Search for Gravitational Waves from Inspiraling Compact Binaries using TAMA300 data

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TAMA binary inspiral event search
Hideyuki Tagoshi (Osaka Univ., Japan)
3rd TAMA symposium, ICRR, 2/6/2003
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Coalescing compact binaries
Neutron stars Black holes
Inspiral phase of coalescing compact binaries are
main target because Expected event rate of NS-NS
merger a few within 200Mpc /year Well known
waveform, etc. Possibility of MACHO black
holes
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TAMA Binary inspiral search

• Neutron star binary search
• TAMA-LISM coincident event search for mass range
  (onestep search)
• Lower mass
• Higher mass

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Matched filter

• Detector outputs
• known gravitational waveform
  (template)
• noise.
• Outputs of matched filter
• noise spectrum density
• signal to noise ratio
• Matched filtering is the process to find optimal
• parameters which realize

Post-Newtonian approximation
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Matched filtering analysis
52 sec
t
Read data

FFT of data Apply transfer function Conversion
to stain equivalent data

Evaluate noise spectrum near the data
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TAMA events and Galactic event
TAMA events
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Search Result TAMA DT6
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Log10Number of events
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Upper limit to the Galactic event rate

• N Upper limit to the average number of events
• over certain threshold
• T Length of data hours
• Detection efficiency

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Galactic event simulation
We perform Galactic event simulation to estimate
detection efficiency Assume binary neutron stars
distribution in our Galaxy
Mass distribute uniformly between

• Give a time during DT6
• Determine mass, position, inclination angle,
  phase by random numbers
• Give a test signal into real data
• Search
• Make event lists and estimate detection efficiency

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Galactic event detection efficiency
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Upper limit to the event rate Poisson statistics

• Threshold ( )
• Expected number of fake events over
  thresholdNbg0.1
• Observed number of events over threshold Nobs0
• Assuming Poisson distribution for the number of
  real/fake events
• over the threshold,
• we obtain upper limit to the expected number of
  real events from

N2.3 (C.L.90)
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Upper limit to the Galactic event rate

• threshold16 (S/N11)
• (fake event rate0.8/year)
• Efficiency
• We also obtain upper limit to the average number
  of events over threshold by standard Poisson
  statistics analysis
• N2.3 (C.L.90)
• Observation time T1039 hours

c.f. Caltech 40m 0.5/hour (C.L.90)
Allen et al. Phys. Rev. Lett. 83, 1498 (1999).
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DT7 analysis
TAMA DT7 2002.8.31 2002.9.2 Best Sensitivity

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DT7 event lists
23.7 hours data
These results will be used for TAMA-LIGO
coincidence analysis.
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chi square
Divide frequency region into bins. Test whether
the contribution to from each bins agree
with that expected from chirp signal
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Variation of Noise power (1 minute average)
TAMA DT6 all 8/19/20/2001
1.09minutes
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Variation of Noise power (1 minute average)
LISM DT6 9/3 9/17/2001
1.09minutes
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TAMA data analysis activity

• Binary inspiral search one step search
  (Tagoshi, Tatsumi,Takahashi)
• 
  TAMA-LISM coincidence
• 
  (Takahashi,Tagoshi,Tatsumi)
• 
  two step search (Tagoshi, Tanaka)
• Binary inspiral search using Wavelet (Kanda)
• Continuous wave from known pulsar (Soida, Ando)
• Burst wave search (Ando)
• Noise veto analysis (Kanda)
• Calibration (Tatsumi, Telada,)
• Interferometer online diagnostic (Ando,)
• BH ringdown search, Stochastic background search,
  etc. will be done.
• Two new post-docs (Tsunesasa(NAOJ),Nakano(Osaka))