An upper limit on the stochastic gravitational-wave background of cosmological origin.

Autor: Abbott BP, Abbott R, Acernese F, Adhikari R, Ajith P, Allen B, Allen G, Alshourbagy M, Amin RS, Anderson SB, Anderson WG, Antonucci F, Aoudia S, Arain MA, Araya M, Armandula H, Armor P, Arun KG, Aso Y, Aston S, Astone P, Aufmuth P, Aulbert C, Babak S, Baker P, Ballardin G, Ballmer S, Barker C, Barker D, Barone F, Barr B, Barriga P, Barsotti L, Barsuglia M, Barton MA, Bartos I, Bassiri R, Bastarrika M, Bauer TS, Behnke B, Beker M, Benacquista M, Betzwieser J, Beyersdorf PT, Bigotta S, Bilenko IA, Billingsley G, Birindelli S, Biswas R, Bizouard MA, Black E, Blackburn JK, Blackburn L, Blair D, Bland B, Boccara C, Bodiya TP, Bogue L, Bondu F, Bonelli L, Bork R, Boschi V, Bose S, Bosi L, Braccini S, Bradaschia C, Brady PR, Braginsky VB, Brand JF, Brau JE, Bridges DO, Brillet A, Brinkmann M, Brisson V, Van Den Broeck C, Brooks AF, Brown DA, Brummit A, Brunet G, Bullington A, Bulten HJ, Buonanno A, Burmeister O, Buskulic D, Byer RL, Cadonati L, Cagnoli G, Calloni E, Camp JB, Campagna E, Cannizzo J, Cannon KC, Canuel B, Cao J, Carbognani F, Cardenas L, Caride S, Castaldi G, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cepeda C, Cesarini E, Chalermsongsak T, Chalkley E, Charlton P, Chassande-Mottin E, Chatterji S, Chelkowski S, Chen Y, Christensen N, Chung CT, Clark D, Clark J, Clayton JH, Cleva F, Coccia E, Cokelaer T, Colacino CN, Colas J, Colla A, Colombini M, Conte R, Cook D, Corbitt TR, Corda C, Cornish N, Corsi A, Coulon JP, Coward D, Coyne DC, Creighton JD, Creighton TD, Cruise AM, Culter RM, Cumming A, Cunningham L, Cuoco E, Danilishin SL, D'Antonio S, Danzmann K, Dari A, Dattilo V, Daudert B, Davier M, Davies G, Daw EJ, Day R, De Rosa R, Debra D, Degallaix J, Del Prete M, Dergachev V, Desai S, Desalvo R, Dhurandhar S, Di Fiore L, Di Lieto A, Di Paolo Emilio M, Di Virgilio A, Díaz M, Dietz A, Donovan F, Dooley KL, Doomes EE, Drago M, Drever RW, Dueck J, Duke I, Dumas JC, Dwyer JG, Echols C, Edgar M, Effler A, Ehrens P, Ely G, Espinoza E, Etzel T, Evans M, Evans T, Fafone V, Fairhurst S, Faltas Y, Fan Y, Fazi D, Fehrmann H, Ferrante I, Fidecaro F, Finn LS, Fiori I, Flaminio R, Flasch K, Foley S, Forrest C, Fotopoulos N, Fournier JD, Franc J, Franzen A, Frasca S, Frasconi F, Frede M, Frei M, Frei Z, Freise A, Frey R, Fricke T, Fritschel P, Frolov VV, Fyffe M, Galdi V, Gammaitoni L, Garofoli JA, Garufi F, Genin E, Gennai A, Gholami I, Giaime JA, Giampanis S, Giardina KD, Giazotto A, Goda K, Goetz E, Goggin LM, González G, Gorodetsky ML, Gobler S, Gouaty R, Granata M, Granata V, Grant A, Gras S, Gray C, Gray M, Greenhalgh RJ, Gretarsson AM, Greverie C, Grimaldi F, Grosso R, Grote H, Grunewald S, Guenther M, Guidi G, Gustafson EK, Gustafson R, Hage B, Hallam JM, Hammer D, Hammond GD, Hanna C, Hanson J, Harms J, Harry GM, Harry IW, Harstad ED, Haughian K, Hayama