LIGO-G030158-04-Z LIGO Scientific Collaboration 1 Upper Limits on the Rate of Gravitational Wave Bursts from the First LIGO Science Run Edward Daw Louisiana.

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Presentation transcript:

LIGO-G Z LIGO Scientific Collaboration 1 Upper Limits on the Rate of Gravitational Wave Bursts from the First LIGO Science Run Edward Daw Louisiana State University

LIGO-G Z LIGO Scientific Collaboration 2 Searching for ‘Unmodelled’ Bursts The LIGO burst group searches for waveforms from sources for which we cannot currently make an accurate prediction of the waveform shape. AIM METHODS Time-Frequency Plane Search ‘TFCLUSTERS’ Pure Time-Domain Search ‘SLOPE’ frequency time ‘Raw Data’ Time-domain high pass filter 0.125s 8Hz

LIGO-G Z LIGO Scientific Collaboration 3 The Analysis Pipeline

LIGO-G Z LIGO Scientific Collaboration 4 Determination of Efficiency Efficiency measured for ‘tfclusters’ algorithm Dotted: source at zenith. Continuous: source position averaged over sky 010 time (ms) amplitude 0 h To measure our efficiency, we must pick a waveform. For this talk, we consider a 1ms Gaussian burst

LIGO-G Z LIGO Scientific Collaboration 5 The ‘S1’ Science Run Data 96.0 hours triple coincidence, science locks »9.3 hours set aside as playground 86.7 hours »5.6 hours lost due to 360 sec granularity in burst search jobs 81.1 hours »26.5 hours cut by epoch veto (L1 H1 H2 combined) 54.6 hours »19.1 hours rejected because of poorly determined interferometer calibration 35.5 hours of data

LIGO-G Z LIGO Scientific Collaboration 6 Upper Limit for 1ms Gaussian Bursts Upper limit in strain compared to prior (cryogenic bar) results: IGEC 2001 combined bar upper limit: < 1 events per day having h=3x per Hz of burst bandwidth. For a 1kHz bandwidth, limit is < 2 events/day at h=3x Astone et al. (2002), report a one sigma excess of one event per day at strain level of h ~ 2x % confidence This result is derived from analysis using the ‘TFCLUSTERS’ algorithm

LIGO-G Z LIGO Scientific Collaboration 7 Conclusions and Future Work The S1 dataset has served as a testing ground for many ideas in the analysis of gravitational wave data for bursts of gravitational waves whose exact waveform is not known. There is a lot of work to do. For example: Analyze the S2 data currently being taken. Sensitivity ~10 times that during S1. Tune our analysis to check the excess claim from Astone et. al. Tighten time window for coincidence between triggers from different interferometers Use time domain waveform correlation as a test of coincident triggers.