Investigations in gravitational radiation

引力辐射研究

• 批准号: ST/V005707/1
• 负责人: Matthew Pitkin
• 金额: $ 4.37万
• 依托单位: Lancaster University
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2021
• 资助国家: 英国
• 起止时间: 2021 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FV005707%2F1
• 关键词: Investigations; gravitational; radiation

Einstein's General Relativity predicts that dynamical systems in strong gravitational fields will emit vast amounts of energy in the form of gravitational waves (GW). These are ripples in the very fabric of spacetime that travel from their sources at the speed of light, carrying information about physical processes responsible for their emission. They are among the most elusive signals from the deepest reaches in the Universe.In September 2015, during the 1st Advanced LIGO observing run, gravitational waves from the collision of two black holes were discovered using the LIGO observatories. The detection of GW150914 resulted in the award of the 2017 Nobel Prize in Physics with explicit recognition of the role of the UK as a critical part of the global team.In August 2017, during the 2nd observing run, LIGO and Virgo detected the first gravitational wave signal from the collision of two neutron stars. GW170817 was observed in coincidence with a gamma-ray burst (GRB) as well as signals across the electromagnetic spectrum, including the optical and infra-red signature of a kilonova. These discoveries have established a new paradigm of multi-messenger astrophysicsThe 3rd observing run of Advanced LIGO and Advanced Virgo (AdV), O3, started on 1st April 2019 and ended in March 2020 during the end of which time the Japanese KAGRA instrument joined the observing network. Modelling GW sources has allowed deeper searches and data from LIGO, Virgo, and GEO have increased our understanding of astronomical phenomena.We are now able to make regular observations of GWs. To date close to 60 observations of coalescing objects, with an unexpectedly wide range of masses, have been made, with event rates being approximately 1 per week. We now have evidence for the existence of black hole/neutron star binaries, the existence of objects in the mass gap between accepted neutron star masses and black hole masses and the first real experimental evidence for the existence of intermediate mass black holes.The aLIGO detectors are based on the quasi-monolithic silica suspension concept developed in the UK for GEO600 and on the high-power lasers developed by our German colleagues in GEO600. The AdV detector also uses a variant of the silica suspension technology. Further, KAGRA is being built with input on cryogenic bonding technology from the UK groups.The consortium groups have led searches for astronomical sources, thanks to funding support received, since first data taking runs began 18 years ago. Key ingredients of several searches were developed at Glasgow.We propose a programme that exploits data from aLIGO, AdV, and KAGRA building on our analysis of data from the most recent LIGO/Virgo science runs. In particular we will observe and analyse signals from the LIGO/Virgo/KAGRA detector network with particular emphasis on compact binary inference, population and cosmological measurements - measurement of the Hubble Constant and tests of General Relativity, application of machine learning techniques for increased efficiency in modelling signals, performing searches, etc, and the search for gravitational wave emission from neutron stars.In parallel, we propose essential detector R&D. 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 in sensing. Our research is targeted towards making innovative improvements in these areas, essential to maximise the astrophysical potential of GW observatories.We have major responsibilities for the silica suspensions in aLIGO, and in the development of enhancements and upgrades to the aLIGO detectors (to form aLIGO+), along with R&D in the areas of mirror coatings for low thermal noise, silicon substrates, cryogenic suspensions and improved interferometer topologies to combat quantum noise.

