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(wow) Words Of Wonders Level 2894 Answers
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Received: 10 January 2022 / Revised: 1 February 2022 / Accepted: 4 February 2022 / Published: 15 February 2022
Gravitational waves from merging binary black holes and neutron stars are always visible. As of 2021, 90 reliable observations of electromagnetic waves have been made by LIGO and Virgo detectors. Work continues on the fourth look to further increase the sensitivity of the detectors, including the introduction of another A + enhancement designed to reduce background noise that limits sensitivity to electromagnetic waves. In this tutorial, we will provide an overview of the optical configuration and capture key features of the LIGO detectors, discuss the basic and technical noise limits of the detector, present the current measurement sensitivities, and evaluate the A+ enhancements installed in the detectors. .
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On September 14, 2015, the Advanced LIGO detectors made the first direct detection of gravitational waves (GWs) from merging binary black holes [1]. Recently, the digitals became fully operational after a five-year hiatus, being upgraded from basic to advanced LIGO. The advanced LIGO detectors introduced new innovations and new processing techniques designed to improve the signal-to-noise ratio of GW signals in the field of atmospheric listening [2, 3, 4]. Modern telescopes have greatly improved the sensitivity of GW signals from the merging of the intermediate-mass black hole, making it possible to detect GW150914 [5].
On August 17, 2017, the Advanced LIGO and Virgo detect gravitational waves from the merger of binary neutron stars and gamma rays [6]. That event caused the telescope to be pointed in the direction of convergence to detect electromagnetic radiation within the entire electromagnetic spectrum [7].
Today, the detectors have advanced significantly for the purpose of creating sensitivity [8]. During the third observation (O3), 90 reliable gravitational wave observations of astrophysical compact binary mergers were reported, as well as many low resolution ones found [9].
Now, between the third and fourth phases of observation, a major improvement in properties known as A+ enhancement is being implemented in LIGO detectors [10, 11]. These improvements focus on lowering the fundamental noise limit of the Advanced LIGO detectors, enabling a higher level of sensitivity to electromagnetic waves.
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Here we will review the design and performance of the advanced LIGO digital detectors that lead to the observation of the fourth run (O4), scheduled to start in December 2022. The second part will briefly discuss the gravitational waves we expect. The third section discusses the Advanced LIGO setup and the closing procedure for the acquisition. The fourth section examines the critical sensitivity limits of the advanced LIGO detectors, as well as the currently implemented sensitivities. Section 5 will discuss current detector work, introducing the topics of point absorbers in optics and compressed light fields. Part 6 will discuss the solutions currently being used in the preparation of O4. Section 7 will discuss future ways to increase detector sensitivity. Appendices Appendices A and B will discuss the basics of the Michelson and Fabry-Pérot interferometric systems, the basic building blocks of a complete Advanced LIGO interferometer.
And k is the frequency and wavenumber of the GW. In formula (2) we defined a standard coordinate system
Greek indices from 0 to 3. With this choice of gauge, the trace of the matrix in equation (2) is zero, and the spatial stress is only in the x and y direction, shifting to the z propagation direction.
Equation (10) is the common strain-length relationship used for GW detection based on Michelson interferometers with two rectangular optical cavities filled with laser light. This prompts the choice for very long interferometer arms; In general, the length of the arms, the more variable the length of change.
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You are right. otherwise, equation (10) breaks down because GW travels in space faster than light can travel through optical channels [16].
Each upper LIGO detector is a long baseline laser interferometer with two 4 km long rectangular arms. The interferometer acts as a converter, converting the GW signal into visible laser power oscillations in the asymmetric port.
The interferometer is equipped with several auxiliary subsystems needed to detect gravitational waves. Auxiliary subsystems include core optical height controllers [17, 18, 19, 20, 21, 22, 23], angle controllers [24, 25, 26, 27, 28, 29, 30, 31], high power stable laser [32, 33, 34], vacuum system [35, 36, 37], optical suspensions [38, 39, 40], seismic isolation [41, 42, 43, 44] and electrical and data acquisition systems [45, 46, 47, 48 ]. This review will focus on the optical configuration and operation of interferometers.
The core of the advanced LIGO detectors are double repeaters, Fabry-Pérot, Michelson interferometers [2, 3], modified with an input and output mode sweeper [49, 50] and complete with pre-stabilized laser light [32]. The entire LIGO optomechanical control system is based on the Pound-Drever-Hall frequency stabilization technique [17].
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Figure 1 shows a simplified optical configuration of O4. The optical configuration is similar to O3 except for the addition of a 300 μm filter cavity [51, 52, 53].
In this section, we will look at the Advanced LIGO setup and the lock-in acquisition process. Appendix A provides an overview of the optical components that make up the advanced LIGO architecture.
The main interferometer consists of seven core optics, shown in Figure 1; power processing mirror, signal processing mirror, beam splitter, and four manual cavity optics known as input test arrays (ITMs) and end test arrays (ETMs).
The main interferometer relies on constructive interference to generate high laser power levels in 4-km-long Fabry-Perot arm cavities (see Appendix B). With more laser power built into the interferometer, more light is modulated to pass through the GW, creating a stronger response observed for the GWs in the detection channel.
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In a Michelson interferometer consisting of two arms and a beam splitter, a destructive error occurs at the asymmetric (detection) station when the beams from the two arms rejoin out of phase so that no light is detected. Constructive interference occurs at the input channel so that all incoming light is reflected back to the laser in the Michelson interferometer (see Appendix A).
A change in a different part of the light in each arm, such as that caused by gravitational waves, will cause the light to exit the Michelson viewing port. On the other hand, often phase changes will have no effect on the light levels at the input or output channel. However, the Michelson detection channel has a high common-mode rejection because both the frequency and intensity variations of the input laser light are rejected by the detection channel.
The signal-to-noise ratio (SNR) of the gravitational wave in the asymmetric port is composed of the laser power signal due to GWs.
Is the laser wavelength and h is the amplitude of the GW voltage. The full solution of the detector is derived in [54, 55] and extended in [23, 56, 57, 58]. A complete review of the detector signal and noise processing can be found in [59, 60].
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Several important assumptions in design design are given in Equation (11). First, the easiest way to enlarge the signal is to increase the length of L. The main consequence of adding more detectors is the installation cost, especially the removed radio tube, which currently limits the LIGO detectors to a distance of 4 km. To increase the wing power
Increases the visible laser signal produced by GWs and is limited by the input power and absorption and propagation losses of the interferometer. By reducing the wavelength of the detector
It would inadvertently increase the sensitivity to GWs, but would require all key detector systems such as source lasers, optical coatings, substrates, and photodetectors to operate.
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