Imperial College Astrophysics Consolidated Grant 2016-2019

帝国理工学院天体物理学综合补助金 2016-2019

• 批准号: ST/N000838/1
• 负责人: Stephen Warren
• 金额: $ 263.88万
• 依托单位: Imperial College London
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2016
• 资助国家: 英国
• 起止时间: 2016 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FN000838%2F1
• 关键词: Imperial; College; Astrophysics; Consolidated; Grant

Our research in Astrophysics includes theareas of cosmology (the study of the Universe), the most distantgalaxies, exoplanets (planets around other stars), and gravitationalwaves (distortion of space-time predicted by Einstein but so far notdetected). This work will make a contribution towards answering someof the greatest questions that can be posed, including: can we findsigns of life outside the solar system? and what is the fate of theUniverse? Our work involves a combination of theory andobservations. We use cutting-edge facilities such as the Planck andHerschel satellites, and LISA Pathfinder (to be launched in 2015), andwe also develop the theory and technology that will lead to proposals for thedevelopment of the next generation of satellites and experiments.Our understanding of the nature of the Universe has changed profoundlyover the past 20 years, since it was discovered that the expansion ofthe Universe is accelerating, and as experiments, primarily thoseobserving the cosmic microwave background, have allowed the accuratemeasurement of the parameters describing the Universe - theproportions of ordinary matter (atoms), dark matter, and dark energy,and the current rate of expansion. Dark matter clumps gravitationallyand outweighs ordinary matter by a factor 5, but what it consists ofis unknown. The even greater mystery is dark energy, which is causingthe acceleration of the Universe, and which dominates the mass-energybudget. Our work in cosmology takes different approaches to answeringthese problems. But the common theme in our research is theunderstanding that advances will come through improved experimentsthat measure quantities (cosmological distances, the rate ofexpansion) more accurately. The experiments rely on better technology(e.g. measurements of polarisation of the cosmic microwavebackground), better understanding of the physics under study (theproperties of supernovae used to measure cosmological distances), andbetter data analysis techniques that improve the precision andaccuracy of the results (applying rigorously the Bayesian formalism tocomplex large datasets).No less profound for humankind has been the discovery, again over thepast 20 years, of planets around many of the nearest stars in ourgalaxy, and the first characterisation of other stellarsystems. If the ultimate goal is to discover life on other planetsthis will be achieved through successive advances in understandinghow different types of planet (rocky/gaseous, large/small) form arounddifferent types of star (old/young, active/inactive, hot/cool) atdifferent radial separations, and of how the star over its lifetimecan affect the conditions on its planets. Our work in this areaincludes theoretical work to understand the mechanisms by whichplanets form, as well as developing a deeper understanding of stellarvariability and how this can subtly bias measurements of theatmospheres of planets (possibly leading to eroneous conclusions), aswell as influence the habitability of planets.A consequence of Einstein's 1915 theory of general relativity, whichdescribes the curvature of space-time due to mass, is that massiveobjects undergoing acceleration radiate energy in the form ofgravitational waves, propagating the signal of the change of curvatureat the speed of light. Gravitational waves have yet to be detected,but their detection is one of the great goals of physics. The effectis extremely subtle, so measurements in space away from sources ofvibration and the influence of the Earth are called for. Our researchon gravitational waves centres on contributing to the development oftechnologies for use in the planned European Space Agency mission LISA(not expected to launch before 2030), and analysis of data from theLISA Pathfinder mission, to be launched in 2015, that will testprototypes of these technologies.

