Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7876
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dc.contributor.authorAasi, J.-
dc.contributor.authorAbadie, J-
dc.contributor.authorAbbott, R-
dc.contributor.authorAbbott, T-
dc.contributor.authorAbernathy, M.R.-
dc.contributor.authorIyer, B.R.-
dc.contributor.author+ 120 Co-authors-
dc.date.accessioned2022-01-18T10:04:15Z-
dc.date.available2022-01-18T10:04:15Z-
dc.date.issued2015-06-
dc.identifier.citationClassical and Quantum Gravity, 2015, Vol. 32, p115012en_US
dc.identifier.issn0264-9381-
dc.identifier.issn1361-6382 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7876-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractIn 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.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://arxiv.org/abs/1410.7764en_US
dc.relation.urihttps://doi.org/10.1088/0264-9381/32/11/115012en_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2015CQGra..32k5012A/abstracten_US
dc.rights2015 IOP Publishing Ltd.en_US
dc.titleCharacterization of the LIGO detectors during their sixth science runen_US
dc.typeArticleen_US
Appears in Collections:Research Papers (TP)

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