Advanced LIGO
J. AasiLIGO, California Institute of Technology, Pasadena, CA 91125, USAB. P. AbbottLIGO, California Institute of Technology, Pasadena, CA 91125, USAR. AbbottLIGO, California Institute of Technology, Pasadena, CA 91125, USAT. D. AbbottLouisiana State University, Baton Rouge, LA 70803, USAM. R. AbernathyLIGO, California Institute of Technology, Pasadena, CA 91125, USAK. AckleyUniversity of Florida, Gainesville, FL 32611, USAC. AdamsLIGO Livingston Observatory, Livingston, LA 70754, USAT. AdamsCardiff University, Cardiff, CF24 3AA, UKP. AddessoUniversity of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, ItalyR. X. AdhikariLIGO, California Institute of Technology, Pasadena, CA 91125, USAV. B. AdyaExperimental Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyC. AffeldtExperimental Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyN. AggarwalLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAO. D. AguiarInstituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, SP, BrazilA. AinInter-University Centre for Astronomy and Astrophysics, Pune 411007, IndiaP AjithInternational Centre for Theoretical Sciences, Tata Institute of Fundamental, Research, Bangalore 560012, IndiaA. AlemicSyracuse University, Syracuse, NY 13244, USAB. AllenData Analysis Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyD. AmariuteiUniversity of Florida, Gainesville, FL 32611, USAS. B. AndersonLIGO, California Institute of Technology, Pasadena, CA 91125, USAW. G. AndersonUniversity of Wisconsin–Milwaukee, Milwaukee, WI 53201, USAK. AraiLIGO, California Institute of Technology, Pasadena, CA 91125, USAM. C. ArayaLIGO, California Institute of Technology, Pasadena, CA 91125, USAC. C. ArceneauxThe University of Mississippi, University, MS 38677, USAJ. S. AreedaCalifornia State University Fullerton, Fullerton, CA 92831, USAG. AshtonUniversity of Southampton, Southampton, SO17 1BJ, UKS. AstLeibniz Universität Hannover, D-30167 Hannover, GermanyS. M. AstonLIGO Livingston Observatory, Livingston, LA 70754, USAP. AufmuthLeibniz Universität Hannover, D-30167 Hannover, GermanyC. AulbertData Analysis Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyB. E. AylottUniversity of Birmingham, Birmingham, B15 2TT, UKS BabakAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Golm, GermanyP. T. BakerMontana State University, Bozeman, MT 59717, USAS. W. BallmerSyracuse University, Syracuse, NY 13244, USAJ. C. BarayogaLIGO, California Institute of Technology, Pasadena, CA 91125, USAM. BarbetUniversity of Florida, Gainesville, FL 32611, USAS. BarclaySUPA, University of Glasgow, Glasgow, G12 8QQ, UKB. C. BarishLIGO, California Institute of Technology, Pasadena, CA 91125, USAD. BarkerB. BarrSUPA, University of Glasgow, Glasgow, G12 8QQ, UKL. BarsottiLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAJ. BartlettM. A. BartonI. BartosColumbia University, New York, NY 10027, USAR. BassiriStanford University, Stanford, CA 94305, USAJ. C. BatchC. BauneExperimental Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyB. BehnkeAlbert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Golm, GermanyA. S. BellSUPA, University of Glasgow, Glasgow, G12 8QQ, UKC. BellSUPA, University of Glasgow, Glasgow, G12 8QQ, UKM. BenacquistaThe University of Texas at Brownsville, Brownsville, TX 78520, USAJ. BergmanG. BergmannExperimental Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyC. P. L. BerryUniversity of Birmingham, Birmingham, B15 2TT, UKJ. BetzwieserLIGO Livingston Observatory, Livingston, LA 70754, USAS. BhagwatSyracuse University, Syracuse, NY 13244, USAR. BhandareRRCAT, Indore, MP 452013, IndiaI. A. BilenkoFaculty of Physics, Lomonosov Moscow State University, Moscow 119991, RussiaG. BillingsleyLIGO, California Institute of Technology, Pasadena, CA 91125, USAJ. BirchLIGO Livingston Observatory, Livingston, LA 70754, USASébastien BiscansLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAC. BiwerSyracuse University, Syracuse, NY 13244, USAJ. K. BlackburnLIGO, California Institute of Technology, Pasadena, CA 91125, USALindy BlackburnNASA/Goddard Space Flight Center, Greenbelt, MD 20771, USAC. D. BlairUniversity of Western Australia, Crawley, WA 6009, AustraliaD. G. BlairUniversity of Western Australia, Crawley, WA 6009, AustraliaO. BockData Analysis Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyT. P. BodiyaLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAP. BojtosMTA Eötvös University, ‘Lendulet’ Astrophysics Research Group, Budapest 1117, HungaryC. BondUniversity of Birmingham, Birmingham, B15 2TT, UKR. BorkLIGO, California Institute of Technology, Pasadena, CA 91125, USAM. BornExperimental Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyS. BoseInter-University Centre for Astronomy and Astrophysics, Pune 411007, IndiaP. R. BradyUniversity of Wisconsin–Milwaukee, Milwaukee, WI 53201, USAV. B. BraginskyFaculty of Physics, Lomonosov Moscow State University, Moscow 119991, RussiaJ. BrauUniversity of Oregon, Eugene, OR 97403, USAD. O. BridgesLIGO Livingston Observatory, Livingston, LA 70754, USAM. BrinkmannExperimental Group, Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik, D-30167 Hannover, GermanyA. F. BrooksLIGO, California Institute of Technology, Pasadena, CA 91125, USAD. BrownSyracuse University, Syracuse, NY 13244, USAN. M. BrownLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USASaps BuchmanStanford University, Stanford, CA 94305, USAA. BuikemaLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAA. BuonannoUniversity of Maryland, College Park, MD 20742, USAL. CadonatiUniversity of Massachusetts Amherst, Amherst, MA 01003, USAJ. Calderón BustilloUniversitat de les Illes Balears—IEEC, E-07122 Palma de Mallorca, SpainJ. B. CampNASA/Goddard Space Flight Center, Greenbelt, MD 20771, USAK. C. CannonCanadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H8, CanadaJ. CaoTsinghua University, Beijing 100084, People’s Republic of ChinaC. D. CapanoUniversity of Maryland, College Park, MD 20742, USAS. CarideUniversity of Michigan, Ann Arbor, MI 48109, USAS. CaudillUniversity of Wisconsin–Milwaukee, Milwaukee, WI 53201, USAM. CavagliàThe University of Mississippi, University, MS 38677, USAC. CepedaLIGO, California Institute of Technology, Pasadena, CA 91125, USAR. ChakrabortyLIGO, California Institute of Technology, Pasadena, CA 91125, USAT. ChalermsongsakLIGO, California Institute of Technology, Pasadena, CA 91125, USAS. J. ChamberlinUniversity of Wisconsin–Milwaukee, Milwaukee, WI 53201, USAS. ChaoNational Tsing Hua University, Hsinchu Taiwan 300P. CharltonCharles Sturt University, Wagga Wagga, NSW 2678, Australia
2015en
ABI
Аннотация
The 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.
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