Investigations in Gravitational Radiation

引力辐射研究

• 批准号: ST/I001085/1
• 负责人: Sheila Rowan
• 金额: $ 270.37万
• 依托单位: University of Glasgow
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2010
• 资助国家: 英国
• 起止时间: 2010 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FI001085%2F1
• 关键词: Investigations; Gravitational; Radiation

Einstein's General Theory of Relativity (GR) predicts that dynamical systems in strong gravitational fields will release vast amounts of energy in the form of gravitational radiation. Gravitational waves are ripples in the fabric of spacetime and travel from their sources at the speed of light, carrying information about physical processes responsible for their emission, obtainable in no other way. They are among the most elusive signals from the deepest reaches in the Universe. Experiments aimed at detecting them have been in development for several decades, but only now are sensitivities reaching levels where real detection is possible within a few years. The worldwide network of interferometric detectors includes the German-UK GEO600, the French-Italian Virgo and the American Laser Interferometer Gravitational-Wave Observatory (LIGO). These detectors have all reached sensitivities close to their design goals and have taken the most sensitive data to date. Cooperation amongst different projects enables continuous data acquisition, with sensitivity to a wide range of sources and phenomena, over most of the sky. Data from GEO, LIGO and Virgo, has already begun to impact our understanding of astronomical phenomena. For example, the most recent observations with these detectors have (a) shown that less than 2% of the Crab pulsar's radiated power is in gravitational waves, (b) ruled out merging binary neutron stars as the progenitor of GRB 070201 (if it occurred in M31) and (c) set a new best upper limit on the strength of the stochastic gravitational-wave background. While the present phase of observations (circa 2010-2011) have a real chance of producing the first detections - possibly from compact binary coalescences, there can be no guarantees. However there is great confidence that the advanced detectors will routinely observe gravitational waves. The Cardiff and Glasgow groups have initiated and led searches for astronomical sources, thanks to the algorithmic and analysis effort that has been supported since the first data taking runs began eight years ago. We propose a programme of continued improvement to GEO600 and to be involved in the characterization and analysis of the resulting data from GEO and the worldwide network of interferometers. In particular we will be carrying out searches for * coalescing binary neutron stars, neutron star-black hole binaries, and black hole binaries * bursts of gravitational waves that may originate from supernovae, and * continuous signals from pulsars and other rotating neutron stars. In parallel, we are proposing research and development on the detector front. Detector sensitivity is mainly limited by thermal noise associated with the substrates of the mirrors, their reflective coatings, and their suspension elements, as well as by noise resulting from the quantum nature of the light used to provide illumination. Thus our research is targeted towards making innovative improvements in these areas. In particular we are taking leading roles in the upgrading of GEO and LIGO in the areas of silica suspensions, optics and interferometry, and for enhancements to the Advanced LIGO program and future interferometers in the areas of dielectric and waveguide mirror coatings, silicon substrates and cryogenic suspensions. In summary, the goal of the Glasgow, Cardiff and Strathclyde groups is to lead the first direct detection of gravitational waves using detectors based on their innovative developments. Once this milestone is achieved, routine observations will help us use this radiation as an observational and theoretical tool to understand * cores of supernovae and neutron stars, * gamma-ray burst engines, * the interactions of black holes and neutron stars, etc. In particular, coalescing compact binaries are self-calibrating standard candles, or sirens, which will be a new precision tool for cosmology and will enable strong field tests of general relativity.