我们在天体物理学方面的研究包括宇宙学（宇宙的研究）、最遥远的星系、系外行星（围绕其他恒星的行星）和引力波（爱因斯坦预测但迄今为止尚未发现的时空扭曲）领域。这项工作将有助于回答一些可能提出的最重大的问题，包括：我们能否找到太阳系外的生命迹象？宇宙的命运是什么？我们的工作涉及理论和观察的结合。我们使用普朗克和赫歇尔卫星以及 LISA 探路者（将于 2015 年发射）等尖端设施，我们还开发理论和技术，为下一代卫星和实验的开发提出建议。自从发现宇宙正在加速膨胀以来，宇宙的本质在过去 20 年里发生了深刻的变化，并且随着实验（主要是观测宇宙微波背景的实验）已经允许精确测量描述宇宙的参数 - 普通物质（原子）、暗物质和暗能量的比例，以及当前的膨胀率。暗物质在引力作用下结块，比普通物质重五倍，但它的成分尚不清楚。更大的谜团是暗能量，它导致宇宙加速，并主导着质能预算。我们在宇宙学方面的工作采用不同的方法来回答这些问题。但我们研究的共同主题是认识到进步将通过改进实验来实现，这些实验可以更准确地测量数量（宇宙距离、膨胀率）。这些实验依赖于更好的技术（例如宇宙微波背景偏振的测量）、对所研究物理的更好理解（用于测量宇宙距离的超新星的特性）以及更好的数据分析技术，以提高结果的精度和准确度（严格应用贝叶斯形式主义来复杂化大型数据集）。对于人类来说同样意义深远的是，在过去的 20 年里，我们又发现了许多离我们最近的行星周围的行星。我们银河系中的恒星，以及其他恒星系统的第一个特征。如果最终目标是发现其他行星上的生命，这将通过不断进步了解不同类型的行星（岩石/气态、大/小）如何围绕不同类型的恒星（老/年轻、活跃/不活跃、热/冷）形成来实现。在不同的径向间隔下，以及恒星在其一生中如何影响其行星上的条件。我们在这一领域的工作包括理论工作，以了解行星形成的机制，以及对恒星变率以及恒星变率如何巧妙地偏差对行星大气的测量（可能导致错误的结论）以及影响行星的宜居性进行更深入的了解.爱因斯坦 1915 年的广义相对论描述了质量引起的时空弯曲，其结果是，经历加速的大质量物体会辐射能量以引力波的形式，以光速传播曲率变化的信号。引力波尚未被探测到，但探测到它们是物理学的伟大目标之一。这种影响极其微妙，因此需要在远离振动源和地球影响的太空中进行测量。我们对引力波的研究集中于为计划中的欧洲航天局 LISA 任务（预计不会在 2030 年之前发射）中使用的技术开发做出贡献，并对将于 2015 年发射的 LISA 探路者任务的数据进行分析，该任务将测试这些任务的原型技术。

项目成果

Solar Neutrino Detection Sensitivity in DARWIN via Electron Scattering

达尔文通过电子散射检测太阳中微子的灵敏度

• DOI: http://dx.10.48550/arxiv.2006.03114
• 发表时间: 2020
• 作者: Aalbers J

Reinterpretation of LHC Results for New Physics: Status and Recommendations after Run 2

新物理学对大型强子对撞机结果的重新解释：第二轮运行后的现状和建议

• DOI: http://dx.10.48550/arxiv.2003.07868
• 发表时间: 2020
• 作者: Abdallah W

Reinterpretation of LHC Results for New Physics: Status and Recommendations after Run 2

新物理学对大型强子对撞机结果的重新解释：第二轮运行后的现状和建议

• DOI: http://dx.10.3204/pubdb-2021-00016
• 发表时间: 2020
• 作者: Abdallah W

DARWIN: towards the ultimate dark matter detector

达尔文：迈向终极暗物质探测器

• DOI: 10.1088/1475-7516/2016/11/017
• 发表时间: 2016-06-22
• 期刊: Journal of Cosmology and Astroparticle Physics
• 影响因子: 6.4
• 作者: J. Aalbers;F. Agostini;M. Alfonsi;F. Amaro;C. Amsler;E. Aprile;L. Arazi;F. Arneodo;P. Barrow
• 通讯作者: P. Barrow

Improved limits on dark matter annihilation in the Sun with the 79-string IceCube detector and implications for supersymmetry

