Improved upper limits on the stochastic gravitational-wave background from 2009-2010 LIGO and Virgo data.-猫眼课题宝

DOI：

10.1103/physrevlett.113.231101

发表时间：

2014-06

期刊：

Physical review letters

影响因子：

8.6

通讯作者：

中科院分区：

物理与天体物理1区

文献类型：

作者：

J. Aasi;B. Abbott;R. Abbott;T. Abbott;M. Abernathy;T. Accadia;F. Acernese;K. Ackley;C. Adams;T. Adams;P. Addesso;R. Adhikari;C. Affeldt;M. Agathos;N. Aggarwal;O. Aguiar;A. Ain;P. Ajith;A. Alemic;B. Allen;A. Allocca;D. Amariutei;M. Andersen;R. Anderson;S. Anderson;W. Anderson;K. Arai;M. Araya;C. Arceneaux;J. Areeda;S. Aston;P. Astone;P. Aufmuth;C. Aulbert;L. Austin;B. Aylott;S. Babak;P. Baker;G. Ballardin;S. Ballmer;J. Barayoga;M. Barbet;B. Barish;D. Barker;F. Barone;B. Barr;L. Barsotti;M. Barsuglia;M. Barton;I. Bartos;R. Bassiri;A. Basti;J. Batch;J. Bauchrowitz;T. Bauer;B. Behnke;M. Bejger;M. Beker;C. Belczynski;A. Bell;C. Bell;G. Bergmann;D. Bersanetti;A. Bertolini;J. Betzwieser;P. Beyersdorf;I. Bilenko;G. Billingsley;J. Birch;S. Biscans;M. Bitossi;M. Bizouard;E. Black;J. Blackburn;L. Blackburn;D. Blair;S. Bloemen;M. Blom;O. Bock;T. Bodiya;M. Boer;G. Bogaert;C. Bogan;C. Bond;F. Bondu;L. Bonelli;R. Bonnand;R. Bork;M. Born;V. Boschi;S. Bose;L. Bosi;C. Bradaschia;P. Brady;V. Braginsky;M. Branchesi;J. Brau;T. Briant;D. Bridges;A. Brillet;M. Brinkmann;V. Brisson;A. Brooks;D. Brown;D. Brown;F. Brückner;S. Buchman;T. Bulik;H. Bulten;A. Buonanno;R. Burman;D. Buskulic;C. Buy;L. Cadonati;G. Cagnoli;J. C. Bustillo;E. Calloni;J. Camp;P. Campsie;K. Cannon;B. Canuel;J. Cao;C. Capano;F. Carbognani;L. Carbone;S. Caride;A. Castiglia;S. Caudill;M. Cavaglià;F. Cavalier;R. Cavalieri;C. Celerier;G. Cella;C. Cepeda;E. Cesarini;R. Chakraborty;T. Chalermsongsak;S. Chamberlin;S. Chao;P. Charlton;É. Chassande-Mottin;X. Chen;Y. Chen;A. Chincarini;A. Chiummo;H. Cho;J. Chow;N. Christensen;Q. Chu;S. Chua;S. Chung;G. Ciani;F. Clara;J. Clark;F. Cleva;E. Coccia;P. Cohadon;A. Colla;C. Collette;M. Colombini;L. Cominsky;M. Constancio;A. Conte;D. Cook;T. Corbitt;M. Cordier;N. Cornish;A. Corpuz;A. Corsi;C. Costa;M. Coughlin;S. Coughlin;J. Coulon;S. Countryman;P. Couvares;D. Coward;M. Cowart;D. Coyne;R. Coyne;K. Craig;J. Creighton;S. Crowder;A. Cumming;L. Cunningham;E. Cuoco;K. Dahl;T. D. Canton;M. Damjanic;S. Danilishin;S. D’Antonio;K. Danzmann;V. Dattilo;H. Daveloza;M. Davier;G. Davies;E. Daw;R. Day;T. Dayanga;G. Debreczeni;J. Degallaix;S. Deléglise;W. Del Pozzo;T. Denker;T. Dent;H. Dereli;V. Dergachev;R. De Rosa;R. Derosa;R. DeSalvo;S. Dhurandhar;M. Díaz;L. Di Fiore;A. Di Lieto;I. Di Palma;A. D. Di Virgilio;A. Donath;F. Donovan;K. Dooley;S. Doravari;S. Dossa;R. Douglas;T. Downes;M. Drago;R. Drever;J. Driggers;Z. Du;S. Dwyer;T. Eberle;T. Edo;M. Edwards;A. Effler;H. Eggenstein;P. Ehrens;J. Eichholz;S. Eikenberry;G. Endrőczi;R. Essick;T. Etzel;M. Evans;T. Evans;M. Factourovich;V. Fafone;S. Fairhurst;Q. Fang;S. Farinon;B. Farr;W. Farr;Marc