G030XXX-00-Z Excess power trigger generator Patrick Brady and Saikat Ray-Majumder University of Wisconsin-Milwaukee LIGO Scientific Collaboration.

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Presentation transcript:

G030XXX-00-Z Excess power trigger generator Patrick Brady and Saikat Ray-Majumder University of Wisconsin-Milwaukee LIGO Scientific Collaboration

G030XXX-00-Z 18/12/2003GWDAW - Dec Excess power method: the basic idea The basic idea: »Pick a start time, a duration (dt), and a frequency band (df) »Fourier transform detector data with specified start time and duration »Sum the power in the frequency band »Calculate probability of obtaining the summed power from Gaussian noise using a  2 distribution with (2 x dt x df) degrees of freedom »If the probability is small, record a trigger »Repeat procedure for all start times, frequency bands and durations For Gaussian noise, the method is optimal to detect bursts of specified duration and frequency bandwidh »Details are in Anderson, Brady, Creighton and Flanagan [PRD 63, (2001)]

G030XXX-00-Z 18/12/2003GWDAW - Dec Excess-power method: time-frequency decomposition Using N data points corresponding to maximum duration of signal to be detected Construct time-frequency planes at multiple resolutions Each plane is constructed to have pixels of unit time- frequency volume Time resolution improves by factor of 2 from plane to plane

G030XXX-00-Z 18/12/2003GWDAW - Dec Excess-power method: Implementation Calculate time-frequency planes as described above’ Compute power in tiles defined by a start-time, duration, low-frequency, frequency band Output is sngl_burst trigger if probability of obtaining power from Gaussian noise is less than user supplied threshold

G030XXX-00-Z 18/12/2003GWDAW - Dec Tuning the search code Parameters available for tuning »Lowest frequency to search »Maximum and minimum time duration of signals »Maximum bandwidth »Confidence threshold »Number of events recorded for each 1 second of data Tuning procedure »Lowest frequency decided based on high glitch rate below 130 Hz »Max duration is 1 second; Min duration is 1/64 seconds »Max bandwidth of a tile 64Hz, but allows for broader band signals by clustering »Tuned confidence threshold and number of events recorded to allow trigger rate ~ 1 Hz

G030XXX-00-Z 18/12/2003GWDAW - Dec Running the search on large data sets Excess power runs standalone using Condor batch scheduler »Directed Acyclic Graph describes workflow Use LALdataFind to locate data »Interrogation of replica catalog maintained by LDR (S. Koranda) All search code in »LAL and LALApps (many contributors) Power code »Generates triggers from each interferometer Coincidence stage of the search is part of the jobs we run »Coincidence needs to be tuned within burst group (See talk by Cadonati)

G030XXX-00-Z 18/12/2003GWDAW - Dec Performance on interferometer data Same data with Sine- Gaussians at 250Hz, h0 = 6e s: uncalibrated data

G030XXX-00-Z 18/12/2003GWDAW - Dec Frequency Dependence of Triggers Hanford 4km: # of triggers in various freq. bands Livingston 4km: # of triggers in various freq. bands Frequency 800 Triggers

G030XXX-00-Z 18/12/2003GWDAW - Dec Measuring the efficiency of algorithm Sine Gaussian waveform »h + (t) = h 0 Sin[ 2  f 0 (t-t 0 ) ] exp[ - (t – t 0 ) 2 /  2 ] »h x (t) = 0 Signal parameters used: »Frequencies: 235, 319, 434, 590, 801 »Q = sqrt(2)  f 0  = 8.89 »h 0 = [10 -21, ] uniform on log scale Location on sky for single detector tests: »Zenith of each detector »Linearly polarized w.r.t. that detector »That is F + =1, F x =0

G030XXX-00-Z 18/12/2003GWDAW - Dec Efficiencies to Q=9 Sine-Gaussians 4km Interferometers

G030XXX-00-Z 18/12/2003GWDAW - Dec Parameter accuracy: peak time and central frequency Peak time Central frequency Q=9 Sine-Gaussian at 235Hz

G030XXX-00-Z 18/12/2003GWDAW - Dec Continuing work as part of LSC burst analysis group Tune the coincidence step to best utilize triggers from excess power Extend efficiency measurements to all sky for sine- Gaussians Extend efficiency measurements to include supernova waveforms Implement multi-detector extension of excess power discussed in Anderson, Brady, Creighton and Flanagan [PRD 63, (2001)] Test alternative statistic involving over-whitened data [See ABCF and/or Vicere PRD 66, (2002)]