爱因斯坦的相对论一般理论（GR）预测，强力引力场中的动力系统将以引力辐射的形式释放大量能量。引力波在时空的结构中是涟漪，并以光速从其来源传播，携带有关其发射的物理过程的信息，无法以其他方式获得。它们是宇宙中最深处的最难以捉摸的信号之一。旨在检测它们的实验已经开发了几十年，但直到现在才达到了几年内实现实际检测水平的敏感性。全球干涉探测器网络包括德国 - 墨西哥Geo600，法国 - 意大利处女座和美国激光干涉仪重力波观测站（LIGO）。这些探测器都达到了接近其设计目标的敏感性，并采用了迄今为止最敏感的数据。在不同项目之间的合作可以使数据获取不断获取，并对大多数天空的敏感性对广泛的来源和现象敏感。 Geo，Ligo和处女座的数据已经开始影响我们对天文现象的理解。例如，使用这些探测器的最新观察结果（a）表明，螃蟹脉冲星的辐射功率的不到2％是在引力波中，（b）排除将二进制中子星合并为GRB 070201的祖先（如果它在M31中）和（c）对施加力的高度强度建立了新的上限。尽管目前的观测阶段（大约2010-2011）有真正的机会产生第一个检测 - 可能是从紧凑型二元合并时出现的，但无法保证。但是，人们对高级探测器通常会观察到引力波的信心。加的夫和格拉斯哥团体已经启动并领导了对天文来源的搜索，这要归功于自八年前开始进行第一批数据以来的算法和分析工作。我们提出了一个对GEO600的持续改进的程序，并参与了GEO和全球干涉仪网络所得数据的表征和分析。特别是，我们将搜索 *合并的二进制中子星，中子星状孔二进制二进制和黑洞二进制 *可能源自超新星的引力波和 *脉冲星和其他旋转中子星的连续信号。同时，我们正在提议在探测器方面进行研发。检测器敏感性主要受热噪声的限制，与镜子的底物，它们的反射涂层以及它们的悬浮元件以及由用于提供照明的光的量子性质所产生的噪声。因此，我们的研究旨在在这些领域进行创新的改进。特别是，我们在二氧化硅悬浮液，光学和干涉测量方面的地理和Ligo升级方面发挥了主导作用，并在介电和波导镜涂层，硅底物和低温悬液的区域中提高了先进的LIGO程序和未来的干涉仪。总而言之，格拉斯哥，加的夫和Strathclyde群体的目标是使用基于其创新发展的探测器首次直接检测引力波。一旦实现了这个里程碑，常规观察将帮助我们将这种辐射用作理论的观察和理论工具，以理解 *超新星和中子星的核心， *伽玛 - 射线爆发引擎， *黑洞和中子星和中子星等的相互作用。相对论。

项目成果

The NINJA-2 project: Detecting and characterizing gravitational waveforms modelled using numerical binary black hole simulations