Favata;H. Fehrmann;M. Fejer;D. Feldbaum;F. Feroz;I. Ferrante;F. Ferrini;F. Fidecaro;L. Finn;I. Fiori;R. Fisher;R. Flaminio;J. Fournier;S. Franco;S. Frasca;F. Frasconi;M. Frede;Z. Frei;A. Freise;R. Frey;T. Fricke;P. Fritschel;V. Frolov;P. Fulda;M. Fyffe;J. Gair;L. Gammaitoni;S. Gaonkar;F. Garufi;N. Gehrels;G. Gemme;E. Génin;A. Gennai;S. Ghosh;J. Giaime;K. Giardina;A. Giazotto;C. Gill;J. Gleason;E. Goetz;R. Goetz;L. Gondán;G. González;N. Gordon;M. Gorodetsky;S. Gossan;S. Gossler;R. Gouaty;C. Gräf;P. Graff;M. Granata;A. Grant;S. Gras;C. Gray;R. Greenhalgh;A. Gretarsson;P. Groot;H. Grote;K. Grover;S. Grunewald;G. Guidi;C. Guido;K. Gushwa;E. Gustafson;R. Gustafson;D. Hammer;G. Hammond;M. Hanke;J. Hanks;C. Hanna;J. Hanson;J. Harms;G. Harry;I. Harry;E. Harstad;M. Hart;M. Hartman;C. Haster;K. Haughian;A. Heidmann;M. Heintze;H. Heitmann;P. Hello;G. Hemming;M. Hendry;I. Heng;A. Heptonstall;M. Heurs;M. Hewitson;S. Hild;D. Hoak;K. Hodge;K. Holt;S. Hooper;P. Hopkins;D. Hosken;J. Hough;E. Howell;Yi-ming Hu;E. Huerta;B. Hughey;S. Husa;S. Huttner;M. Huynh;T. Huynh--Dinh-T.-Huynh--Dinh-1381195806;D. Ingram;R. Inta;T. Isogai;A. Ivanov;B. Iyer;K. Izumi;M. Jacobson;E. James;H. Jang;P. Jaranowski;Y. Ji;F. Jiménez-Forteza;W. Johnson;D. Jones;R. Jones;R. Jonker;L. Ju;H. K;P. Kalmus;V. Kalogera;S. Kandhasamy;G. Kang;J. Kanner;J. Karlén;M. Kasprzack;E. Katsavounidis;W. Katzman;H. Kaufer;K. Kawabe;F. Kawazoe;F. Kéfélian;G. M. Keiser;D. Keitel;D. Kelley;W. Kells;A. Khalaidovski;F. Khalili;E. Khazanov;C. Kim;K. Kim;N. Kim;N. Kim;Y. Kim;E. King;P. King;D. Kinzel;J. Kissel;S. Klimenko;J. Kline;S. Koehlenbeck;K. Kokeyama;V. Kondrashov;S. Koranda;W. Korth;I. Kowalska;D. Kozak;A. Kremin;V. Kringel;A. Królak;G. Kuehn;A. Kumar;P. Kumar;R. Kumar;L. Kuo;A. Kutynia;P. Kwee;M. Landry;B. Lantz;S. Larson;P. Lasky;C. Lawrie;A. Lazzarini;C. Lazzaro;P. Leaci;S. Leavey;E. Lebigot;C. Lee;H. Lee;H. Lee;J. Lee;M. Leonardi;J. Leong;A. Le Roux;N. Leroy;N. Letendre;Y. Levin;B. Levine;J. Lewis;T. G. F. Li;K. Libbrecht;A. Libson;A. Lin;T. Littenberg;V. Litvine;N. Lockerbie;V. Lockett;D. Lodhia;K. Loew;J. Logue;A. Lombardi;M. Lorenzini;V. Loriette;M. Lormand;G. Losurdo;J. Lough;M. Lubinski;H. Lück;Erik Luijten;A. Lundgren;R. Lynch;Y. Ma;J. Macarthur;E. Macdonald;T. Macdonald;B. Machenschalk;M. Macinnis;D. Macleod;F. Magaña-Sandoval;M. Mageswaran;C. Maglione;K. Mailand;E. Majorana;I. Maksimovic;V. Malvezzi;N. Man;G. Manca;I. Mandel;V. Mandic;V. Mangano;N. Mangini;M. Mantovani;F. Marchesoni;F. Marion;S. Márka;Z. Márka;A. Markosyan;E. Maros;J. Marque;F. Martelli;I. Martin;R. Martin;L. Martinelli;D. Martynov;J. Marx;K. Mason;A. Masserot;T. Massinger;F. Matichard

