1. GWDAW10, UTB, Dec. 14 - 17, 20051 Search for inspiraling neutron star binaries using TAMA300 data Hideyuki Tagoshi on behalf of the TAMA collaboration

2. GWDAW10, UTB, Dec. 14 - 17, 20052 Outline I will describe the revised analysis of the binary neutron star search using TAMA300 data. The data we use is TAMA DT6, DT8, and DT9 data. Mass range: 1-3M_solar (for each member star)

3. GWDAW10, UTB, Dec. 14 - 17, 20053 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 This presentation

4. GWDAW10, UTB, Dec. 14 - 17, 20054 Observable distance for inspiraling binaries (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 DT8 Data taking run (2) - Observable range -

5. GWDAW10, UTB, Dec. 14 - 17, 20055 Revised analysis Difference from the analysis so far DT6: mass range 1-2M_solar (PRD70,042003(‘04)) => 1-3M_solar DT8: In the previous analysis, calibration data was not taken into account properly, due to the error of file format. We have redone the analysis. (This was applied to LIGO-TAMA S2-DT8 inspiral analysis too.) DT9: new results (initial results were reported at Amaldi6) Systematic error is estimated.

6. GWDAW10, UTB, Dec. 14 - 17, 20056 Detector outputs: h(t) ： known gravitational waveform (template) n(t) ： noise Matched filter : : one sided noise power spectrum density Parameters (mass, coalescence time, …) are not known a priori. We search the parameter space. We need to introduce fake event reduction method because of non-Gaussian noise Fake event reduction by Matched filtering a measure of the deviation of events from real signal. B. Allen, PRD 71, 062001 (2005)

7. GWDAW10, UTB, Dec. 14 - 17, 20057 We use as the statistic to discriminate fake events from true signals. We set a threshold of as where is determined by the false alarm rate. The chi square cut is automatically introduced by these procedures. This statistic can accommodate large signals which could occur due to mismatch between signals and templates. Chi square cut - statistic -

8. GWDAW10, UTB, Dec. 14 - 17, 20058 Comparison of DT6, DT8 and DT9 efficiency

9. GWDAW10, UTB, Dec. 14 - 17, 20059 DT6, DT8, DT9 trigger lists

10. GWDAW10, UTB, Dec. 14 - 17, 200510 In the case of Gaussian noise, the square of, or, obeys the F distribution with the degree of freedom (2,2p-2). Decision of threshold (p: the number of division of a template in the definition of chi^2. In our case, p=15. ) The probability density function g(z) of z is given by Thus, in Gaussian case, if we make a log(N(z))-log(z+p-1) plot of the triggers, it becomes linear with slope=-p+1. This suggest that z+p-1 is a more natural variable for the estimation of the false alarm rate than. and

11. GWDAW10, UTB, Dec. 14 - 17, 200511 DT9 threshold (1) Looks like linear, although the slope is Different from Gaussian case

12. GWDAW10, UTB, Dec. 14 - 17, 200512 DT9 threshold (2) Threshold = 2.24 for the false alarm rate = 1/yr

13. GWDAW10, UTB, Dec. 14 - 17, 200513 DT8 threshold Threshold = 2.04 for the false alarm rate = 1/yr

14. GWDAW10, UTB, Dec. 14 - 17, 200514 DT6 threshold Threshold = 2.40 for the false alarm rate = 1/yr Unfortunately, the DT6 distribution does not look like linear even in this log-log plot. It is not easy to have accurate estimate of the false alarm rate. Thus, we take a very large value of the threshold to have a conservative upper limit.

15. GWDAW10, UTB, Dec. 14 - 17, 200515 Systematic errors (1) 1. Uncertainty of Galactic simulation Uncertainty of mass distribution Uncertainty of the position of solar system in our Galaxy Error due to finite number of simulation 2. Uncertainty of ρ due to uncertainty of theoretical wave form -10% at most. 3. Calibration error It is not know exactly (although it is expected to be less than 5%). We take a conservative value (+-10%) 4. Uncertainty of threshold (for a given false alarm rate)

16. GWDAW10, UTB, Dec. 14 - 17, 200516 Systematic errors (2) DT6DT8DT9 Uncertainty of the binary distribution model +0.03 -0.04 +0.03 -0.05 +0.03 -0.05 Error of Monte Carlo injection +0.01 -0.01 +0.01 -0.01 +0.01 -0.01 Uncertainty of wave form-0.03-0.04 Calibration error +0.03 -0.03 +0.05 -0.04 +0.04 -0.04 Uncertainty of threshold +0.00 -0.00 +0.03 -0.02 +0.01 -0.02 Total error of efficiency +0.05 -0.05 +0.07 -0.08 +0.05 -0.07 preliminarysummary

17. GWDAW10, UTB, Dec. 14 - 17, 200517 Upper limit to the Galactic events Data length [hours] Mass range of a member star [Msolar] Detection probability of Galactic signals Threshold of ζ (false alarm rate = 1 /yr) Upper limit to the Milky Way Galaxy events [events /yr] (C.L.=90%) DT68761-30.1821.8130 DT811001-30.6013.730 DT94861-30.6917.760 DT8 gives the most stringent upper limit because of Largest length of data Rather high sensitivity to the Galactic events Very stable operation (low threshold) (DT9’s detection probability would have been much larger. However, the first half of DT9 was not very stable. Fake events with large ζ were produced during that period. They degrade the detection probability of DT9.)

18. GWDAW10, UTB, Dec. 14 - 17, 200518 Summary Reanalysis of DT6 and DT8, and the analysis of DT9 to search for the neutron star binaries were done. the low mass binary black hole higher mass bh-bh and/or bh-ns binaries with spin We will perform the search for in the near future

19. GWDAW10, UTB, Dec. 14 - 17, 200519

20. GWDAW10, UTB, Dec. 14 - 17, 200520 DT8 threshold (1)

21. GWDAW10, UTB, Dec. 14 - 17, 200521 DT6 threshold (1)

22. GWDAW10, UTB, Dec. 14 - 17, 200522 DT6, DT8, DT9 trigger lists plot