Investigation of magnetic noise in advanced Virgo

Cirone, A.; Fiori, I.; Paoletti, F.; Perez, M. M.; Rodríguez, A. R.; Swinkels, B. L.; Vazquez, A.; Gemme, G.; Chincarini, A.

doi:10.1088/1361-6382/ab4974

Cited by 20 publications

(28 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The low frequency part is dominated by the coupling of the ambient magnetic field to the small magnets that are attached to the back of each TM mirror and they are used to control the mirror position. The coupling to these magnets is known to decay as f 3 , where f is the frequency [36]. The measurements at NEB and WEB confirmed the expected behavior, while the magnetic coupling measured in CEB does not follow the same slope.…”

Section: Electromagnetic Noise Injectionsmentioning

confidence: 56%

“…An in-depth discussion on magnetic injections can be found in [36]. Here, we comment on the two most important features of the measured coupling function: the low frequency part (up to 100 Hz) with a declining slope and the high frequency part (above 100 Hz) with a rising slope.…”

Section: Electromagnetic Noise Injectionsmentioning

confidence: 88%

“…The last method we mention is noise injections. The noise injection technique is well known in the GW detector community [4,29,36,49]. The aim is to produce controlled and localized enhancements of the detector ambient noise in order to have a sizeable effect in the gravitational-wave signal allowing for the measurement of a noise coupling function.…”

Section: Experimental Methodsmentioning

confidence: 99%

“…In Advanced Virgo, we have significantly reduced the ambient magnetic field in proximity of the TM mirrors vacuum chambers [36]. The main actions consisted of: (i) rerouting electric cables at further distance from chambers; (ii) using mains cables with twisted hot and neutral wires in the chamber proximity; and, (iii) replacing several step-down power supplies with toroidal shaped core types for the reduction of stray magnetic field.…”

Section: Environmental Noise Couplings and Sourcesmentioning

confidence: 99%

See 3 more Smart Citations

The Hunt for Environmental Noise in Virgo during the Third Observing Run

et al. 2020

Self Cite

View full text Add to dashboard Cite

The first twenty years of operation of gravitational-wave interferometers have shown that these detectors are affected by physical disturbances from the surrounding environment. These are seismic, acoustic, or electromagnetic disturbances that are mainly produced by the experiment infrastructure itself. Ambient noise can limit the interferometer sensitivity or potentially generate transients of non-astrophysical origin. Between 1 April 2019 and 27 March 2020, the network of second generation interferometers—LIGO, Virgo and GEO—performed the third joined observing run, named O3, searching for gravitational signals from the deep universe. A thorough investigation has been done on each detector before and during data taking in order to optimize its sensitivity and duty cycle. In this paper, we first revisit typical sources of environmental noise and their coupling paths, and we then describe investigation methods and tools. Finally, we illustrate applications of these methods in the hunt for environmental noise at the Virgo interferometer during the O3 run and its preparation phase. In particular, we highlight investigation techniques that might be useful for the next observing runs and the future generation of terrestrial interferometers.

show abstract

Section: Electromagnetic Noise Injectionsmentioning

confidence: 56%

Section: Electromagnetic Noise Injectionsmentioning

confidence: 88%

Section: Experimental Methodsmentioning

confidence: 99%

Section: Environmental Noise Couplings and Sourcesmentioning

confidence: 99%

See 2 more Smart Citations

The Hunt for Environmental Noise in Virgo during the Third Observing Run

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

“…Current gravitational wave (GW) detectors are sensitive to signals in a frequency band that ranges between 10 Hz and 10 kHz. Their sensitivity can be affected by several dominant sources of noise, such as ground motion [1], local terrestrial gravity [2], magnetic noise [3], thermal [4] and quantum noise [5].…”

Section: Introductionmentioning

confidence: 99%

Seismic and Newtonian Noise in the GW Detectors

Trozzo

Badaracco

2022

Galaxies

View full text Add to dashboard Cite

Gravitational wave detectors aim to measure relative length variations of the order of ΔL/L≃10−21, or less. Thus, any mechanism that is able to reproduce such a tiny variation can, in principle, threaten the sensitivity of these instruments, representing a source of noise. There are many examples of such noise, and seismic and Newtonian noise are among these and will be the subject of this review. Seismic noise is generated by the incessant ground vibration that characterizes Earth. Newtonian noise is instead produced by the tiny fluctuations of the Earth’s gravitational field. These fluctuations are generated by variations of air and soil density near the detector test masses. Soil density variations are produced by the same seismic waves comprising seismic noise. Thus, it makes sense to address these two sources of noise in the same review. An overview of seismic and Newtonian noise is presented, together with a review of the strategies adopted to mitigate them.

show abstract