K, Heefner J, Heitmann H, Hello P, Heng IS, Heptonstall A, Hewitson M, Hild S, Hirose E, Hoak D, Hodge KA, Holt K, Hosken DJ, Hough J, Hoyland D, Huet D, Hughey B, Huttner SH, Ingram DR, Isogai T, Ito M, Ivanov A, Johnson B, Johnson WW, Jones DI, Jones G, Jones R, Sancho de la Jordana L, Ju L, Kalmus P, Kalogera V, Kandhasamy S, Kanner J, Kasprzyk D, Katsavounidis E, Kawabe K, Kawamura S, Kawazoe F, Kells W, Keppel DG, Khalaidovski A, Khalili FY, Khan R, Khazanov E, King P, Kissel JS, Klimenko S, Kokeyama K, Kondrashov V, Kopparapu R, Koranda S, Kozak D, Krishnan B, Kumar R, Kwee P, La Penna P, Lam PK, Landry M, Lantz B, Laval M, Lazzarini A, Lei H, Lei M, Leindecker N, Leonor I, Leroy N, Letendre N, Li C, Lin H, Lindquist PE, Littenberg TB, Lockerbie NA, Lodhia D, Longo M, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lu P, Lubinski M, Lucianetti A, Lück H, Machenschalk B, Macinnis M, Mackowski JM, Mageswaran M, Mailand K, Majorana E, Man N, Mandel I, Mandic V, Mantovani M, Marchesoni F, Marion F, Márka S, Márka Z, Markosyan A, Markowitz J, Maros E, Marque J, Martelli F, Martin IW, Martin RM, Marx JN, Mason K, Masserot A, Matichard F, Matone L, Matzner RA, Mavalvala N, McCarthy R, McClelland DE, McGuire SC, McHugh M, McIntyre G, McKechan DJ, McKenzie K, Mehmet M, Melatos A, Melissinos AC, Mendell G, Menéndez DF, Menzinger F, Mercer RA, Meshkov S, Messenger C, Meyer MS, Michel C, Milano L, Miller J, Minelli J, Minenkov Y, Mino Y, Mitrofanov VP, Mitselmakher G, Mittleman R, Miyakawa O, Moe B, Mohan M, Mohanty SD, Mohapatra SR, Moreau J, Moreno G, Morgado N, Morgia A, Morioka T, Mors K, Mosca S, Mossavi K, Mours B, Mowlowry C, Mueller G, Muhammad D, Mühlen HZ, Mukherjee S, Mukhopadhyay H, Mullavey A, Müller-Ebhardt H, Munch J, Murray PG, Myers E, Myers J, Nash T, Nelson J, Neri I, Newton G, Nishizawa A, Nocera F, Numata K, Ochsner E, O'Dell J, Ogin GH, O'Reilly B, O'Shaughnessy R, Ottaway DJ, Ottens RS, Overmier H, Owen BJ, Pagliaroli G, Palomba C, Pan Y, Pankow C, Paoletti F, Papa MA, Parameshwaraiah V, Pardi S, Pasqualetti A, Passaquieti R, Passuello D, Patel P, Pedraza M, Penn S, Perreca A, Persichetti G, Pichot M, Piergiovanni F, Pierro V, Pinard L, Pinto IM, Pitkin M, Pletsch HJ, Plissi MV, Poggiani R, Postiglione F, Principe M, Prix R, Prodi GA, Prokhorov L, Punken O, Punturo M, Puppo P, Putten Sv, Quetschke V, Raab FJ, Rabaste O, Rabeling DS, Radkins H, Raffai P, Raics Z, Rainer N, Rakhmanov M, Rapagnani P, Raymond V, Re V, Reed CM, Reed T, Regimbau T, Rehbein H, Reid S, Reitze DH, Ricci F, Riesen R, Riles K, Rivera B, Roberts P, Robertson NA, Robinet F, Robinson C, Robinson EL, Rocchi A, Roddy S, Rolland L, Rollins J, Romano JD, Romano R, Romie JH, Röver C, Rowan S, Rüdiger A, Ruggi P, Russell P, Ryan K, Sakata S, Salemi F, Sandberg V, Sannibale V, Santamaría L, Saraf S, Sarin P, Sassolas B, Sathyaprakash BS, Sato S, Satterthwaite M, Saulson PR, Savage