detection efficiency : 1x10-5 Observation result : 7x10-2 events/sec The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  16. Galactic event rate 6 x 103 events/sec Galactic GW energy rate 6 x 10–4Moc 2/sec (90% C.L.) Too large for real events Originate in residual fake triggers Summary • Burst-wave analysis with TAMA300 data TAMA300 DT9, 200hours of data Excess Power filter, Fake reduction Galactic event simulation (Simulated-signal injection test) The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  17. Current works TAMA detector improvement(Noise hunting, Better isolation) Better filter (Filter tuning, better burst filter) Coincidence analysis(LIGO, ROG) • We need … More realistic waveform catalog More realistic Galactic model Next-generation detector to cover our Galaxy (Ad-LIGO, LCGT) Conclusion • Conclusion This work … Scheme to set upper limits for Galactic events from observation data The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

  18. End The 9th Gravitational Wave Data Analysis Workshop (December 15-18, 2004, Annecy, France)

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