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Advanced LIGO

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dc.contributor.authorLIGO Scientific Collaboration,
dc.contributor.authorAasi, J.
dc.contributor.authorAbbott, B.
dc.contributor.authorAbbott, R.
dc.contributor.authorAbbott, T.
dc.contributor.authorAbernathy, M.
dc.contributor.authorAckley, K.
dc.contributor.authorAdams, C.
dc.contributor.authorAdams, T.
dc.contributor.authorAddesso, P.
dc.contributor.authorAdhikari, R.
dc.contributor.authorAdya, V.
dc.contributor.authorAffeldt, C.
dc.contributor.authorAggarwal, N.
dc.contributor.authorAguiar, O.
dc.contributor.authorAin, A.
dc.contributor.authorAjith, P.
dc.contributor.authorAlemic, A.
dc.contributor.authorAllen, B.
dc.contributor.authorAmariutei, D.
dc.contributor.authoret al.
dc.date.issued2015
dc.descriptionPart of Focus Issue: Advanced Interferometric Gravitational Wave Detectors
dc.description.abstractThe Advanced LIGO gravitational wave detectors are second-generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA, USA. The two instruments are identical in design, and are specialized versions of a Michelson interferometer with 4 km long arms. As in Initial LIGO, Fabry–Perot cavities are used in the arms to increase the interaction time with a gravitational wave, and power recycling is used to increase the effective laser power. Signal recycling has been added in Advanced LIGO to improve the frequency response. In the most sensitive frequency region around 100 Hz, the design strain sensitivity is a factor of 10 better than Initial LIGO. In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid and high frequencies. Data collecting runs with these new instruments are planned to begin in mid-2015.
dc.description.statementofresponsibilityThe LIGO Scientific Collaboration ... S E Hollitt ... D J Hosken ... E J King ... J Munch ... D J Ottaway ... P J Veitch ... et al.
dc.identifier.citationClassical and Quantum Gravity, 2015; 32(7):074001-1-074001-41
dc.identifier.doi10.1088/0264-9381/32/7/074001
dc.identifier.issn0264-9381
dc.identifier.issn1361-6382
dc.identifier.orcidBrown, D. [0000-0001-7851-3939]
dc.identifier.orcidHollitt, S. [0000-0002-4962-3546]
dc.identifier.orcidOttaway, D. [0000-0001-6794-1591]
dc.identifier.orcidVeitch, P. [0000-0002-2597-435X]
dc.identifier.urihttp://hdl.handle.net/2440/92575
dc.language.isoen
dc.publisherInstitute of Physics Publishing
dc.rights© 2015 IOP Publishing Ltd
dc.source.urihttps://doi.org/10.1088/0264-9381/32/7/074001
dc.subjectgravitational waves; interferometers; seismic isolation; optics
dc.titleAdvanced LIGO
dc.typeJournal article
pubs.publication-statusPublished

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