Current long baseline gravitational wave detectors
Squeezed light sources for current and future interferometric gravitational-wave detectors
... 5.3.1 Bowtie cavity motivation and effect of backscattered light A squeezed light source for the purpose of gravitational-wave detection must produce squeezing in the audio frequency band. This presents a ...
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Noise Cancellation for Gravitational Wave Detectors
... We also discuss the suitability of our simulation as an estimate of Newtonian noise at the LIGO sites. The problem is set up as a full time-domain simulation of seismic fields and instrumental noise. Instrumental noise ...
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Quantum limited measurements in gravitational wave detectors
... 6.6.2 Improving the ovenβs thermal characteristics Initial tests of the oven in vacuum revealed that the heat conduction characteristics were unsatisfactory for the oven assembled with no heat conducting pastes. ...
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Improving the Performance and Sensitivity of Gravitational Wave Detectors
... A difference in the two resonant frequencies of about 5 mHz, obtained experimentally in the first prototype, and a difference in the two lengths of 0.5 mm, well within machin- ing tolerances, provide us with a common ...
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Future Networks of Gravitational Wave Detectors: Quantum Noise and Space Detectors
... a long and winding road through grad school, there are many people to ...on gravitational wave detection, and I appreciate his effort in making this ...
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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 ...
11
Mirror thermal noise in interferometric gravitational wave detectors
... for gravitational radiation? Often hailed as a βnew window on the universe,β gravitational waves promise to tell us about massive compact objects in the universe that we might not find by conven- tional ...
11
Exploring the sensitivity of next generation gravitational wave detectors
... GW detectors scale with detector length [16, 17], and is complementary to the detailed sensitivity analysis of the Einstein Telescope (ET, a proposed next generation European detector) presented in [18, ...km ...
11
Future Long Baseline Neutrino Facilities and Detectors
... charged current event rate superimposed on the π π β π π oscillation probability is shown in Figure ...charged current muon neutrino event rate per year in a 34 kt liquid argon (200 kt water Cherenkov) ...
35
Calibration of the LIGO gravitational wave detectors in the fifth science run
... the long-term characteristics of the instrument increased, a great deal of improvements were made to our measurement techniques compared with prior results ...future detectors will have more sophisticated ...
49
Enhancing the sensitivity of future laser-interferometric gravitational wave detectors
... In chapter 3 we discussed the thermal noise arising from dielectric mirrors used in all pre- vious and current gravitational wave detectors. This is a consequence of the presence of Brownian ...
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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 ...a long-term impact ...
17
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 ...
16
An investigation of eddy-current damping of multi-stage pendulum suspensions for use in interferometric gravitational wave detectors
... Eddy-current damping has been considered for use in other interferometric gravitational wave detectors. The VIRGO ( French-Italian ) group have previously investigated the possible adverse ...
7
Cross-correlation searches for persistent gravitational waves with Advanced LIGO and noise studies for current and future ground-based gravitational-wave detectors.
... two detectors, run the search, and look at how often their detection statistic takes on certain values by random ...two detectors, and so this method will give an independent estimate of how often, by ...
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Narrowing the Filter-Cavity Bandwidth in Gravitational-Wave Detectors via Optomechanical Interaction
... Therefore, the optical loss becomes the key limiting factor in the filer-cavity performance. Isogai et al. have exper- imentally demonstrated that the optical losses from current mirror technology are sufficiently ...
5
Design and experimental demonstration of a laser modulation system for future gravitational-wave detectors
... There is a technical challenge in the MZM system as a laser modulation system in GW detectors. Displacements of optics in the MZM system introduce a new noise couplings to the GW readout channel. This paper ...
21
Coatings and surface treatments for enhanced performance suspensions for future gravitational wave detectors
... This is required due to the coupling between the vertical and horizontal axes due to the curvature of the Earth. This can be achieved through use of high mechanical Q materials, which are compatible with cryogenic ...
24
Brownian Thermal Noise in Interferometric Gravitational Wave Detectors and Single Photon Optomechanics
... the baseline parameters of advanced LIGO, the highest contribution to coating Brownian noise arises from the coating-substrate bending noise caused by losses in tantala layers, because these layers are much more ...
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When light gets pushy: radiation pressure effects in interferometric gravitational wave detectors
... the current generation of detectors, would be based on dual-recycled Michelson interferometers with Fabry-Perot arm cavities, however the observatory would be formed from 3 identical, nested ...
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