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Status of TAMA data analysis

Status of TAMA data analysis. Hideyuki Tagoshi (Osaka Univ.) on behalf of the TAMA collaboration. Outline. TAMA300 data taking history TAMA data analysis Inspiral analysis Burst analysis Ringdown analysis Summary. Data taking run (1) - Observation runs -. TAMA observation runs.

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Status of TAMA data analysis

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  1. Status of TAMA data analysis Hideyuki Tagoshi (Osaka Univ.) on behalf of the TAMA collaboration The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  2. Outline • TAMA300 data taking history • TAMA data analysis • Inspiral analysis • Burst analysis • Ringdown analysis • Summary The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  3. Data taking run (1)- Observation runs - • TAMA observation runs Today’s talk The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  4. Data taking run (2)- Obervable range - Observable range Detectable distance for binary inspirals (SNR=10, optimal direction and polarization) 1.4 Mo binary inspirals DT6: 33kpc DT8: 42kpc DT9: 72kpc (～30kpc on average) Now, TAMA300 covers most part of our Galaxy DT6 DT9 DT8 The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  5. TAMA data analysis- overview - Inspiral of compact binaries waveforms are well-known (chirp) Bursts from stellar-core collapses, etc wavefoms are not known precisely Black holes quasi-normal mode damped sinusoidal waves (ringdown) Pulsars continuous periodic waves Others veto analysis, etc. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  6. neutron stars black holes Gravitational Waves Inspiral analysis (1) Inspiral phase of coalescing compact binaries are promising target because expected event rate of NS-NS merger for LCGT and advLIGO is a few within 200Mpc / year, and because waveforms are well-known, etc. chirp signal amplitude time The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  7. Inspiral analysis (2)- Matched filtering - • Detector outputs: h(t) ：　known gravitational waveform (template) n(t) ： noise • Matched filter : Sn(f) : noise power spectrum We need to introduce fake event reduction method because of non-Gaussian noise • Fake event reduction by χ2 selection a measure of the deviation of events from real signal. Parameters (mass, coalescence time, …) are not known a priori. We must search the parameter space. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  8. Inspiral analysis (3)-ρ- χ2 relation - Galactic signals TAMA triggers vs Galactic signals TAMA triggers ρ • We found that the ρ- χ2 relation is different between the • non-Gaussian triggers and the simulated Galactic signals. • Thus, we can distinguish them and reduce the fake event rate • produced by non-Gaussian noise. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  9. Inspiral analysis (4)- DT8 result - mass region:1-3Msolar Mass region :1‐3Msol Log10[Number of events] Threshold Set False alarm rate to 0.8 event/yr The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  10. Inspiral analysis (5)-Upper limit to the Galactic event rate - • Threshold=12.5 (～S/N = 9) • (fake event rate = 0.8 / year) • Detection efficiency from Galactic event simulation: • We obtain upper limit to the average number of events which exceed the threshold by standard Poisson statistics analysis • NUL = 2.3(C.L. = 90%) • Observation time T ＝ 1163 hours Upper limit to the event rate events/hour = 29 event/yr (C.L.= 90 %) (1-3Msolar) The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  11. Inspiral analysis (6)- summary - • DT6(2001) (1038 hours) • Range: ～33kpc • 83 events/yr (1-2Msolar) • DT8(2003) (1163 hours) • Range: ～42kpc • 29 events/yr (1-3Msolar) • DT9(2003-4) (558 hours) • Range: ～72kpc • analysis is not finished Initial results of DT8 analysis: Takahashi et al. Class.Quant.Grav. 21 (2004) S697 The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  12. Inspirla analysis (7)- Coincident analysis - (20m IFO, Kamioka) Coincident analysis of DT6 data of TAMA and LISM was done. orientation latitude longitude TAMA 225°35.68°N 139.54°E LISM165°36.25°N 137.18°E Kamioka (LCGT, CLIO site) 220km west from Tokyo • Distance between TAMA and LISM ～ 220km • Maximum delay of signal arrival time～0.73msec • Relation between TAMA and LISM arms direction Kamioka 220km Tokyo (NAOJ) IIAS The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  13. Inspiral analysis (8)- Coincident analysis - Data length: 275 hours H.Takahashi et al. PRD70, 042003 (2004) TAMA triggers LISM triggers compare require consistency DT6 results 99.96% triggers are removed by coincident analysis The number of remained triggers are consistent with the accidental coincidence (no detection) The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  14. Inspiral analysis (9)- Coincident analysis - • We demonstrated the power of coincident analysis by real data. • Many technical issue were tackled. Now, LIGO-TAMA coincident analysis which targets the inspiral signals is now underway by LIGO-TAMA joint working group (S. Fairhurst, H.Takahashi, et al.) Please see the poster by Takahashi. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  15. Burst analysis (1)- overview - Target: Unmodelled: Stellar-core collapse, etc Ref. waveforms by numerical sim. Schemes: Excess-power filter Fake reduction: Veto with auxiliary channel Time-scale selection Galactic simulation  detection efficiency  Upper limit for event rate • Excess-power filter analysis (Ando et al. gr-qc/0411027) Detectable range : ~ 300 pc (optimal direction, polarization) The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  16. Raw Data (time series) Total power in given T-F region Burst analysis (2)- Excess power filter - Evaluate signal power in given time-freqency regions • Burst filter : Excess power filter Spectrogram Time- Frequency plane (spectrogram) Freq. sum Signal !! Assumptions for signal … time scale, frequency band Robust for waveform uncertainties The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  17. Burst analysis (3)- Target waveforms - • Burst waves by stellar core collapse. Reference waveforms general relativistic, conformal flat, axisymmetric simulation byDimmelmeier et al. (DFM) 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 Common characteristics Short burst waves Spike wave ~1msec Duration time <30msec • Determine time-frequency band • Fake reduction The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  18. 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 analysis (4)- Fake reduction - Two veto methods • Fake reduction, Injection test 1. Time-scale selection Burst signal < 100 msec Most detector noises > a few seconds Confirm that false dismissal rate is small by injection tests remove long-duration triggers 2. Veto with monitor channels Correlated bursts in intensity monitor channel Effective to short spikes The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  19. Burst analysis (5)- Analysis results - Trigger rate with vetoes • Analysis results 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 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  20. Upper limit Assume a Poisson distribution for the observed event number N obs N ul Galactic event rate 5 x 103 events/sec GW energy rate 4 x 10–4Moc 2/sec (90% C.L.) Burst analysis (6)- Results - DT9, 2nd half : 200 hours (Christmas, new-year holidays) Better noise level Stable environment Event-selection threshold : SNR>2.9 Detection efficiency : 1.5x10-5 Observation result : 7.5x10-2 events/sec • Results of Galactic injection test The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  21. Galactic event rate 5 x 103 events/sec Galactic GW energy rate 4 x 10–4Moc 2/sec (90% C.L.) • Akutsu et al. (Poster): DT9 analysis by an ALF filter • Hayama (Poster): Development of a wavelet-based filter • LIGO-TAMA coincidence analysis Burst analysis (7)- Summary - • Burst-wave analysis with TAMA300 data TAMA300 DT9, 200hours of data Excess Power filter, Fake reduction Galactic event simulation Too large for real events Originate in residual fake triggers Details can be found in Ando et al., gr-qc/0411027 Other activities of burst analysis in TAMA The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  22. Ringdown analysis (1) inspiral-merger Ringdown Binary, SN expl. BH formation Kerr BH core collapse QNMs perturbed BH Waveform: Damped sinusoid (Quasi-normal modes) h(t)=exp(－πfct/Q)sin(2πfct) Fitting formula for the least damped QNM by Echeverria (1989) central frequency M: mass a: angular momentum (non-dimension) Quality factor * Probe for BH direct observation * BH physics in inspiral-merger, core collapses, ... * Good SNR expected, ~ 100@10kpc (TAMA sensitivity) The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  23. fc = 100 ~ 2500 [Hz] (a = 0 ~ 0.998) Q = 2 ~ 33.3 Ringdown analysis (2)- template space - s(f): signal + noise h(f): template Sn(f): noise power spectrum Template space (parameter space) construction in (fc, Q) plane which is slightly more efficient than previously proposed methods. (Nakano et al., PRD68, 102003 (2003), PTP 111, 781 (2004) ) Q 682 templates (SNR loss < 2%) This template space is effectively independent to Sn(f) because of its narrow band nature. fc The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  24. F B Ringdown analysis (3)- Event selection - True signal : * exponential tail * symmetric around the local maximum Fake triggers : * exp rising, no tail Time t Time Domain Cuts: -cut expected tail filter output Time t -cut True signal ---> smaller The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17 Time t

