We report the results of a recent search for the lowest value of thermal noise that can be achieved in LIGO by changing the shape of mirrors, while fixing the mirror radius and maintaining a low diffractional loss. The result of this minimization is a beam with thermal noise a factor of 2.32 (in power) lower than previously considered Mesa Beams and a factor of 5.45 (in power) lower than the Gaussian beams employed in the current baseline design. Mirrors that confine these beams have been found to be roughly conical in shape, with an average slope approximately equal to the mirror radius divided by arm length, and with mild corrections varying at the Fresnel scale. Such a mirror system, if built, would impact the sensitivity of LIGO, increasing the event rate of observing gravitational waves in the frequency range of maximum sensitivity roughly by a factor of three compared to an Advanced LIGO using Mesa beams (assuming all other noises remain unchanged). We discuss the resulting beam and mirror properties and study requirements on mirror tilt, displacement and figure error, in order for this beam to be used in LIGO detectors.
We want to explain non-observation of electromagnetic counterpart of currently confirmed ten gravitational wave signals from the black hole mergers assuming their existence in the hidden mirror universe. Mirror matter, which interacts with our world only through gravity, is a candidate of dark matter and its density can exceed ordinary matter density five times. Since mirror world is considered to be colder, star formation there started earlier and mirror black holes had more time to pick up the mass and to create more binary systems within the LIGO reachable zone. Totally we estimate a factor…
The implications of Mexican-hat mirrors: calculations of thermoelastic noise and interferometer sensitivity to perturbation for the Mexican-hat-mirror proposal for advanced LIGO
Analysis of LIGO data for gravitational waves from binary neutron stars
我们报告的搜索引力波从合并紧凑的双星系统在银河系和麦哲伦云。该分析使用了三个LIGO干涉仪中的两个在第一次LIGO科学运行期间获得的数据，并说明了使用干涉仪数据设置螺旋事件率上限的方法。分析管道的描述，特别注意两个干涉仪之间的数据选择和重合。我们建立了$\mathcal{R}<$ 1.7 \times 10^{2} $ per year per Milky Way Equivalent Galaxy (MWEG), with 90% confidence, on the coalescence rate of binary systems in which each component has a mass in the range 1--3 $ M_ \odot $的观测上限.
Thermoelastic-damping noise from sapphire mirrors in a fundamental-noise-limited interferometer
我们报告的第一个高精度干涉仪使用大蓝宝石镜，我们提出了第一个直接的，宽带测量的基本热噪声在这些镜子。我们的研究结果与Braginsky等人的热弹性阻尼噪声预测吻合得很好。A 264，1（1999）]和Cerdonio等人[Phys. Rev. D 63，082003（2001）]，它们已被用于预测先进干涉引力波探测器的天体物理范围。
Excess noise from scattered light poses a persistent challenge in the analysis of data from gravitational wave detectors such as LIGO. We integrate a physically motivated model for the behavior of these "glitches" into a standard Bayesian analysis pipeline used in gravitational wave science. This allows for the inference of the free parameters in this model, and subtraction of these models to produce glitch-free versions of the data. We show that this inference is an effective discriminator of the presence of the features of these glitches, even when those features may not be discernible in st…
Presented is the description of a new and general method used to search for $γ$-ray counterparts to gravitational-wave (GW) triggers. This method is specifically applied to single GW detector triggers. Advanced LIGO data from observing runs O1 and O2 were analyzed, thus each GW trigger comes from either the LIGO-Livingston or the LIGO-Hanford interferometer. For each GW trigger, Fermi Gamma-ray Burst Monitor data is searched and the most significant subthreshold signal counterpart is selected. Then, a methodology is defined in order to establish which of GW-$γ$-ray pairs are likely to have a c…
我们测量了在音频（5 Hz - 4 kHz）的单一交叉偏振干涉仪的光热效应。在法布里-珀罗干涉仪中，一个偏振方向的光被截断以周期性地加热干涉仪反射镜，而正交偏振方向的光测量反射镜长度的变化。抛光固体金属镜的测试显示出与Braginsky等人[“Thermodynamical fluctuations and photo-thermal散粒噪声in引力波antennas，”Physics Letters A 264，1-10（1999）]和Cerdonio等人[“Thermoelastic effects at low temperatures and quantum limits in displacement measurement，“Physical Review D 63 082003（2001）]描述了未涂覆的光学器件。
The response of the Advanced LIGO interferometers is known to vary with time [arXiv:1608.05134]. Accurate calibration of the interferometers must therefore track and compensate for temporal variations in calibration model parameters. These variations were tracked during the first three Advanced LIGO observing runs, and compensation for some of them has been implemented in the calibration procedure. During the second observing run, multiplicative corrections to the interferometer response were applied while producing calibrated strain data both in real-time and in high-latency. In a high-latenc…
We compare a conventional Mach-Zehnder light-pulse atom interferometer based on diffractive mirrors with one that uses specular reflection. In contrast to diffractive mirrors that generate a symmetric configuration, specular mirrors realized, for example, by evanescent fields lead under the influence of gravity to an asymmetric geometry. In such an arrangement the interferometer phase contains nonrelativistic signatures of proper time.
In this paper we consider the properties of the 10 confirmed by the LIGO Collaboration gravitational wave signals from the black hole mergers. We want to explain non-observation of electromagnetic counterpart and higher then expected merging rates of these events, assuming the existence of their sources in the hidden mirror universe. Mirror matter, which interacts with our world only through gravity, is a candidate of dark matter and its density can exceed ordinary matter density five times. Since mirror world is considered to be colder, star formation there started earlier and mirror black ho…
