The Local oscillator in gravitational wave detectors
Future Networks of Gravitational Wave Detectors: Quantum Noise and Space Detectors
... interferometric gravitational wave detectors, we measure the light coming out of the interferometer to see if there is a signal present or not, but there is nothing special to the light exiting an ...
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Squeezed light sources for current and future interferometric gravitational-wave detectors
... Due to its wide transparency range (400 nm – 4 µ m), [56] periodically-poled KTP was used as the nonlinear crystal for the 2 µm squeezer, in both the SHG and OPO. At 1984 nm the refractive index of KTP is lower than that ...
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Noise Cancellation for Gravitational Wave Detectors
... only be determined by a full array measurement. So far, this has only been done at the Y-end station at the LIGO Hanford site (see Section 6.4 for details). A single seismometer measurement cannot determine the ...
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Quantum limited measurements in gravitational wave detectors
... For Gravitational Wave Detection This chapter outlines a proposal for a modified speed-meter interferometer that beats the standard quantum limit over a broad frequency ...
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Mitigating Noise in Interferometric Gravitational Wave Detectors
... 7.3 Evading quantum radiation pressure noise To solve the aforementioned issue, we make use of the fact that the output field emerging from the cavity contains information about the quantum radiation pressure noise that ...
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Improving the Performance and Sensitivity of Gravitational Wave Detectors
... the gravitational wave observatory Advanced LIGO, this system will study the behavior of metals in the elastic regime, far from the yield stress that would introduce plastic ...
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Arm length stabilisation for advanced gravitational wave detectors
... order of 1nagnitude in the LIGO detection band.. In this final section of the chapter , a brief description of Initial LIGO is given , followed by a description of some [r] ...
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Homodyne detection for laser-interferometric gravitational wave detectors
... Figure 1.2: Depiction of the cryostat of the explorer bar detector, which has operated at cern since 1990. Explorer was oriented in parallel to the allegro detector at LSU[9] to enable searches for coincident detections. ...
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Thermal noise in BEC-phononic gravitational wave detectors
... Figure 2 Time evolution of the optimal bound for the strain sensitivity as provided by the QFI for n = 1, m = 2, T = 0 (blue, solid), T = 150 nK (red, dashed), m = 6, T = 0 (black, solid), T = 150 nK (green, dotted) and ...
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Quantum correlation measurements in interferometric gravitational wave detectors
... interferometric gravitational wave detectors, such as the Advanced Laser Interferometer Gravitational wave Observatory (LIGO), is limited by quantum shot noise, quantum radiation ...
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Mirror thermal noise in interferometric gravitational wave detectors
... for gravitational radiation? Often hailed as a “new window on the universe,” gravitational waves promise to tell us about massive compact objects in the universe that we might not find by conven- tional ...
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Exploring the sensitivity of next generation gravitational wave detectors
... There are several areas of R&D which will determine the quantum noise in future detectors. First among these is work into increasing the measured squeezing levels [45– 54]. Second is prototyping of the ...
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Calibration of the LIGO gravitational wave detectors in the fifth science run
... coil actuators, forcing the Michelson into the linear regime where Eq. A.3 is valid. The actuation function of the suspended input test masses can be ap- proximated by the center-of-mass force-to-displacement transfer ...
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Sensitivity of the advanced LIGO detectors at the beginning of gravitational wave astronomy
... Because O1 was the first observing run, and work remains to be done on the detectors to bring them to their design sensitivity, not all of the interferometer parameters were at their design values during O1. Most ...
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A 'Violin-Mode' shadow sensor for interferometric gravitational wave detectors
... by a system of sensors and actuators, intended to compensate for drifts in, and excitations of, the suspension [6]. The lateral eigenmodes, or ‘Violin-Modes,’ of the vertically orientated silica suspension fibres are ...
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Enhancing the sensitivity of future laser-interferometric gravitational wave detectors
... 4.1.2 Sensitivity of a speed meter Since the early 1990s it has been known that the measurement of momentum, known to be a quantum non-demolition (QND) observable, offers the ability to surpass the SQL in interferometric ...
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Exploring the sensitivity of gravitational wave detectors to neutron star physics
... GW detectors operating at high optical ...thermal wave- front distortion in the input test masses and the beam ...future detectors, such as Cosmic Explorer and Einstein ...
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Classification methods for noise transients in advanced gravitational-wave detectors
... the detectors ( 10 Hz ) will be limited by the effects of seismic ...the detectors ’ duty ...advanced detectors will be for the most part newly designed instruments, never assembled or tested ...
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Correlated noise in networks of gravitational-wave detectors: Subtraction and mitigation
... FIG. 1: Correlated noise budget for a stochastic background search with the LIGO Hanford and Livingston detectors. The noise budget is given in terms of normalized energy density; see Eq. 8. Red is the correlated ...
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Vibration isolation stacks for gravitational wave detectors - finite element analysis
... Here, u is the vertical offset between the center of mass of a plate and the base level of the rubber supports for the stage above, and z is the vertical offset between the pendulum s[r] ...
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