爱因斯坦的一般相对论预测，强力引力场中的动力系统将以引力波（GW）的形式发出大量能量。这些是时空的涟漪，它以光速从源头传播，携带有关负责发射的物理过程的信息。它们是宇宙中最深处的最难以捉摸的信号之一。在2015年9月，在第一个高级Ligo观察过程中，使用Ligo天文台发现了两个黑洞的碰撞引力波。 GW150914的检测导致了2017年诺贝尔物理学奖的奖励，并明确认识了英国作为全球团队的关键部分的作用。在2017年8月，在第二次观察跑步期间，Ligo和Pirgo在两位中子星的碰撞中发现了第一个引力波。 GW170817与伽马射线爆发（GRB）以及跨电磁频谱的信号相吻合，包括Kilonova的光学和红外签名。这些发现建立了一个新的多通信天天体物理学范式，第三个观察，即高级里戈和高级处女座（ADV），O3，于2019年4月1日开始，并于2020年3月在日本Kagra仪器结束时结束了。建模GW来源允许Ligo，处女座和GEO的更深入的搜索和数据增加了我们对天文现象的理解。我们现在能够定期观察GWS。迄今为止，已经进行了近60个共聚物的观察结果，其中已经进行了大量群体，事件速率约为每周1个。现在，我们有证据表明存在黑洞/中子星二进制文件，在公认的中子星质量和黑洞质量和黑洞质量之间存在质量差距中的物体以及第一个真正的实验证据，是存在中间质量黑洞的存在。 Geo600。 ADV检测器还使用二氧化硅悬浮技术的变体。此外，Kagra是由英国集团对低温键合技术的投入来建立的。由于收到的资金支持，该财团集团已领导了对天文来源的搜索，因为自18年前开始进行了第一次数据。我们在格拉斯哥开发了几种搜索的关键要素。我们提出了一项程序，该程序利用Aligo，Adv和Kagra Building的数据来利用我们对最新Ligo/Ligo/处女座科学运行的数据的分析。特别是，我们将观察和分析来自Ligo/处女座/Kagra探测器网络的信号，特别强调紧凑型二进制推理，人口和宇宙学测量 - 测量伙伴常数和一般相对性的测试，机器学习技术的应用，以增加机器学习技术的效率，以增加效率，并提高搜索搜索，并在搜索中搜索，以及搜索型的搜索，以及从中的搜索，我们从中搜索了良好的gravtity sequose sequose sequose sequose sequose sequose sequine starsion sequins starsion starsion starsion starsion starsion。研发。检测器灵敏度主要受热噪声，与镜子的底物，反射涂层以及它们的悬浮元素以及噪声相关的热噪声限制，以及由传感中使用的光的量子性质产生的噪声。 Our research is targeted towards making innovative improvements in these areas, essential to maximise the astrophysical potential of GW observatories.We have major responsibilities for the silica suspensions in aLIGO, and in the development of enhancements and upgrades to the aLIGO detectors (to form aLIGO+), along with R&D in the areas of mirror coatings for low thermal noise, silicon substrates, cryogenic suspensions and improved干涉仪拓扑作用以对抗量子噪声。

项目成果

Searches for continuous gravitational waves from young supernova remnants in the early third observing run of Advanced LIGO and Virgo

• DOI: 10.3847/1538-4357/ac17ea
• 发表时间: 2021-05
• 期刊: The Astrophysical Journal

Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo窶冱 first three observing runs

使用 Advanced LIGO 和 Advanced Virgo 前三次观测运行的数据搜索各向异性引力波背景

• DOI: 10.1103/physrevd.104.022005
• 发表时间: 2021
• 期刊: Physical Review D
• 影响因子: 5
• 作者: R. Abbott et al.

Population synthesis and parameter estimation of neutron stars with continuous gravitational waves and third-generation detectors

连续引力波和第三代探测器的中子星星群合成与参数估计

• DOI: 10.1093/mnras/stad3811
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Hua Y

