Jump to ContentJump to Main Navigation
Gravity's Ghost and Big DogScientific Discovery and Social Analysis in the Twenty-First Century$

Harry Collins

Print publication date: 2013

Print ISBN-13: 9780226052298

Published to Chicago Scholarship Online: May 2014

DOI: 10.7208/chicago/9780226052328.001.0001

Show Summary Details
Page of

PRINTED FROM CHICAGO SCHOLARSHIP ONLINE (www.chicago.universitypressscholarship.com). (c) Copyright University of Chicago Press, 2017. All Rights Reserved. Under the terms of the licence agreement, an individual user may print out a PDF of a single chapter of a monograph in CHSO for personal use (for details see http://www.chicago.universitypressscholarship.com/page/privacy-policy). Subscriber: null; date: 30 March 2017

(p.179) Appendix 2 The Burst Group Abstract Prepared for the Arcadia Meeting

(p.179) Appendix 2 The Burst Group Abstract Prepared for the Arcadia Meeting

Gravity's Ghost and Big Dog
University of Chicago Press

We present the results from a search for unmodeled gravitational-wave bursts in the data collected by the network of LIGO, GEO 600 and Virgo detectors between November 2006 and November 2007. Data collected when two or more out of the four LIGO/Virgo detectors were operating simultaneously is analyzed, except for a few combinations which would contribute little observation time. The total observation time analyzed is approximately 248 days. The search is performed by three different analyses and over the entire sensitive band of the instruments of 64−6000 Hz. All analysis cuts, including veto conditions, are established in a blind way using time-shifted (background) data. The overall sensitivity of the search to incoming gravitational-wave bursts expressed in terms of their root-sum-square (rss) strain amplitude hrss lies in the range of 6 × 10−22 − 6 × 10−21 Hz−1/2 [tentative] and reflects the most sensitive search for gravitational-wave bursts performed so far. One event in one of the analyses survives all selection cuts, with a strength that is marginally significant compared to the distribution of background events, and is subjected to additional investigations. Given the significance and its resemblance in frequency and waveform to background events, we do not identify this event as a gravitational-wave signal. We interpret this search result in terms of a Frequentist upper limit on the rate of gravitational-wave events (p.180) detectable by the instruments. When combined with the previous search using earlier (2005–2006) data from the fifth science run (S5) of the LIGO detectors, this is at the level of 3.3 events per year [tentative] at 90% confidence level. Assuming several types of plausible burst waveforms we also present event rate versus strength exclusion curves.