A cryogenic silicon interferometer for gravitational-wave detection
R. X. Adhikari(California Institute of Technology), K. Arai(California Institute of Technology), A. F. Brooks(California Institute of Technology), C Wipf(California Institute of Technology), O Aguiar(Instituto Nacional de Pesquisas Espaciais), P. A. Altin(Australian National University), B. Barr(University of Glasgow), L Barsotti(Massachusetts Institute of Technology), R. Bassiri(Stanford University), A Bell(University of Glasgow), G. Billingsley(California Institute of Technology), R. Birney(University of the West of Scotland), D. G. Blair(The University of Western Australia), E Bonilla(Stanford University), J. H. Briggs(University of Glasgow), D. Brown(ARC Centre of Excellence for Gravitational Wave Discovery), Robert L. Byer(Stanford University), H Cao(ARC Centre of Excellence for Gravitational Wave Discovery), M. Constancio(Instituto Nacional de Pesquisas Espaciais), S. J. Cooper(University of Birmingham), T. R. Corbitt(Louisiana State University), D. C. Coyne(California Institute of Technology), A Cumming(University of Glasgow), E. J. Daw(University of Sheffield), R. T. DeRosa(LIGO Scientific Collaboration), G. Eddolls(University of Glasgow), J. Eichholz(Australian National University), M Evans(Massachusetts Institute of Technology), M. M. Fejer(Stanford University), E. C. Ferreira(Instituto Nacional de Pesquisas Espaciais), A. Freise(University of Birmingham), В. В. Фролов(LIGO Scientific Collaboration), S. Gras(Massachusetts Institute of Technology), A Green(University of Florida), H Grote(Cardiff University), E. K. Gustafson(California Institute of Technology), E. D. Hall(Massachusetts Institute of Technology), G. Hammond(University of Glasgow), J. Harms(Gran Sasso Science Institute), G Harry(American University), K. Haughian(University of Glasgow), D. Heinert(Friedrich Schiller University Jena), M. C. Heintze(LIGO Scientific Collaboration), F. Hellman(University of California, Berkeley), J. Hennig(Max Planck Institute for Gravitational Physics), M Hennig, S. Hild(Maastricht University), J. Hough(University of Glasgow), W Johnson(Louisiana State University), Brittany Kamai(California Institute of Technology), D. P. Kapasi(Australian National University), K. Komori(Massachusetts Institute of Technology), D Koptsov(Lomonosov Moscow State University), M. Korobko(Universität Hamburg), W Z Korth(California Institute of Technology), K. Kuns(Massachusetts Institute of Technology), B. Lantz(Stanford University), S. Leavey(Max Planck Institute for Gravitational Physics), F. Magaña‐Sandoval(University of Florida), G. L. Mansell(Massachusetts Institute of Technology), A. S. Markosyan(Stanford University), A. Markowitz(California Institute of Technology), I. W. Martin(University of Glasgow), R. M. Martin(Montclair State University), Д. В. Мартынов(University of Birmingham), D. E. McClelland(Australian National University), G. I. McGhee(University of Glasgow), T. McRae, J Mills(Cardiff University), V Mitrofanov(Lomonosov Moscow State University), M. Molina-Ruiz(University of California, Berkeley), C. M. Mow–Lowry(University of Birmingham), J. Münch, P. G. Murray, S. Ng, M A Okada, D. J. Ottaway, L Prokhorov, Volker Quetschke(The University of Texas Rio Grande Valley), S. Reid(University of Strathclyde), D Reitze, J. W. Richardson, R. Robie, I. M. Romero-Shaw(ARC Centre of Excellence for Gravitational Wave Discovery), R. K. Route, Sheila Rowan, R Schnabel(Universität Hamburg), M Schneewind(Max Planck Institute for Gravitational Physics), Frank Seifert(National Institute of Standards and Technology), D Shaddock, B Shapiro, D. H. Shoemaker, A S Silva, B Slagmolen, J. R. Smith(California State University, Fullerton), N Smith, J. Steinlechner(Maastricht University), K Strain, D Taira, S Tait, D. B. Tanner(University of Florida), Z. Tornasi, C Torrie, M Van Veggel, J Vanheijningen, P. J. Veitch, A. R. Wade, Gordon G. Wallace, R. L. Ward, R. Weiss, P. Weßels, B. Willke, H. Yamamoto, M. J. Yap, C. Zhao
Cited by 195Open Access
Abstract
The detection of gravitational waves from compact binary mergers by LIGO has opened the era of gravitational wave astronomy, revealing a previously hidden side of the cosmos. To maximize the reach of the existing LIGO observatory facilities, we have designed a new instrument that will have 5 times the range of Advanced LIGO, or greater than 100 times the event rate. Observations with this new instrument will make possible dramatic steps toward understanding the physics of the nearby universe, as well as observing the universe out to cosmological distances by the detection of binary black hole coalescences. This article presents the instrument design and a quantitative analysis of the anticipated noise floor.
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