All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

• DOI: 10.1103/physrevd.104.102001
• 发表时间: 2021-07
• 作者: The Ligo Scientific Collaboration;The Virgo Collaboration;T. Abbott;T. Abbott;F. Acernese;K. Ackley;C. Adams;N. Adhikari;R. Adhikari;V. Adya;C. Affeldt;D. Agarwal;M. Agathos;K. Agatsuma;N. Aggarwal;O. Aguiar;L. Aiello;A. Ain;P. Ajith;T. Akutsu;S. Albanesi;A. Allocca;P. Altin;A. Amato;C. Anand;S. Anand;A. Ananyeva;S. Anderson;W. Anderson;M. Ando;T. Andrade;N. Andrés;T. Andri'c;S. Angelova;S. Ansoldi;J. Antelis;S. Antier;S. Appert;K. Arai;K. Arai;Y. Arai;S. Araki;A. Araya;M. Araya;J. Areeda;M. Arène;N. Aritomi;N. Arnaud;S. Aronson;K. Arun;H. Asada;Y. Asali;G. Ashton;Y. Aso;M. Assiduo;S. Aston;P. Astone;F. Aubin;C. Austin;S. Babak;F. Badaracco;M. Bader;C. Badger;S. Bae;Y. Bae;A. Baer;S. Bagnasco;Y. Bai;L. Baiotti;J. Baird;R. Bajpai;M. Ball;G. Ballardin;S. Ballmer;A. Balsamo;G. Baltus;S. Banagiri;D. Bankar;J. Barayoga;C. Barbieri;B. Barish;D. Barker;P. Barneo;F. Barone;B. Barr;L. Barsotti;M. Barsuglia;D. Barta;J. Bartlett;M. Barton;I. Bartos;R. Bassiri;A. Basti;M. Bawaj;J. Bayley;A. Baylor;M. Bazzan;B. B'ecsy;V. Bedakihale;M. Bejger;I. Belahcene;V. Benedetto;D. Beniwal;T. Bennett;J. Bentley;M. BenYaala;F. Bergamin;B. Berger;S. Bernuzzi;D. Bersanetti;A. Bertolini;J. Betzwieser;D. Beveridge;R. Bhandare;U. Bhardwaj;D. Bhattacharjee;S. Bhaumik;I. Bilenko;G. Billingsley;S. Bini;R. Birney;O. Birnholtz;S. Biscans;M. Bischi;S. Biscoveanu;A. Bisht;B. Biswas;M. Bitossi;M. Bizouard;J. Blackburn;C. Blair;D. Blair;R. Blair;F. Bobba;N. Bode;M. Boer;G. Bogaert;M. Boldrini;L. D. Bonavena;F. Bondu;E. Bonilla;R. Bonnand;P. Booker;B. A. Boom;R. Bork;V. Boschi;N. Bose;S. Bose;V. Bossilkov;V. Boudart;Y. Bouffanais;A. Bozzi;C. Bradaschia;P. Brady;A. Bramley;A. Branch;M. Branchesi;J. Brau;M. Breschi;T. Briant;J. Briggs;A. Brillet;M. Brinkmann;P. Brockill;A. Brooks;J. Brooks;D. Brown;S. Brunett;G. Bruno;R. Bruntz;J. Bryant;T. Bulik;H. Bulten;A. Buonanno;R. Buscicchio;D. Buskulic;C. Buy;R. Byer;L. Cadonati;G. Cagnoli;C. Cahillane;J. C. Bustillo;J. Callaghan;T. Callister;E. Calloni;J. 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Fornal;P. Forsyth;A. Franke;S. Frasca;F. Frasconi;C. Frederick;J. Freed;Z. Frei;A. Freise;R. Frey;P. Fritschel;V. Frolov;G. G. Fronz'e-G.;Y. Fujii;Y. Fujikawa;M. Fukunaga;M. Fukushima;P. Fulda;M. Fyffe;H. Gabbard;B. Gadre;J. Gair;J. Gais;S. Galaudage;R. Gamba;D. Ganapathy;A. Ganguly;D. Gao;S. Gaonkar;B. Garaventa;C. Garc'ia-N'unez;C. Garc'ia-Quir'os;F. Garufi;B. Gateley;S. Gaudio;V. Gayathri;G. Ge;G. Gemme;A. Gennai;J. George;O. Gerberding;L. Gergely;P. Gewecke;S. Ghonge;A. Ghosh;A. Ghosh;Shaon Ghosh;Shrobana