Observation results by the TAMA300 detector on gravitational wave bursts from stellar-core collapses

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We present the current state of veto studies in TAMA300 by monitor signals of the interferometer and its environment. In GW data analysis, fake GW events may bury real GW events or worse upper limits on the event rate. Thus, fakeevent rejection is an important issue. In general, we can reject these fake events by the monitor signals, since these fake events are induced due to detector instabilities. However, using all monitor signals for the fake-event rejection would increase the accidental rejection probability and dead time without improving veto efficiency, since all monitor signals do not have correlations to the detector instabilities. Here, we analyze coincidences between the main and selected monitor signals with the optimal parameters for the fake-event rejection. Then, coincident events are rejected as the fake events. For the signal selection and parameter optimization, we systematically investigate the correlations with the detector instabilities. As a result, we achieved 30-99% veto efficiency using ten selected monitor signals with the 3.2% accidental rejection probability and 0.2% dead time.

Section: Resultsmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A systematical veto by all monitor signals in a gravitational-wave detector

Ishidoshiro¹,

Ando²,

Tsubono³

et al. 2007

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“…The LIGO-TAMA search targeted millisecond-duration signals with frequency content in the 700-2000 Hz frequency regime (i.e., partially overlapping the present search) and had a detection efficiency of at least 50% (90%) for signals with h rss greater than ∼2 × 10 −19 Hz −1/2 (10 −18 Hz −1/2 ). Among other searches with broad-band interferometric detectors [33][34][35], the most recent one by the TAMA collaboration reported an upper limit of 0.49 events day −1 at the 90% confidence level based on an analysis of 8.1 days of the TAMA300 instrument's ninth data taking run (DT9) in 2003-2004. The best sensitivity of this TAMA search was achieved when looking for narrow-band signals at TAMA's best operating frequency, around 1300 Hz, and it was at h rss ≈ 10 −18 Hz −1/2 for 50% detection efficiency [35].…”

Section: Discussionmentioning

confidence: 99%

Search for gravitational-wave bursts in LIGO data from the fourth science run

Abbot¹

2008

The fourth science run of the LIGO and GEO 600 gravitational-wave detectors, carried out in early 2005, collected data with significantly lower noise than previous science runs. We report on a search for short-duration gravitationalwave bursts with arbitrary waveform in the 64-1600 Hz frequency range appearing in all three LIGO interferometers. Signal consistency tests, data quality cuts and auxiliary-channel vetoes are applied to reduce the rate of spurious triggers. No gravitational-wave signals are detected in 15.5 days of live observation time; we set a frequentist upper limit of 0.15 day −1 (at 90% confidence level) on the rate of bursts with large enough amplitudes to be detected reliably. The amplitude sensitivity of the search, characterized using Monte Carlo simulations, is several times better than that of previous searches. We also provide rough estimates of the distances at which representative supernova and binary black hole merger signals could be detected with 50% efficiency by this analysis.PACS numbers: 04.80. Nn, 95.85.Sz

“…Over the past decade, the search for these signals has been independently performed by individual detectors or by homogeneous networks of resonant bars [4] or laser interferometers [5][6][7][8][9]. The first coincident burst analysis between interferometers with different broadband sensitivity and orientation was performed by the TAMA and LIGO Scientific Collaborations [10].…”

Section: Introductionmentioning

confidence: 99%

A joint search for gravitational wave bursts with AURIGA and LIGO

Baggio¹,

Bignotto²,

Bonaldi³

et al. 2008

The first simultaneous operation of the AURIGA detector 63 and the LIGO observatory 64 was an opportunity to explore real data, joint analysis methods between two very different types of gravitational wave detectors: resonant bars and interferometers. This paper describes a coincident gravitational wave burst search, where data from the LIGO interferometers are cross-correlated at the time of AURIGA candidate events to identify coincident transients. The analysis pipeline is tuned with two thresholds, on the signal-to-noise ratio of AURIGA candidate events and on the significance of the cross-correlation test in LIGO. The false alarm rate is estimated by introducing time shifts between data sets and the network detection efficiency is measured by adding simulated gravitational wave signals to the detector output. The simulated waveforms have a significant fraction of power in the narrower AURIGA band. In the absence of a detection, we discuss how to set an upper limit on the rate of gravitational waves and to interpret it according to different source models. Due to the short amount of analyzed data and to the high rate of non-Gaussian transients in the detectors' noise at the time, the relevance of this study is methodological: this was the first joint search for gravitational wave bursts among detectors with such different spectral sensitivity and the first opportunity for the resonant and interferometric communities to unify languages and techniques in the pursuit of their common goal.