Reports on Progress in Physics LIGO : the Laser Interferometer Gravitational-Wave Observatory
M Lormand,P Lu,M Lubinski,A Lucianetti,H Lück,B Machenschalk,M MacInnis,M Mageswaran,K Mailand,I Mandel,V Mandic,S Márka,Z Márka,A Markosyan,J Markowitz,E Maros,I W Martin,R M Martin,J N Marx,K Mason,F Matichard,L Matone,R A Matzner,N Mavalvala,R McCarthy,D E McClelland,S C McGuire,M McHugh,G McIntyre,D J A McKechan,K McKenzie,M Mehmet,A Melatos,A C Melissinos,D F Menéndez,G Mendell,R A Mercer,S Meshkov,C Messenger,M S Meyer,J Miller,J Minelli,Y Mino,V P Mitrofanov,G Mitselmakher,R Mittleman,O Miyakawa,B Moe,S D Mohanty,S R P Mohapatra,G Moreno,T Morioka,K Mors,K Mossavi,C MowLowry,G Mueller,H Müller-Ebhardt,D Muhammad,S Mukherjee,H Mukhopadhyay,A Mullavey,J Munch,P G Murray,E Myers,J Myers,T Nash,J Nelson,G Newton,A Nishizawa,K Numata,J O’Dell,B O’Reilly,R O’Shaughnessy,E Ochsner,G H Ogin,D J Ottaway,R S Ottens,H Overmier,B J Owen,Y Pan,C Pankow,M A Papa,V Parameshwaraiah,P Patel,M Pedraza,S Penn,A Perraca,V Pierro,I M Pinto,M Pitkin,H J Pletsch,M V Plissi,F Postiglione,M Principe,R Prix,L Prokhorov,O Punken,V Quetschke,F J Raab,D S Rabeling,H Radkins,P Raffai,Z Raics,N Rainer,M Rakhmanov,V Raymond,C M Reed,T Reed,H Rehbein,S Reid,D H Reitze,R Riesen,K Riles,B Rivera,P Roberts,N A Robertson,C Robinson,E L Robinson,S Roddy,C Röver,J Rollins,J D Romano,J H Romie,S Rowan,A Rüdiger,P Russell,K Ryan,S Sakata,L Sancho de la Jordana,V Sandberg,V Sannibale,L Santamarı́a,S Saraf,P Sarin,B S Sathyaprakash,S Sato,M Satterthwaite,P R Saulson,R Savage,P Savov,M Scanlan,R Schilling,R Schnabel,R Schofield,B Schulz,B F Schutz,P Schwinberg,J Scott,S M Scott,A C Searle,B Sears,F Seifert,D Sellers,A S Sengupta,A Sergeev,B Shapiro,P Shawhan,D H Shoemaker,A Sibley,X Siemens,D Sigg,S Sinha,A M Sintes,B J J Slagmolen,J Slutsky,J R Smith,M R Smith,N D Smith,K Somiya,B Sorazu,A Stein,L C Stein,S Steplewski,A Stochino,R Stone,K A Strain,S Strigin,A Stroeer,A L Stuver,T Z Summerscales,K-X Sun,M Sung,P J Sutton,G P Szokoly,D Talukder,L Tang,D B Tanner,S P Tarabrin,J R Taylor,R Taylor,J Thacker,K A Thorne,A Thüring,K V Tokmakov,C Torres,C Torrie,G Traylor,M Trias,D Ugolini,J Ulmen,K Urbanek,H Vahlbruch,M Vallisneri,C Van Den Broeck,M V van der Sluys,A A van Veggel,S Vass,R Vaulin,A Vecchio,J Veitch,P Veitch,C Veltkamp,A Villar,C Vorvick,S P Vyachanin,S J Waldman,L Wallace,R L Ward,A Weidner,M Weinert,A J Weinstein,R Weiss,L Wen,S Wen,K Wette,J T Whelan,S E Whitcomb,B F Whiting,C Wilkinson,P A Willems,H R Williams,L Williams,B Willke,I Wilmut,L Winkelmann,W Winkler,C C Wipf,A G Wiseman,G Woan,R Wooley,J Worden,W Wu,I Yakushin,H Yamamoto,Z Yan,S Yoshida,M Zanolin,J Zhang,L Zhang,C Zhao,N Zotov,M E Zucker,H zur Mühlen,J Zweizig
semanticscholar（2009）
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摘要
The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study gravitational waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech–MIT project supported by the National Science Foundation, operates three multi-kilometer interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to gravitational wave strains smaller than one part in 1021. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources. (Some figures in this article are in colour only in the electronic version) This article was invited by B Berger.