• DOI: 10.1088/0264-9381/31/11/115004
• 发表时间: 2014-01
• 作者: The Ligo Scientific Collaboration;The Virgo Collaboration;T. V. C. 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. K. 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. Bruckner;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. Del'eglise;W. D. Pozzo;T. Denker;T. Dent;H. Dereli;V. Dergachev;R. Rosa;R. Derosa;R. DeSalvo;S. Dhurandhar;M. D'iaz;L. Fiore;A. Lieto;I. Palma;A. 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. EndrHoczi;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. Gonz'alez;N. Gordon;M. Gorodetsky;S. Gossan;S. Gossler;R. Gouaty;C. Graf;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;Y. Hu;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. Jim'enez-Forteza;W. Johnson;D. Jones;R. Jones;R. Jonker;L. Ju;K. Haris;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. K'ef'elian;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;B. Krishnan;A. Kr'olak;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. L. 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. Luck;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. M'arka;Z. M'arka;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;L. Matone;R. Matzner;N. Mavalvala;N. Mazumder;G. Mazzolo;R. McCarthy-;D. McClelland;S. Mcguire;G. Mcintyre;J. McIver;K. McLin;D. Meacher;G. Meadors;M. Mehmet;J. Meidam;M. Meinders;A. Melatos;G. Mendell;R. Mercer;S. Meshkov;C. Messenger;P. Meyers;H. Miao;C. Michel;E. Mikhailov;L. Milano;S. Milde;J. Miller;Y. Minenkov;C. Mingarelli;C. Mishra;S. Mitra;V. Mitrofanov;G. Mitselmakher;R. Mittleman;B. Moe;P. Moesta;M. Mohan;S. Mohapatra;D. Moraru;G. Moreno;N. Morgado;S. Morriss;K. Mossavi;B. Mours;C. Mow-Lowry;C. Mueller;G. Mueller;S. Mukherjee;A. Mullavey;J. Munch;D. Murphy;P. Murray;A. Mytidis;M. Nagy;D. Kumar;I. Nardecchia;L. Naticchioni;R. Nayak;V. Necula;G. Nelemans;I. Neri;M. Neri;G. Newton;T. Nguyen;A. Nitz;F. Nocera;D. Nolting;M. Normandin;L. Nuttall;E. Ochsner;J. O'Dell;E. Oelker;J. Oh;S. Oh;F. Ohme;P. Oppermann;B. O'reilly;R. O’Shaughnessy;C. Osthelder;D. Ottaway;R. Ottens;H. Overmier;B. Owen;C. Padilla;A. Pai;O. Palashov;C. Palomba;H. Pan;Y. Pan;C. Pankow;F. Paoletti;R. Paoletti;M. Papa;H. Paris;A. Pasqualetti;R. Passaquieti;D. Passuello;M. Pedraza;S. Penn;A. Perreca;M. Phelps;M. Pichot;M. Pickenpack;F. Piergiovanni;V. Pierro;L. Pinard;I. Pinto;M. Pitkin;J. Poeld;R. Poggiani;A. Poteomkin;J. Powell;J. Prasad;S. Premachandra;T. Prestegard;L. Price;M. Prijatelj;S. Privitera;G. Prodi;L. Prokhorov;O. Puncken;M. Punturo;P. Puppo;J. Qin;V. Quetschke;E. Quintero;G. Quiroga;R. Quitzow-James;F. Raab;D. Rabeling;I. R'acz;H. Radkins;P. Raffai;S. Raja;G. Rajalakshmi;M. Rakhmanov;C. Ramet;K. Ramirez;P. Rapagnani;V. Raymond;V. Re;J. Read;C. Reed;T. Regimbau;S. Reid;D. Reitze;E. Rhoades;F. Ricci;K. Riles;N. Robertson;F. Robinet;A. Rocchi;M. Rodruck;L. Rolland;J. Rollins;R. Romano;G. Romanov;J. Romie;D. Rosi'nska;S. Rowan;A. Rudiger;P. Ruggi;K. Ryan;F. Salemi;L. Sammut;V. Sandberg;J. Sanders;V. Sannibale;I. Santiago-Prieto;E. Saracco;B. Sassolas;B. Sathyaprakash;P. Saulson;R. Savage;J. Scheuer;R. Schilling;R. Schnabel;R. Schofield;E. Schreiber;D. Schuette;B. Schutz;J. Scott;S. Scott;D. Sellers;A. Sengupta;D. Sentenac;V. Sequino;A. Sergeev;D. Shaddock;S. Shah;M. Shahriar;M. Shaltev;B. Shapiro;P. Shawhan;D. Shoemaker;T. Sidery;K. Siellez;X. Siemens;D. Sigg;D. Simakov;A. Singer;L. Singer;R. Singh;A. Sintes;B. Slagmolen;J. Slutsky;J. R. Smith;M. Smith;R. Smith;N. Smith-Lefebvre;E. Son;B. Sorazu;T. Souradeep;L. Sperandio;A. Staley;J. Stebbins;J. Steinlechner;S. Steinlechner;B. Stephens;S. Steplewski;S. Stevenson;R. Stone;D. Stops;K. Strain;N. Straniero;S. Strigin;R. Sturani;A. Stuver;T. Summerscales;S. Susmithan;P. Sutton;B. Swinkels;M. Tacca;D. Talukder;D. Tanner;S. Tarabrin;R. Taylor;A. Braack;M. Thirugnanasambandam;M. Thomas;P. Thomas;K. Thorne;K. Thorne;E. Thrane;V. Tiwari;K. Tokmakov;C. Tomlinson;A. Toncelli;M. Tonelli;O. Torre;C. Torres;C. Torrie;F. Travasso;G. Traylor;M. Tse;D. Ugolini;C. Unnikrishnan;A. Urban;K. Urbanek;H. Vahlbruch;G. Vajente;G. Valdes;M. Vallisneri;J. Brand;C. Broeck;S. V. D. Putten;M. V. D. Sluys;J. V. Heijningen;A. V. Veggel;S. Vass;M. Vas'uth;R. Vaulin;A. Vecchio;G. Vedovato;J. Veitch;P. Veitch;K. Venkateswara;D. Verkindt;S. Verma;F. Vetrano;A. Vicer'e;R. Vincent-Finley;J. Vinet;S. Vitale;T. Vo;H. Vocca;C. Vorvick;W. Vousden;S. Vyachanin;A. Wade;L. Wade;M. Wade;M. Walker;L. Wallace;M. Wang;X. Wang;R. Ward;M. Was;B. Weaver;L.-W. Wei;M. Weinert;A. Weinstein;R. Weiss;T. Welborn;L. Wen;P. Wessels;M. West;T. Westphal;K. Wette;J. Whelan;S. Whitcomb;D. White;B. Whiting;K. Wiesner;C. Wilkinson;K. Williams;L. Williams;R. Williams;T. Williams;A. Williamson;J. Willis;B. Willke;M. Wimmer;W. Winkler;C. Wipf;A. Wiseman;H. Wittel;G. Woan;J. Worden;J. Yablon;I. Yakushin;H. Yamamoto;C. Yancey;H. Yang;Z. Yang;S. Yoshida;M. Yvert;A. Zadro.zny;M. Zanolin;J. Zendri;Fan Zhang;L. Zhang;C. Zhao;X. Zhu;M. Zucker;S. Zuraw;J. Zweizig;M. Boyle;B. Brugmann;L. Buchman;M. Campanelli;T. Chu;Z. Etienne;M. Hannam;J. Healy;I. Hinder;L. Kidder;P. Laguna;Y. T. Liu;L. London;C. Lousto;G. Lovelace;I. MacDonald;P. Marronetti;P. Mosta;D. Muller;B. Mundim;H. Nakano;V. Paschalidis;L. Pekowsky;D. Pollney;H. Pfeiffer;M. Ponce;M. Purrer;G. Reifenberger;C. Reisswig;L. Santamar'ia;M. Scheel;S. Shapiro;D. Shoemaker;C. Sopuerta;U. Sperhake;B. Szil'agyi;N. W. Taylor;W. Tichy;P. Tsatsin;Y. Zlochower

