[PDF] Top 20 Improving the Performance and Sensitivity of Gravitational Wave Detectors

... As detailed here, the performance of the CESAR algorithm is perhaps too slow for con- venient usage. One approach to mitigating this factor would be to introduce a persistent memory store that keeps track of the ... See full document

... the detectors are most sensitive in a frequency range from about 800 Hz to 3 kHz, and this overlaps with only 1/5 of the bandwidth of our burst ...the performance of resonant bar detectors is ... See full document

... 2, improving the high fre- quency sensitivity of Advanced ...frequency sensitivity of Advanced ...high-frequency sensitivity will allow us to track the late inspiral and eventual merger of ... See full document

... advanced detectors places more stringent requirements on disturbances introduced by potential squeezing sub-systems than previous ...the sensitivity of interferometric wave detectors over ... See full document

... noise performance was found to be very close to the fundamental shot-noise limited performance of the detectors themselves, under all practical conditions of illumination, and over the desired VM ... See full document

... broadband sensitivity improve- ment once aLIGO is limited by radiation pressure noise ...(only improving high-frequency sensitivity, eventually at the expense of low-frequency sensitivity) ... See full document

... frequency sensitivity of gravitational wave detectors are important for increasing the observable population of astrophys- ical sources, such as intermediate mass compact black hole binary ... See full document

... all detectors, are used to increase the dynamic range of the coil actuators during initial control of the test ...the detectors approach designed sensitivity [2, ... See full document

... tion detectors. The approved second generation detectors seek higher sensitivity in the 100 Hz regime and ex- tension to lower frequencies as the most promising and feasible directions to ...based ... See full document

... of gravitational-wave bursts, since combining so many detectors naturally suppresses the background from accidental coincidences — to well below one per year, in our case — while maintaining high ... See full document

... its sensitivity in some frequency bands, and the relative event rates for different types of sources can aid the decision-making process for selecting the best detector ... See full document

... Many types of thermal noise can not be excited directly, and to measure these in low-noise ma- terials requires a low-noise instrument. Chapter 4 describes the construction and the commissioning of LIGO’s Thermal Noise ... See full document

... novel detectors are described below, has been retro-fitted to an aLIGO test-mass/mirror suspension ...displacement sensitivity of 100 pm (rms) / √Hz at 500 Hz, over a detection span of  ... See full document

... LIGO detectors is common, and enables early experience with new hardware configu- ...the gravitational wave ...measured gravitational wave ... See full document

... advanced detectors will be directly dependent on the dimensions of the fibers used to suspend the ...noise performance at low frequency in advanced interferometric gravitational wave ... See full document

... the sensitivity of the detector inside the linewidth of the signal recycling cavity, at the expense of deceased sensitivity outside the bandwidth of the ...to sensitivity and versatility comes at the ... See full document

... We parametrize an event by the coincidence variables δ t e , rA, and rf h given for each of the six possible pairs of detectors. These variables allow us to favor signals that are coherent in the network. We also ... See full document

... detect gravitational waves started in the 1960s when Joseph Weber con- structed resonant bars and attempted to read out the excitations of the bars by gravitational-wave bursts ...interferometer ... See full document

... the gravitational wave channel as displacement ...design sensitivity in the frequency band 10 – 500 Hz, but is below the current noise floor by a factor of ≥ ... See full document

... We also include the noise contributions of our seismometers in Figure 5.3 to demonstrate how close we are able to get to the fundamental limit of Wiener filtering. Since the Wiener filter accepts, as inputs, the signals ... See full document