Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 701, Issue 2, Pages L68-L74Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/701/2/L68
Keywords
gamma rays: bursts; gravitational waves; pulsars: individual (SGR 1900+14); stars: neutron
Categories
Funding
- United States National Science Foundation
- Science and Technology Facilities Council of the United Kingdom
- Max-Planck-Society
- State of Niedersachsen/Germany
- Australian Research Council
- Council of Scientific and Industrial Research of India
- Istituto Nazionale di Fisica Nucleare of Italy
- Spanish Ministerio de Educacion y Ciencia
- Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- National Aeronautics and Space Administration
- Carnegie Trust
- Leverhulme Trust
- David and Lucile Packard Foundation
- Research Corporation
- Alfred P. Sloan Foundation
- Science and Technology Facilities Council [PP/E001203/1, ST/G504284/1, PP/F001118/1, PP/F00110X/1, ST/F01032X/1, PP/F001096/1] Funding Source: researchfish
- STFC [PP/F001096/1, PP/E001203/1, ST/F01032X/1, PP/F001118/1, ST/G504284/1, PP/F00110X/1] Funding Source: UKRI
- Direct For Mathematical & Physical Scien
- Division Of Physics [0905184, 653582, 0757058] Funding Source: National Science Foundation
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We present the results of a LIGO search for short-duration gravitational waves (GWs) associated with the 2006 March 29 SGR 1900+14 storm. A new search method is used, stacking the GW data around the times of individual soft-gamma bursts in the storm to enhance sensitivity for models in which multiple bursts are accompanied by GW emission. We assume that variation in the time difference between burst electromagnetic emission and potential burst GW emission is small relative to the GW signal duration, and we time-align GW excess power time-frequency tilings containing individual burst triggers to their corresponding electromagnetic emissions. We use two GW emission models in our search: a fluence-weighted model and a flat (unweighted) model for the most electromagnetically energetic bursts. We find no evidence of GWs associated with either model. Model-dependent GW strain, isotropic GW emission energy E-GW, and gamma = E-GW/E-EM upper limits are estimated using a variety of assumed waveforms. The stacking method allows us to set the most stringent model-dependent limits on transient GW strain published to date. We find E-GW upper limit estimates (at a nominal distance of 10 kpc) of between 2 x 10(45) erg and 6 x 10(50) erg depending on the waveform type. These limits are an order of magnitude lower than upper limits published previously for this storm and overlap with the range of electromagnetic energies emitted in soft gamma repeater (SGR) giant flares.
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