Thermorefractive noise of finite-sized cylindrical test masses

Heinert, D.; Gurkovsky, A. G.; Nawrodt, R.; Vyatchanin, S. P.; Yamamoto, K.

doi:10.1103/physrevd.84.062001

Cited by 11 publications

(9 citation statements)

References 28 publications

(51 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The transition between the two regimes occurs at f ∼ 1.3 Hz for the OMC cavity. The same result has been obtained more recently for a finite cavity of cylindrical geometry [13], which restrains its validity to the range where r th is much larger than the wavelength and much smaller than the transverse size of the cavity (1 cm). This corresponds to a valid frequency range of 10 mHz-100 kHz, which covers well the frequency range of interest here.…”

Section: Advanced Virgo Output Mode Cleanersupporting

confidence: 79%

Upper-limit on the Advanced Virgo output mode cleaner cavity length noise

Bonnand

Ducrot

Gouaty

et al. 2017

Class. Quantum Grav.

View full text Add to dashboard Cite

Abstract. The Advanced Virgo detector uses two monolithic optical cavities at its output port to suppress higher order modes and radio frequency sidebands from the carrier light used for gravitational wave detection. These two cavities in series form the output mode cleaner. We present a measured upper limit on the length noise of these cavities that is consistent with the thermo-refractive noise prediction of 8 × 10 −16 m/Hz 1/2 at 15 Hz. The cavity length is controlled using Peltier cells and piezo-electric actuators to maintain resonance on the incoming light. A length lock precision of 3.5 × 10 −13 m is achieved. These two results are combined to demonstrate that the broadband length noise of the output mode cleaner in the 10-60 Hz band is at least a factor 10 below other expected noise sources in the Advanced Virgo detector design configuration.PACS numbers: 04.80. Nn, 95.55.Ym

show abstract

Section: Advanced Virgo Output Mode Cleanersupporting

confidence: 79%

Upper-limit on the Advanced Virgo output mode cleaner cavity length noise

Bonnand

Ducrot

Gouaty

et al. 2017

Class. Quantum Grav.

View full text Add to dashboard Cite

show abstract

“…A rough estimate of thermal noise from thermoelastic (Zener) damping was obtained by directly applying [14] the Fluctuation-Dissipation Theorem. We treat the crystal as an 0.8 mm radius cylinder, and follow the calculation done by Heinert et al [15]. This yields a spectral density of ∆k taking into account both thermorefractive and thermoelastic fluctuations.…”

Section: Noise Sourcesmentioning

confidence: 99%

A new bound on excess frequency noise in second harmonic generation in PPKTP at the 10^−19 level

Yeaton-Massey¹,

Adhikari²

2012

Opt. Express

View full text Add to dashboard Cite

Abstract:We report a bound on the relative frequency fluctuations in nonlinear second harmonic generation. A 1064 nm Nd:YAG laser is used to read out the phase of a Mach-Zehnder interferometer while PPKTP, a nonlinear crystal, is placed in each arm to generate second harmonic light. By comparing the arm length difference of the Mach Zehnder as read out by the fundamental 1064 nm light, and its second harmonic at 532 nm, we can bound the excess frequency noise introduced in the harmonic generation process. We report an amplitude spectral density of frequency noise with total RMS frequency deviation of 3 mHz and a minimum value of 20 µHz/Hz 1/2 over 250 seconds with a measurement bandwidth of 128 Hz, corresponding to an Allan deviation of 10 −19 at 20 seconds.

show abstract

“…beam splitters, cavity couplers, but also the first layers of highly reflective dielectric mirrors). The respective noise is called thermo-refractive (TR) noise and has been analyzed for the coatings [22], the beam splitter [23] and the cavity input test masses [24].…”

Section: Noise Due To Temperature Fluctuationsmentioning

confidence: 99%

Fluctuation Dissipation at work: Thermal noise in reflective optical coatings for GW detectors

Heinert

Hofmann

Nawrodt

2014

2014 IEEE Metrology for Aerospace (MetroAeroSpace)

View full text Add to dashboard Cite

In this paper we summarize the fundamentals of thermal noise in gravitational wave detectors as a metrological application. We repeat the evolution of noise calculation beginning at the classical process of Brownian motion via the FluctuationDissipation theorem (FDT) of Callen and Welton and arriving at the direct formulation of the FDT. Using this direct approach we present the effect of anisotropic substrates on the Brownian coating noise using a finite element analysis. Previous investigations identified Brownian coating noise to dominate the thermal noise spectrum of current and future detectors. We summarize and discuss different existing ideas to reduce this kind of noise allowing for an increased sensitivity of future detectors.

show abstract

Thermorefractive noise of finite-sized cylindrical test masses

Cited by 11 publications

References 28 publications

Upper-limit on the Advanced Virgo output mode cleaner cavity length noise

Upper-limit on the Advanced Virgo output mode cleaner cavity length noise

A new bound on excess frequency noise in second harmonic generation in PPKTP at the 10^−19 level

Fluctuation Dissipation at work: Thermal noise in reflective optical coatings for GW detectors

Contact Info

Product

Resources

About