Ghosh;B. Giacomazzo;L. Giacoppo;J. Giaime;K. Giardina;D. Gibson;C. Gier;M. Giesler;P. Giri;F. Gissi;J. Glanzer;A. Gleckl;P. Godwin;E. Goetz;R. Goetz;N. Gohlke;B. Goncharov;G. Gonz'alez;A. Gopakumar;M. Gosselin;R. Gouaty;D. Gould;B. Grace;A. Grado;M. Granata;V. Granata;A. Grant;S. Gras;P. Grassia;C. Gray;R. Gray;G. Greco;A. Green;R. Green;A. Gretarsson;E. Gretarsson;D. Griffith;W. Griffiths;H. L. Griggs;G. Grignani;A. Grimaldi;S. Grimm;H. Grote;S. Grunewald;P. Gruning;D. Guerra;G. Guidi;A. R. Guimaraes;G. Guix'e;H. Gulati;H.-K. Guo;Y. Guo;Anchal Gupta;Anuradha Gupta;P. Gupta;E. Gustafson;R. Gustafson;F. Guzmán;S. Ha;L. Haegel;A. Hagiwara;S. Haino;O. Halim;E. Hall;E. Hamilton;G. Hammond;W. Han;M. Haney;J. Hanks;C. Hanna;M. Hannam;O. Hannuksela;H. Hansen;T. Hansen;J. Hanson;T. Harder;T. Hardwick;K. Haris;J. Harms;G. Harry;I. Harry;D. Hartwig;K. Hasegawa;B. Haskell;R. Hasskew;C. Haster;K. Hattori;K. Haughian;H. Hayakawa;K. Hayama;F. Hayes;J. Healy;A. Heidmann;A. Heidt;M. Heintze;J. Heinze;J. Heinzel;H. Heitmann;F. Hellman;P. Hello;A. Helmling-Cornell;G. Hemming;M. Hendry;I. Heng;E. Hennes;J. Hennig;M. Hennig;A. Hernandez;F. Vivanco;M. Heurs;S. Hild;P. Hill;Y. Himemoto;A. Hines;Y. Hiranuma;N. Hirata;E. Hirose;S. Hochheim;D. Hofman;J. Hohmann;D. Holcomb;N. Holland;I. J. Hollows;Z. J. Holmes;K. Holt;D. Holz;Z. Hong;P. Hopkins;J. Hough;S. Hourihane;E. Howell;C. Hoy;D. Hoyland;A. Hreibi;B. Hsieh;Y. Hsu;G-Z. Huang;H. Huang;P. Huang;Y. Huang;Y. Huang;Y. Huang;M. Hubner;A. Huddart;B. Hughey;D. Hui;V. Hui;S. Husa;S. Huttner;R. Huxford;T. Huynh--Dinh-T.-Huynh--Dinh-1381195806;S. Ide;B. Idzkowski;A. Iess;B. Ikenoue;S. Imam;K. Inayoshi;C. Ingram;Y. Inoue;K. Ioka;M. Isi;K. Isleif;K. Ito;Y. Itoh;B. Iyer;K. Izumi;V. JaberianHamedan;T. Jacqmin;S. Jadhav;S. Jadhav;A. L. James;A. Jan;K. Jani;J. Janquart;K. Janssens;N. Janthalur;P. Jaranowski;D. Jariwala;R. Jaume;A. Jenkins;K. Jenner;C. Jeon;M. Jeunon;W. Jia;H. Jin;G. Johns;A. W. Jones;D. Jones;J. Jones;P. Jones;R. Jones;R. Jonker;L. Ju;P. Jung;K. Jung;J. Junker;V. Juste;K. Kaihotsu;T. Kajita;M. Kakizaki;C. Kalaghatgi;V. Kalogera;B. Kamai;M. Kamiizumi;N. Kanda;S. Kandhasamy;G. Kang;J. Kanner;Y. Kao;S. Kapadia;D. Kapasi;S. Karat;C. Karathanasis;S. Karki;R. Kashyap;M. Kasprzack;W. Kastaun;S. Katsanevas;E. Katsavounidis;W. Katzman;T. Kaur;K. Kawabe;K. Kawaguchi;N. Kawai;T. Kawasaki;F. K'ef'elian;D. Keitel;J. Key;S. Khadka;F. Khalili;S. Khan;E. Khazanov;N. Khetan;M. Khursheed;N. Kijbunchoo;C. Kim;J. Kim;J. 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Nested sampling for physical scientists

• DOI: 10.1038/s43586-022-00121-x
• 发表时间: 2022-05-26
• 期刊: NATURE REVIEWS METHODS PRIMERS
• 作者: Ashton, Greg;Bernstein, Noam;Yallup, David
• 通讯作者: Yallup, David