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Abadie, J.,Abbott, B. P.,Abbott, R.,Abbott, T. D.,Abernathy, M.,Accadia, T.,Acernese, F.,Adams, C.,Adhikari, R. X.,Affeldt, C.,Agathos, M.,Agatsuma, K.,Ajith, P.,Allen, B.,Ceron, E. Amador,Amariutei, IOP Publishing 2012 The Astrophysical journal Vol.760 No.1
<P>We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole, and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10(-2) M-circle dot c(2) at 150 Hz, with a median limit of 17 Mpc. For short-hard GRBs we place exclusion distances on binary neutron star and neutron-star-black-hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16 Mpc and 28 Mpc, respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. However, projecting these exclusions to the sensitivities of Advanced LIGO and Virgo, which should begin operation in 2015, we find that the detection of gravitational waves associated with GRBs will become quite possible.</P>
The characterization of Virgo data and its impact on gravitational-wave searches
Aasi, J,Abadie, J,Abbott, B P,Abbott, R,Abbott, T D,Abernathy, M,Accadia, T,Acernese, F,Adams, C,Adams, T,Addesso, P,Adhikari, R,Affeldt, C,Agathos, M,Agatsuma, K,Ajith, P,Allen, B,Allocca, A,Ceron, E IOP Publishing 2012 Classical and quantum gravity Vol.29 No.15
Characterization of the LIGO detectors during their sixth science run
Aasi, J,Abadie, J,Abbott, B P,Abbott, R,Abbott, T,Abernathy, M R,Accadia, T,Acernese, F,Adams, C,Adams, T,Adhikari, R X,Affeldt, C,Agathos, M,Aggarwal, N,Aguiar, O D,Ajith, P,Allen, B,Allocca, A,Ceron IOP Publishing 2015 Classical and quantum gravity Vol.32 No.11
<P>In 2009-2010, the Laser Interferometer Gravitational-Wave Observatory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves (GWs) of astrophysical origin. The sensitivity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the GW readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources.</P>
Aasi, J.,Abadie, J.,Abbott, B. P.,Abbott, R.,Abbott, T.,Abernathy, M. R.,Accadia, T.,Acernese, F.,Adams, C.,Adams, T.,Addesso, P.,Adhikari, R. X.,Affeldt, C.,Agathos, M.,Aggarwal, N.,Aguiar, O. D.,Aji American Physical Society 2015 PHYSICAL REVIEW D - Vol.91 No.2
<P>Searches for a stochastic gravitational-wave background (SGWB) using terrestrial detectors typically involve cross-correlating data from pairs of detectors. The sensitivity of such cross-correlation analyses depends, among other things, on the separation between the two detectors: the smaller the separation, the better the sensitivity. Hence, a colocated detector pair is more sensitive to a gravitational-wave background than a noncolocated detector pair. However, colocated detectors are also expected to suffer from correlated noise from instrumental and environmental effects that could contaminate the measurement of the background. Hence, methods to identify and mitigate the effects of correlated noise are necessary to achieve the potential increase in sensitivity of colocated detectors. Here we report on the first SGWB analysis using the two LIGO Hanford detectors and address the complications arising from correlated environmental noise. We apply correlated noise identification and mitigation techniques to data taken by the two LIGO Hanford detectors, H1 and H2, during LIGO's fifth science run. At low frequencies, 40-460 Hz, we are unable to sufficiently mitigate the correlated noise to a level where we may confidently measure or bound the stochastic gravitational-wave signal. However, at high frequencies, 460-1000 Hz, these techniques are sufficient to set a 95% confidence level upper limit on the gravitational-wave energy density of Omega(f) < 7.7 x 10(-4) (f/900 Hz)(3), which improves on the previous upper limit by a factor of similar to 180. In doing so, we demonstrate techniques that will be useful for future searches using advanced detectors, where correlated noise (e.g., from global magnetic fields) may affect even widely separated detectors.</P>