Stacked Search For Gravitational Waves From The 2006 Sgr 1900+14 Storm

LIGO Scientific Collaboration

Research output: Contribution to journalArticleAcademicpeer-review

42 Citations (Web of Science)

Abstract

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.
Original languageEnglish
Pages (from-to)L68-L74
Number of pages7
JournalAstrophysical Journal Letters
Volume701
Issue number2
DOIs
Publication statusPublished - 20 Aug 2009
Externally publishedYes

Keywords

  • gamma rays: bursts
  • gravitational waves
  • pulsars: individual (SGR 1900+14)
  • stars: neutron
  • MAGNETIZED NEUTRON-STARS
  • SOFT GAMMA-REPEATERS

Cite this