Thermal charge carrier driven noise in transmissive semiconductor optics

Bruns, Florian; Vyatchanin, S. P.; Dickmann, Johannes; Glaser, Rene; Heinert, D.; Nawrodt, R.; Kroker, Stefanie

doi:10.1103/physrevd.102.022006

Cited by 10 publications

(3 citation statements)

References 31 publications

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“…The magnitude of this effect is described by a carrier dispersion coefficient γ c = dn/dn c (different for electrons and holes). The carrier density noise was estimated as [31]:…”

Section: Phase Noisementioning

confidence: 99%

A cryogenic silicon interferometer for gravitational-wave detection

Adhikari¹,

Aguiar²,

Arai³

et al. 2020

Class. Quantum Grav.

184

110

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The detection of gravitational waves from compact binary mergers by LIGO has opened the era of gravitational wave astronomy, revealing a previously hidden side of the cosmos. To maximize the reach of the existing LIGO observatory facilities, we have designed a new instrument able to detect gravitational waves at distances 5 times further away than possible with Advanced LIGO, or at greater than 100 times the event rate. Observations with this new instrument will make possible dramatic steps toward understanding the physics of the nearby universe, as well as observing the universe out to cosmological distances by the detection of binary black hole coalescences. This article presents the instrument design and a quantitative analysis of the anticipated noise floor. • Quantum noise will be reduced by increasing the optical power stored in the arms. In Advanced LIGO, the stored power is limited by thermally induced wavefront distortion effects in the fused silica test masses. These effects will be alleviated by choosing a test mass material with a high thermal conductivity, such as silicon. • The test mass temperature will be lowered to 123 K, to mitigate thermo-elastic noise. This species of thermal noise is especially problematic in test masses ‡ 1/e 2 intensity § Round-trip loss; see section 5.2 (DRFPMI) with frequency dependent squeezed light injection. The beam from a 2µm prestabilized laser (PSL), passes through an input mode cleaner (IMC) and is injected into the DRFPMI via the power-recycling mirror (PRM). Signal bandwidth is shaped via the signal recycling mirror (SRM). A squeezed vacuum source (SQZ) injects this vacuum into the DRFPMI via an output Faraday isolator (OFI) after it is reflected off a filter-cavity to provide frequency dependent squeezing. A Faraday isolator (FCFI) facilitates this coupling to the filter cavity. The output from the DRFPMI is incident on a balanced homodyne detector, which employs two output mode cleaner cavities (OMC1 and OMC2) and the local oscillator light picked off from the DRFPMI. Cold shields surround the input and end test masses in both the X and Y arms (ITMX, ITMY, ETMX and ETMY) to maintain a temperature of 123 K in these optics. The high-reflectivity coatings of the test masses are made from amorphous silicon. detected (with SNR = 8) as a function of the total mass of the binary (in the source frame). (B) Donut visualization of the horizon distance of LIGO Voyager, aLIGO, and A+, shown with a population of binary neutron star mergers (yellow) and 30-30 M binary black hole mergers (gray). This assumes a Madau-Dickinson star formation rate [7] and a typical merger time of 100 Myr.

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“…The magnitude of this effect is described by a carrier dispersion coefficient γ c = dn/dn c (different for electrons and holes). The carrier density noise was estimated as [31]:…”

Section: Phase Noisementioning

confidence: 99%

A cryogenic silicon interferometer for gravitational-wave detection

Adhikari¹,

Aguiar²,

Arai³

et al. 2020

Class. Quantum Grav.

184

110

View full text Add to dashboard Cite

show abstract

“…Additionally, the semiconductor nature of silicon gives rise to refractive index fluctuations due to the motion of free carriers in the silicon test masses. Initial estimates of this noise source [90] suggested that the phase noise induced by these fluctuations could be significant, but a more recent analysis that includes Debye screening indicates that this noise will lie several orders of magnitude below the total thermal noise of the substrate [91]. We therefore do not consider this noise source.…”

Section: Substratesmentioning

confidence: 99%

Gravitational-wave physics with Cosmic Explorer: Limits to low-frequency sensitivity

et al. 2021

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Cosmic Explorer is a next-generation ground-based gravitational-wave observatory concept, envisioned to begin operation in the 2030s and expected to be capable of observing binary neutron star and black hole mergers back to the time of the first stars. Cosmic Explorer's sensitive band will extend below 10 Hz, where the design is predominantly limited by geophysical, thermal, and quantum noises. In this work, thermal, seismic, gravity-gradient, quantum, residual gas, scattered-light, and servo-control noises are analyzed in order to motivate facility and vacuum system design requirements, potential test mass suspensions, Newtonian noise reduction strategies, improved inertial sensors, and cryogenic control requirements. Our analysis shows that, with improved technologies, Cosmic Explorer can deliver a strain sensitivity better than 10 −23 Hz −1=2 down to 5 Hz. Our work refines and extends previous analysis of the Cosmic Explorer concept and outlines the key research areas needed to make this observatory a reality.

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“…This noise is called thermoelastic noise [22]. A second noise source is called charge carrier driven noise [23]. Here, the charge carrier distribution fluctuates and so the refractive index.…”

Section: Introductionmentioning

confidence: 99%

Thermally induced refractive index fluctuations in transmissive optical components and their influence on the sensitivity of Einstein telescope

Meyer

Dickmann

Kroker

et al. 2022

Class. Quantum Grav.

Self Cite

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With a relative length measurement precision of better than 10−23, gravitational wave interferometers are the most precise instruments that have ever been built. With this enormous sensitivity many noise sources potentially effect gravitational wave detector sensitivity, each of which must be investigated to ensure confidence in design sensitivity. We present calculations of photoelastic noise as well as thermo refractive noise in the beam splitter (BS) and the input test masses (ITM) in Einstein Telescope (ET). It turns out that the amplitude of the photoelastic noise in the ET low-frequency detector is about five orders of magnitude below the maximum design sensitivity and five orders of magnitude below that of the ET high-frequency detector, whereas thermo refractive noise impairs the design sensitivity by approximately 20%.

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Thermal charge carrier driven noise in transmissive semiconductor optics

Cited by 10 publications

References 31 publications

A cryogenic silicon interferometer for gravitational-wave detection

A cryogenic silicon interferometer for gravitational-wave detection

Gravitational-wave physics with Cosmic Explorer: Limits to low-frequency sensitivity

Thermally induced refractive index fluctuations in transmissive optical components and their influence on the sensitivity of Einstein telescope

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