Constraints on cosmic strings using data from the first Advanced LIGO observing run
Constraints on cosmic strings using data from the first Advanced LIGO observing run
复制标题
DOI：
10.1103/physrevd.97.102002
复制
发表时间：
2018-05-08
影响因子：
5
通讯作者：
Zweizig, J.
中科院分区：
文献类型：
--
作者：
Abbott, B. P.;Abbott, R.;Zweizig, J.
宇宙弦是宇宙早期在大统一理论尺度相变中形成的拓扑缺陷。它们也被预测在弦理论的背景下形成。南部-后藤宇宙弦网络失去能量的主要机制是通过产生环和随后的引力波发射，从而为宇宙弦的存在提供了实验签名。在这里，我们报告了在Advanced LIGO 2015-2016观测运行（O 1）的数据中专门搜索宇宙弦环引力波爆发的分析。在数据中没有发现这种信号的证据，因此我们为最近的三个环分布模型设定了宇宙弦参数的上限。在本文中，我们首先推导出弦张力G亩和相互交换概率的约束，不仅使用O 1数据集上进行的突发分析，但也从以前发表的LIGO随机O 1分析，脉冲星定时阵列，宇宙微波背景和大爆炸核合成实验的结果。我们表明，这些数据集是互补的，因为它们探测宇宙弦环在非常不同的时代产生的引力波。最后，我们表明，数据集排除了我们考虑的三个循环分布模型的参数空间的大部分。
Cosmic strings are topological defects which can be formed in grand unified theory scale phase transitions in the early universe. They are also predicted to form in the context of string theory. The main mechanism for a network of Nambu-Goto cosmic strings to lose energy is through the production of loops and the subsequent emission of gravitational waves, thus offering an experimental signature for the existence of cosmic strings. Here we report on the analysis conducted to specifically search for gravitational-wave bursts from cosmic string loops in the data of Advanced LIGO 2015-2016 observing run (O1). No evidence of such signals was found in the data, and as a result we set upper limits on the cosmic string parameters for three recent loop distribution models. In this paper, we initially derive constraints on the string tension G mu and the intercommutation probability, using not only the burst analysis performed on the O1 data set but also results from the previously published LIGO stochastic O1 analysis, pulsar timing arrays, cosmic microwave background and big-bang nucleosynthesis experiments. We show that these data sets are complementary in that they probe gravitational waves produced by cosmic string loops during very different epochs. Finally, we show that the data sets exclude large parts of the parameter space of the three loop distribution models we consider.