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Pinpointing the Origin of Noisy Compact Binary Mergers

查明嘈杂的紧凑型二元合并的根源

基本信息

批准号：
ST/T000325/1
负责人：
Laura Nuttall
金额：
$ 24.65万
依托单位：
University of Portsmouth
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2020
资助国家：
英国
起止时间：
2020 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=ST%2FT000325%2F1
关键词：
Pinpointing Origin Noisy Compact Binary

项目摘要

Gravitational waves are ripples in the fabric of spacetime, which carry information away from the source that created them, at the speed of light. Any non-spherically symmetric accelerated masses will produce gravitational waves, just at differing strengths. Compact object mergers, such as the collisions of neutron stars and black holes, are some of the strongest sources of detectable gravitational waves. Around 1.3 billion years ago, two black holes roughly 30 and 35 times the mass of the Sun collided with one another, and sent gravitational waves rippling throughout our Universe. In 2015, these gravitational waves swept through the Earth, and were detected by the LIGO interferometers. Since this groundbreaking initial discovery, nine more signals from the merger of black holes have been observed with the LIGO and the Virgo detectors. We estimate the masses of the black holes which collided to create these ten signals to be between 5 and 67 times the mass of the Sun. The black hole mass distribution is not thought to be continuous however. Simulations of metal-poor massive stars, around 130-250 the mass of the Sun, predict they end their lives in a pair instability supernova. In these stars, electron and positron pairs are created in the core, which cause the star to become unstable and collapse. In these supernovae no remnant is created. This means there should be a gap in the black hole mass distribution; there should be no black holes with masses between 50 - 130 times the mass of the Sun. Gravitational waves provide a unique way of probing this gap. The aims of this proposal are twofold. Our first aim is to map out the gap in the black hole mass distribution using gravitational-wave observations. The techniques we need to develop to be capable of probing this mass gap will also lead us toward our second goal - facilitating future joint gravitational-wave and electromagnetic observations.The first and only gravitational-wave signal from a neutron star coalescence, was almost simultaneously detected with gamma rays. In subsequent hours and days, the counterpart was observed across the electromagnetic spectrum. With these spectacular observations, we have been able to determine the nature of short gamma ray bursts and understand where much of the heavy elements are made. This proposal will maximise the chances of making further multi-messenger observations, which will be vital for probing many areas of physics, including estimating the expansion of the Universe.Although these two goals are very distinct, the techniques we need to develop to achieve these objectives are very similar. Both aims rely on investigating and improving the output of gravitational-wave detectors. This proposal will therefore develop novel methods of overcoming and understanding the variation of gravitational-wave detector noise. In addition to achieving the goals of this proposal, this research will have far reaching consequences in other areas of gravitational-wave astronomy. For example, our work will allow for more rigorous tests of General Relativity to be performed and ensure confident detections of gravitational-wave signals that are different to those that have currently been observed.

引力波是时空结构中的涟漪，它以光速将信息从产生它们的源头带走。任何非球对称的加速质量都会产生引力波，只是强度不同。紧凑的物体合并，如中子星和黑洞的碰撞，是可探测到的引力波的最强来源之一。大约13亿年前，两个质量分别是太阳30倍和35倍的黑洞相互碰撞，并在我们的宇宙中发出引力波。2015年，这些引力波扫过地球，并被LIGO干涉仪探测到。自从这一突破性的初步发现以来，LIGO和Virgo探测器又观测到了9个黑洞合并的信号。我们估计碰撞产生这十个信号的黑洞的质量是太阳质量的5到67倍。然而，黑洞的质量分布并不被认为是连续的。对质量约为太阳130-250倍的贫金属大质量恒星的模拟预测，它们会以一对不稳定超新星的形式结束生命。在这些恒星中，电子和正电子对在核心中产生，这导致星星变得不稳定并崩溃。在这些超新星中没有残余物产生。这意味着黑洞质量分布中应该有一个缺口;不应该有质量在50 - 130倍太阳质量之间的黑洞。引力波提供了一种独特的方式来探测这个差距。这项建议有两个目的。我们的第一个目标是利用引力波观测绘制出黑洞质量分布中的差距。我们需要开发的探测质量间隙的技术也将引导我们实现第二个目标--促进未来的引力波和电磁波联合观测。第一个也是唯一一个来自中子星星合并的引力波信号几乎是与伽马射线同时探测到的。在随后的几个小时和几天里，在整个电磁频谱中观察到了对应物。通过这些壮观的观测，我们已经能够确定短伽马射线爆发的性质，并了解大部分重元素的来源。这一提议将最大限度地提高进一步进行多信使观测的机会，这对于探索许多物理学领域至关重要，包括估计宇宙的膨胀。尽管这两个目标非常不同，但我们需要开发的技术非常相似。这两个目标都依赖于研究和改进引力波探测器的输出。因此，这一提议将开发克服和理解引力波探测器噪声变化的新方法。除了实现这一提议的目标外，这项研究还将在引力波天文学的其他领域产生深远的影响。例如，我们的工作将允许对广义相对论进行更严格的测试，并确保对与目前观察到的引力波信号不同的引力波信号进行可靠的检测。

项目成果

期刊论文数量（10）

专著数量（0）

科研奖励数量（0）

会议论文数量（0）

专利数量（0）

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3a

搜索与费米和斯威夫特在 LIGO–Virgo Run O3a 期间检测到的伽马射线爆发相关的引力波

DOI：
10.3847/1538-4357/abee15
发表时间：
2021
期刊：
The Astrophysical Journal
影响因子：
0
作者：
Abbott, R.;Abbott, T. D.;Abraham, S.;Acernese, F.;Ackley, K.;Adams, C.;Adhikari, R. X.;Adya, V. B.;Affeldt, C.;Agathos, M.
通讯作者：
Agathos, M.

Impact of noise transients on low latency gravitational-wave event localization

DOI：
10.1103/physrevd.105.103021
发表时间：
2022-02
期刊：
Physical Review D
影响因子：
5
作者：
R. Macas;Joshua Pooley;L. Nuttall;D. Davis;M. Dyer;Y. Lecoeuche;J. Lyman;J. McIver;K. Rink-K.-Rin
通讯作者：
R. Macas;Joshua Pooley;L. Nuttall;D. Davis;M. Dyer;Y. Lecoeuche;J. Lyman;J. McIver;K. Rink-K.-Rin

GLADE+ : an extended galaxy catalogue for multimessenger searches with advanced gravitational-wave detectors

GLADE：使用先进引力波探测器进行多信使搜索的扩展星系目录