IMPLICATIONS FOR THE ORIGIN OF GRB 051103 FROM LIGO OBSERVATIONS

• DOI: 10.1088/0004-637x/755/1/2
• 发表时间: 2012-08-10
• 期刊: ASTROPHYSICAL JOURNAL
• 影响因子: 4.9
• 作者: Abadie, J.;Abbott, B. P.;Was, M.
• 通讯作者: Was, M.

SEARCH FOR GRAVITATIONAL WAVES ASSOCIATED WITH GAMMA-RAY BURSTS DURING LIGO SCIENCE RUN 6 AND VIRGO SCIENCE RUNS 2 AND 3

• DOI: 10.1088/0004-637x/760/1/12
• 发表时间: 2012-11-20
• 期刊: ASTROPHYSICAL JOURNAL
• 影响因子: 4.9
• 作者: Abadie, J.;Abbott, B. P.;Zhang, X. -L.
• 通讯作者: Zhang, X. -L.

All-sky search for periodic gravitational waves in the full S5 LIGO data

在完整的 S5 LIGO 数据中全天搜索周期性引力波

• DOI: 10.1103/physrevd.85.022001
• 发表时间: 2012
• 期刊: Physical Review D
• 影响因子: 5
• 作者: Abadie J

The characterization of Virgo data and its impact on gravitational-wave searches

• DOI: 10.1088/0264-9381/29/15/155002
• 发表时间: 2012-08-07
• 期刊: CLASSICAL AND QUANTUM GRAVITY
• 影响因子: 3.5
• 作者: Aasi, J.;Abadie, J.;Zweizig, J.
• 通讯作者: Zweizig, J.