R, Savov P, Scanlan M, Schilling R, Schnabel R, Schofield R, Schulz B, Schutz BF, Schwinberg P, Scott J, Scott SM, Searle AC, Sears B, Seifert F, Sellers D, Sengupta AS, Sentenac D, Sergeev A, Shapiro B, Shawhan P, Shoemaker DH, Sibley A, Siemens X, Sigg D, Sinha S, Sintes AM, Slagmolen BJ, Slutsky J, van der Sluys MV, Smith JR, Smith MR, Smith ND, Somiya K, Sorazu B, Stein A, Stein LC, Steplewski S, Stochino A, Stone R, Strain KA, Strigin S, Stroeer A, Sturani R, Stuver AL, Summerscales TZ, Sun KX, Sung M, Sutton PJ, Swinkels BL, Szokoly GP, Talukder D, Tang L, Tanner DB, Tarabrin SP, Taylor JR, Taylor R, Terenzi R, Thacker J, Thorne KA, Thorne KS, Thüring A, Tokmakov KV, Toncelli A, Tonelli M, Torres C, Torrie C, Tournefier E, Travasso F, Traylor G, Trias M, Trummer J, Ugolini D, Ulmen J, Urbanek K, Vahlbruch H, Vajente G, Vallisneri M, Vass S, Vaulin R, Vavoulidis M, Vecchio A, Vedovato G, van Veggel AA, Veitch J, Veitch P, Veltkamp C, Verkindt D, Vetrano F, Viceré A, Villar A, Vinet JY, Vocca H, Vorvick C, Vyachanin SP, Waldman SJ, Wallace L, Ward H, Ward RL, Was M, Weidner A, Weinert M, Weinstein AJ, Weiss R, Wen L, Wen S, Wette K, Whelan JT, Whitcomb SE, Whiting BF, Wilkinson C, Willems PA, Williams HR, Williams L, Willke B, Wilmut I, Winkelmann L, Winkler W, Wipf CC, Wiseman AG, Woan G, Wooley R, Worden J, Wu W, Yakushin I, Yamamoto H, Yan Z, Yoshida S, Yvert M, Zanolin M, Zhang J, Zhang L, Zhao C, Zotov N, Zucker ME, Zweizig J
Jazyk: angličtina
Zdroj: Nature [Nature] 2009 Aug 20; Vol. 460 (7258), pp. 990-4.
DOI: 10.1038/nature08278
Abstrakt: A stochastic background of gravitational waves is expected to arise from a superposition of a large number of unresolved gravitational-wave sources of astrophysical and cosmological origin. It should carry unique signatures from the earliest epochs in the evolution of the Universe, inaccessible to standard astrophysical observations. Direct measurements of the amplitude of this background are therefore of fundamental importance for understanding the evolution of the Universe when it was younger than one minute. Here we report limits on the amplitude of the stochastic gravitational-wave background using the data from a two-year science run of the Laser Interferometer Gravitational-wave Observatory (LIGO). Our result constrains the energy density of the stochastic gravitational-wave background normalized by the critical energy density of the Universe, in the frequency band around 100 Hz, to be <6.9 x 10(-6) at 95% confidence. The data rule out models of early Universe evolution with relatively large equation-of-state parameter, as well as cosmic (super)string models with relatively small string tension that are favoured in some string theory models. This search for the stochastic background improves on the indirect limits from Big Bang nucleosynthesis and cosmic microwave background at 100 Hz.
Databáze: MEDLINE