  25. Ringdown analysis (4)- Detection probability - for Galactic events Lower Mass Larger Mass 100% 50% Assumption: E～0.03MBHis radiated by QNM gravitational wave 10% The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  26. DT6: DT8: DT9: (SNR > 20) Ringdown analysis (5)- Galactic event rate - Tobs [Hours] DT6: 959 DT8: 1086 DT9: 430 Preliminary fc > 1500Hz: (M < 20Msolar) Integrated over Q axis The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  27. Ringdown analysis (6)- Summary - * BH ringdown is promising GW source * Matched filtering code developed * TAMA has good sensitivity to detect Galactic events, detection probability > 10% * DT6, DT8, DT9 analysis is almost done See Tsunesada et al. gr-qc/0410037 : Initial results which include detection probability, pamameter estimation errors, etc. and poster by Tsunesada for more discussion of the results The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  28. Summary • Inspiral analysis, burst analysis, ringdown analysis have been developed and the results for DT6-9 are now being obtained. • The tasks needed to be done; • inspiral : lower and higher mass search, spin, etc. • burst: other filters, more effective fake reduction method, • ringdown: more effective fake reduction method. • All of these are now under investigation. • Coincidence analysis • LIGO-TAMA joint analysis for inspiral and burst is in progress. • ROG-TAMA (bar-interferometer) • Other activity • Continuous wave search (target: 1987A remnant) K.Soida et al., Class. Quantum Grav. 20 (2003) S645 • ALF filter analysis, Wavelet method, • Veto analysis, …… The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

  29. End The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.17

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