使用 79 弦 IceCube 探测器改进了对太阳暗物质湮灭的限制以及对超对称性的影响

• DOI: 10.1088/1475-7516/2016/04/022
• 发表时间: 2016-01-04
• 期刊: Journal of Cosmology and Astroparticle Physics
• 影响因子: 6.4
• 作者: I. C. M. Aartsen;K. Abraham;M. Ackermann;J. Adams;J. Aguilar;M. Ahlers;M. Ahrens;D. Altmann;T. Anderson;I. Ansseau;G. Anton;M. Archinger;C. Arguelles;T. Arlen;J. Auffenberg;X. Bai;S. Barwick;V. Baum;R. Bay;J. Beatty;J. Tjus;K. Becker;E. Beiser;S. BenZvi;P. Berghaus;D. Berley;E. Bernardini;A. Bernhard;D. Besson;G. Binder;D. Bindig;M. Bissok;E. Blaufuss;J. Blumenthal;D. Boersma;C. Bohm;M. Borner;F. Bos;D. Bose;S. Boser;O. Botner;J. Braun;L. Brayeur;H. Bretz;N. Buzinsky;J. Casey;M. Casier;E. Cheung;D. Chirkin;A. Christov;K. Clark;L. Classen;S. Coenders;G. Collin;J. Conrad;D. Cowen;A. H. C. Silva;M. Danninger;J. Daughhetee;J. Davis;M. Day;J. Andr'e;C. Clercq;E. del Pino Rosendo;H. Dembinski;S. Ridder;P. Desiati;K. D. Vries;G. Wasseige;M. With;T. DeYoung;J. C. D'iaz;V. Lorenzo;J. Dumm;M. Dunkman;B. Eberhardt;J. Edsjo;T. Ehrhardt;B. Eichmann;S. Euler;P. Evenson;S. Fahey;A. Fazely;J. Feintzeig;J. Felde;K. Filimonov;C. Finley;S. Flis;C.;T. Fuchs;T. Gaisser;R. Gaior;J. Gallagher;L. Gerhardt;K. Ghorbani;D. Gier;L. Gladstone;M. Glagla;T. Glusenkamp;A. Goldschmidt;G. Golup;J. G. Gonzalez;D. G'ora;D. Grant;Z. Griffith;A. Gross;C. Ha;C. Haack;A. H. Ismail;A. Hallgren;F. Halzen;E. Hansen;B. Hansmann;K. Hanson;D. Hebecker;D. Heereman;K. Helbing;R. Hellauer;S. Hickford;J. Hignight;G. Hill;K. Hoffman;R. Hoffmann;K. Holzapfel;A. Homeier;K. Hoshina;F. Huang;M. Huber;W. Huelsnitz;P. O. Hulth;K. Hultqvist;S. In;A. Ishihara;E. Jacobi;G. Japaridze;M. Jeong;K. Jero;B. Jones;M. Jurkovič;A. Kappes;T. Karg;A. Karle;U. Katz;M. Kauer;A. Keivani;J. Kelley;J. Kemp;A. Kheir;ish;ish;J. Kiryluk;S. Klein;G. Kohnen;R. Koirala;H. Kolanoski;R. Konietz;L. Kopke;C. Kopper;S. Kopper;D. Koskinen;M. Kowalski;K. Krings;G. Kroll;M. Kroll;G. Kruckl;J. Kunnen;N. Kurahashi;T. Kuwabara;M. Labare;J. Lanfranchi;M. Larson;M. Lesiak;M. Leuermann;J. Leuner;L. Lu;J. Lunemann;J. Madsen;G. Maggi;K. Mahn;M. M;elartz;elartz;R. Maruyama;K. Mase;H. Matis;R. Maunu;F. McNally;K. Meagher;M. Medici;M. Meier;A. Meli;T. Menne;G. Merino;T. Meures;S. Miarecki;E. Middell;L. Mohrmann;T. Montaruli;R. Morse;R. Nahnhauer;U. Naumann;G. Neer;H. Niederhausen;S. Nowicki;D. Nygren;A. Pollmann;A. Olivas;A. Omairat;A. O'Murchadha;T. Palczewski;H. P;ya;ya;D. Pankova;L. Paul;J. Pepper;C. Heros;C. Pfendner;D. Pieloth;E. Pinat;J. Posselt;P. Price;G. Przybylski;M. Quinnan;C. Raab;L. Radel;M. Rameez;K. Rawlins;R. Reimann;M. Relich;E. Resconi;W. Rhode;M. Richman;S. Richter;B. Riedel;S. Robertson;M. Rongen;C. Rott;T. Ruhe;D. Ryckbosch;L. Sabbatini;H. S;er;er;A. S;rock;rock;J. S;roos;roos;S. Sarkar;C. Savage;K. Schatto;M. Schimp;P. Schlunder;T. Schmidt;S. Schoenen;S. Schoneberg;A. Schonwald;L. Schulte;L. Schumacher;P. Scott;D. Seckel;S. Seunarine;H. Silverwood;D. Soldin;M. Song;G. Spiczak;C. Spiering;M. Stahlberg;M. Stamatikos;T. Stanev;Ale;er Stasik;er;A. Steuer;T. Stezelberger;R. Stokstad;A. Stossl;R. Strom;N. Strotjohann;G. Sullivan;M. Sutherl;H. Taavola;I. Taboada;J. Tatar;S. Ter;A. Terliuk;G. Tevsi'c;S. Tilav;P. Toale;M. Tobin;S. Toscano;D. Tosi;M. Tselengidou;A. Turcati;E. Unger;M. Usner;S. Vallecorsa;J. V;enbroucke;enbroucke;N. Eijndhoven;S. Vanheule;J. Santen;J. Veenkamp;M. Vehring;M. Voge;M. Vraeghe;C. Walck;A. Wallace;M. Wallraff;N. W;kowsky;kowsky;C. Weaver;C. Wendt;S. Westerhoff;B. Whelan;K. Wiebe;C. Wiebusch;L. Wille;D. Williams;L. Wills;H. Wissing;M. Wolf;T. R. Wood;K. Woschnagg;D. Xu;X. Xu;Y. Xu;J. Yáñez;G. Yodh;S. Yoshida;M. Zoll
• 通讯作者: M. Zoll