Erratum: Upper Limits on Gravitational-Wave Emission in Association with the 27 Dec 2004 Giant Flare of SGR1806-20 [Phys. Rev. Lett.<b>95</b>, 081103 (2005)]

Baggio, Lucio; Bignotto, M.; Bonaldi, M.; Cerdonio, M.; Conti, L.; Rosa, M. De; Falferi, P.; Fortini, P.; Inguscio, M.; Liguori, N.; Marín, F.; Mezzena, R.; Mion, A.; Ortolan, A.; Prodi, G. A.; Poggi, S.; Salemi, F.; Soranzo, G.; Taffarello, L.; Vedovato, G.; Vinante, Andrea; Vitale, S.; Zendri, J.-P.

doi:10.1103/physrevlett.95.139903

Cited by 15 publications

(17 citation statements)

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“…However, the only other published GW search associated with the SGR 1806 ÿ 20 hyperflare used the AURIGA bar detector [42] to place upper limits on the GW waveform strength emitted for frequencies around 900 Hz. At the time of the event, H1's strain noise equivalent in the 900 Hz region was a factor 5 lower than AURIGA's.…”

Section: Discussionmentioning

confidence: 99%

Search for gravitational wave radiation associated with the pulsating tail of the SGR1806−20hyperflare of 27 December 2004 using LIGO

Abbott¹,

Abbott²,

Adhikari³

et al. 2007

Phys. Rev. D

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We have searched for gravitational waves (GWs) associated with the SGR 1806 ÿ 20 hyperflare of 27 December 2004. This event, originating from a Galactic neutron star, displayed exceptional energetics. Recent investigations of the x-ray light curve's pulsating tail revealed the presence of quasiperiodic oscillations (QPOs) in the 30 -2000 Hz frequency range, most of which coincides with the bandwidth of the LIGO detectors. These QPOs, with well-characterized frequencies, can plausibly be attributed to seismic modes of the neutron star which could emit GWs. Our search targeted potential quasimonochromatic GWs lasting for tens of seconds and emitted at the QPO frequencies. We have observed no candidate signals above a predetermined threshold, and our lowest upper limit was set by the 92.5 Hz QPO observed in the interval from 150 s to 260 s after the start of the flare. This bound corresponds to a (90% confidence) root-sum-squared amplitude h 90% rss-det 4:5 10 ÿ22 strain Hz ÿ1=2 on the GW waveform strength in the detectable polarization state reaching our Hanford (WA) 4 km detector. We illustrate the astrophysical significance of the result via an estimated characteristic energy in GW emission that we would expect to be able to detect. The above result corresponds to 7:7 10 46 erg ( 4:3 10 ÿ8 M c 2 ), which is of the same order as the total (isotropic) energy emitted in the electromagnetic spectrum. This result provides a means to probe the energy reservoir of the source with the best upper limit on the GW waveform strength published and represents the first broadband asteroseismology measurement using a GW detector.

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Section: Discussionmentioning

confidence: 99%

Search for gravitational wave radiation associated with the pulsating tail of the SGR1806−20hyperflare of 27 December 2004 using LIGO

Abbott¹,

Abbott²,

Adhikari³

et al. 2007

Phys. Rev. D

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“…No signal was seen, allowing upper limits on the gravitational energy emitted in the flare to be placed of O(10 −8 M c 2 ), comparable to the electromagnetic energy emitted by the galactic neutron star (see also ref. [241] for a search in Auriga data). Other searches for soft gamma ray repeaters have been carried out in S5 data [242], and a special search [243] was carried out for the 2006 storm of SGR 1900+14 [244], using stacking of LIGO data for individual bursts in the storm.…”

Section: Triggered Burst Searchesmentioning

confidence: 99%

Gravitational waves: Sources, detectors and searches

Riles

2013

Progress in Particle and Nuclear Physics

122

156

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Gravitational wave science should transform in this decade from a study of what has not been seen to a full-fledged field of astronomy in which detected signals reveal the nature of cataclysmic events and exotic objects. The LIGO Scientific Collaboration and Virgo Collaboration have recently completed joint data runs of unprecedented sensitivities to gravitational waves. So far, no gravitational radiation has been seen (although data mining continues). It seems likely that the first detection will come from 2nd-generation LIGO and Virgo interferometers now being installed. These new detectors are expected to detect ∼40 coalescences of neutron star binary systems per year at full sensitivity. At the same time, research and development continues on 3rd-generation underground interferometers and on space-based interferometers. In parallel there is a vigorous effort in the radio pulsar community to detect ∼several-nHz gravitational waves via the timing residuals from an array of pulsars at different locations in the sky. As the dawn of gravitational wave astronomy nears, this review, intended primarily for interested particle and nuclear physicists, describes what we have learned to date and the prospects for direct discovery of gravitational waves.

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“…An upper limit of E gw < 7.7 × 10 46 erg was achieved around the 92.5 Hz QPO, with a significantly weaker constraint placed in the kHz range where one expects the f -mode. The most sensitive gravitational wave search of the giant flare was from the AURIGA bar detector (Baggio et al 2005). They searched for exponentially decaying signals (with decay time 0.1 s) in a small frequency band around 900 Hz.…”

Section: Current Observational Limitsmentioning

confidence: 99%

Gravitational Waves from Neutron Stars: A Review

Lasky

2015

Publ. Astron. Soc. Aust.

168

109

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Neutron stars are excellent emitters of gravitational waves. Squeezing matter beyond nuclear densities invites exotic physical processes, many of which violently transfer large amounts of mass at relativistic velocities, disrupting spacetime and generating copious quantities of gravitational radiation. I review mechanisms for generating gravitational waves with neutron stars. This includes gravitational waves from radio and millisecond pulsars, magnetars, accreting systems, and newly born neutron stars, with mechanisms including magnetic and thermoelastic deformations, various stellar oscillation modes, and core superfluid turbulence. I also focus on what physics can be learnt from a gravitational wave detection, and where additional research is required to fully understand the dominant physical processes at play.

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Erratum: Upper Limits on Gravitational-Wave Emission in Association with the 27 Dec 2004 Giant Flare of SGR1806-20 [Phys. Rev. Lett.95, 081103 (2005)]

Cited by 15 publications

References 0 publications

Search for gravitational wave radiation associated with the pulsating tail of the SGR1806−20hyperflare of 27 December 2004 using LIGO

Search for gravitational wave radiation associated with the pulsating tail of the SGR1806−20hyperflare of 27 December 2004 using LIGO

Gravitational waves: Sources, detectors and searches

Gravitational Waves from Neutron Stars: A Review

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