来自不同来源的引力波预计会叠加在一起，形成随机的背景。这一背景预计将包含来自整个宇宙历史的独特信息，这些信息是通过标准的电磁观测无法获得的，使其研究对理解宇宙的演化具有至关重要的意义。我们利用LIGO和Virgo探测器的最新数据对随机背景进行了搜索。与大多数随机引力波背景模型的预测一致，这些数据没有显示随机引力波信号的证据。假设引力波谱Ω_{gw}(F)=Ω_{α}(f/f_{ref})^{α}，我们在4个频段(41.5-1726赫兹)的每个频段内对背景的能量密度设定95%的置信度上限。在41.5Hz41.5Hz谱指数α=0的频段内，我们将随机背景的能量密度限制为Ω_{gw}(F)&lt；5.6×10^~(-6)。对于600-1000赫兹频段，Ω_{gw}(F)&lt；0.14(f/900赫兹)^{3}，比以前报告的最佳上限低2.5倍。我们发现Ω_{gw}(F)&lt；1.8×10^~(-4)}在170-600赫兹的谱指数为零，Ω_{gw}(F)&lt；1.0(f/1300赫兹)^{3}在1000-1726赫兹，这是以前没有设置过直接限制的频带。这四个波段的极限是随机背景下迄今为止最低的直接测量值。鉴于BICEP2实验最近声称可能存在膨胀引力波的证据，我们讨论了这些结果的含义。

Gravitational waves from a variety of sources are predicted to superpose to create a stochastic background. This background is expected to contain unique information from throughout the history of the Universe that is unavailable through standard electromagnetic observations, making its study of fundamental importance to understanding the evolution of the Universe. We carry out a search for the stochastic background with the latest data from the LIGO and Virgo detectors. Consistent with predictions from most stochastic gravitational-wave background models, the data display no evidence of a stochastic gravitational-wave signal. Assuming a gravitational-wave spectrum of Ω_{GW}(f)=Ω_{α}(f/f_{ref})^{α}, we place 95% confidence level upper limits on the energy density of the background in each of four frequency bands spanning 41.5-1726 Hz. In the frequency band of 41.5-169.25 Hz for a spectral index of α=0, we constrain the energy density of the stochastic background to be Ω_{GW}(f)<5.6×10^{-6}. For the 600-1000 Hz band, Ω_{GW}(f)<0.14(f/900 Hz)^{3}, a factor of 2.5 lower than the best previously reported upper limits. We find Ω_{GW}(f)<1.8×10^{-4} using a spectral index of zero for 170-600 Hz and Ω_{GW}(f)<1.0(f/1300 Hz)^{3} for 1000-1726 Hz, bands in which no previous direct limits have been placed. The limits in these four bands are the lowest direct measurements to date on the stochastic background. We discuss the implications of these results in light of the recent claim by the BICEP2 experiment of the possible evidence for inflationary gravitational waves.

Improved upper limits on the stochastic gravitational-wave background from 2009-2010 LIGO and Virgo data.

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