1. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.171 Status of TAMA data analysis Hideyuki Tagoshi (Osaka Univ.) on behalf of the TAMA collaboration

2. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.172 Outline TAMA300 data taking history TAMA data analysis 1.Inspiral analysis 2.Burst analysis 3.Ringdown analysis Summary

3. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.173 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 data 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) DT9 Nov. 2003 - Jan., 2004 Automatic operation 6 weeks1.5x10 -21 /Hz 1/2 558 hours (27 hours) Data taking run (1) - Observation runs - TAMA observation runs Today’s talk

4. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.174 Detectable distance for binary inspirals (SNR=10, optimal direction and polarization) DT9 DT6 Now, TAMA300 covers most part of our Galaxy DT6: 33kpc DT8: 42kpc DT9: 72kpc ( ～ 30kpc on average) 1.4 M o binary inspirals Observable range DT8 Data taking run (2) - Obervable range -

5. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.175 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.

6. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.176 Gravitational Waves neutron stars black holes 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 Inspiral analysis (1)

7. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.177 Detector outputs: h(t) ： known gravitational waveform (template) n(t) ： noise Matched filter : S n (f) : noise power spectrum We need to introduce fake event reduction method because of non-Gaussian noise Fake event reduction by χ 2 selection Inspiral analysis (2) - Matched filtering - 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.

8. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.178 We found that the ρ- χ 2 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. Galactic signals TAMA triggers TAMA triggers vs Galactic signals Inspiral analysis (3) -ρ- χ 2 relation - ρ

9. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.179 Log 10 [Number of events] Mass region :1 ‐ 3Msol Threshold Set False alarm rate to 0.8 event/yr Inspiral analysis (4) - DT8 result - mass region:1-3M solar

10. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1710 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 N UL = 2.3 (C.L. = 90%) Observation time T ＝ 1163 hours = 29 event/yr (C.L.= 90 %) events/hour (1-3M solar ) Upper limit to the event rate

11. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1711 Inspiral analysis (6) - summary - DT6(2001) (1038 hours) Range: ～ 33kpc 83 events/yr (1-2M solar ) DT8(2003) (1163 hours) Range: ～ 42kpc 29 events/yr (1-3M solar ) 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

12. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1712 Relation between TAMA and LISM arms direction Distance between TAMA and LISM ～ 220km orientation latitude longitude TAMA 225° 35.68°N 139.54°E LISM 165° 36.25°N 137.18°E Tokyo (NAOJ) Kamioka 220km Maximum delay of signal arrival time ～ 0.73msec Kamioka (LCGT, CLIO site) 220km west from Tokyo IIAS Inspirla analysis (7) - Coincident analysis - Coincident analysis of DT6 data of TAMA and LISM was done. (20m IFO, Kamioka)

13. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1713 Inspiral analysis (8) - Coincident analysis - TAMA triggersLISM triggers compare require consistency DT6 results H.Takahashi et al. PRD70, 042003 (2004) 99.96% triggers are removed by coincident analysis The number of remained triggers are consistent with the accidental coincidence (no detection) Data length: 275 hours

14. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1714 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.

15. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1715 Burst analysis (1) - overview - Excess-power filter analysis (Ando et al. gr-qc/0411027) 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 Detectable range : ~ 300 pc (optimal direction, polarization)

16. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1716 Burst filter : Excess power filter Burst analysis (2) - Excess power filter - Raw Data (time series) Total power in given T-F region Assumptions for signal … time scale, frequency band Robust for waveform uncertainties Signal !! Evaluate signal power in given time-freqency regions Spectrogram Freq. sum Time- Frequency plane (spectrogram)

17. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1717 Burst analysis (3) - Target waveforms - H.Dimmelmeier et al, Astron. Astrophys. 393 (2002) 523. Amplitude : h rss : 4 x 10 -22 /Hz 1/2 (at Galactic center: 8.5kpc) Energy : E tot : 9 x 10 -8 M o c 2 Reference waveforms general relativistic, conformal flat, axisymmetric simulation by Dimmelmeier et al. (DFM) 26 waveforms Burst waves by stellar core collapse. Common characteristics Short burst waves Spike wave ~1msec Duration time <30msec Determine time-frequency band Fake reduction

18. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1718 Burst analysis (4) - Fake reduction - Fake reduction, Injection test 2. Veto with monitor channels Burst signal < 100 msec Most detector noises > a few seconds Correlated bursts in intensity monitor channel remove long-duration triggers 1. Time-scale selection Two veto methods Effective to short spikes Less than 2% Safety check : not to reject real signals Confirm that monitor channel bursts were not caused by real GW signal Hardware and software injections veto threshold Event threshold Hardware injection results DT8 analysis results (before veto) False-dismissal rate estimation Calibration : SNR (filter output)  h rss Confirm that false dismissal rate is small by injection tests

19. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1719 Burst analysis (5) - Analysis results - Analysis results Improvement in rates with veto analyses Better in DT9 than DT8 Fake rate : 30 –100 times Sensitivity : 3-6 times Still many fake events Trigger rate with vetoes DT9 DT8 DT6 DT9 (before veto) Much larger than results with Gaussian noise

20. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1720 Burst analysis (6) - Results - Results of Galactic injection test Event-selection threshold : SNR>2.9 Detection efficiency : 1.5x10 -5 Observation result : 7.5x10 -2 events/sec Galactic event rate 4 x 10 –4 M o c 2 /sec GW energy rate 5 x 10 3 events/sec (90% C.L.) Upper limit Assume a Poisson distribution for the observed event number N obs  N ul DT9, 2 nd half : 200 hours (Christmas, new-year holidays) Better noise level Stable environment

21. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1721 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 Galactic event rate 4 x 10 –4 M o c 2 /sec Galactic GW energy rate 5 x 10 3 events/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 Details can be found in Ando et al., gr-qc/0411027 Other activities of burst analysis in TAMA

22. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1722 Ringdown analysis (1) inspiral-merger Binary, SN expl. BH formation Ringdown Kerr BH core collapse perturbed BH Waveform: Damped sinusoid (Quasi-normal modes) central frequency Quality factor * Probe for BH direct observation * BH physics in inspiral-merger, core collapses,... * Good SNR expected, ~ 100@10kpc (TAMA sensitivity) QNMs h(t)=exp( － πf c t/Q)sin(2πf c t) M: mass a: angular momentum (non-dimension) Fitting formula for the least damped QNM by Echeverria (1989)

23. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1723 Template space (parameter space) construction in (f c, Q) plane which is slightly more efficient than previously proposed methods. (Nakano et al., PRD68, 102003 (2003), PTP 111, 781 (2004) ) s(f): signal + noise h(f): template S n (f): noise power spectrum f c = 100 ~ 2500 [Hz] Q = 2 ~ 33.3 (a = 0 ~ 0.998) 682 templates(SNR loss < 2%) fcfc Q Ringdown analysis (2) - template space - This template space is effectively independent to S n (f) because of its narrow band nature.

24. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1724 B F True signal : * exponential tail * symmetric around the local maximum -cut Time t Fake triggers : * exp rising, no tail True signal ---> smaller Time Domain Cuts: Time t filter output expected tail Ringdown analysis (3) - Event selection -

25. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1725 for Galactic events 10% 100% 50% Larger Mass Lower Mass Ringdown analysis (4) - Detection probability - Assumption: E ～ 0.03M BH is radiated by QNM gravitational wave

26. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1726 f c > 1500Hz: (M < 20M solar ) DT6: DT8: DT9: (SNR > 20) Integrated over Q axis Preliminary Ringdown analysis (5) - Galactic event rate - T obs [Hours] DT6: 959 DT8: 1086 DT9: 430

27. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1727 * BH ringdown is promising GW source * TAMA has good sensitivity to detect Galactic events, detection probability > 10% * Matched filtering code developed Ringdown analysis (6) - Summary - * 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

28. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1728 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, ……

29. The 4th TAMA Symposium and the Winter School of GW @ Osaka City University, 2005.2.1729 End