Status of Japanese gravitational wave detectors

Arai, K.; Takahashi, Ryutaro; Tatsumi, Daisuke; Izumi, K.; Wakabayashi, Yaka; Ishizaki, Hideharu; Fukushima, Mitsuhiro; Yamazaki, Toshitaka; Fujimoto, Masa–Katsu; Takamori, A.; Tsubono, K.; DeSalvo, R.; Bertolini, A.; Márka, S.; Sannibale, V.; Uchiyama, Takashi; Miyakawa, O.; Miyoki, S.; Agatsuma, K.; Saito, Takeshi; Kuroda, K.; Nakatani, I.; Telada, S.; Yamamoto, K.; Tomaru, T.; Suzuki, Toshikazu; Haruyama, T.; Sato, Nobuaki; Yamamoto, A.; Shintomi, T.

doi:10.1088/0264-9381/26/20/204020

Cited by 24 publications

(21 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Thermal noise basing on the change of the refractive index on temperature -thermorefractive (TR) noise -is one key noise process in the design of interferometric gravitational wave detectors [1][2][3]. Wherever the laser beam passes matter, the temperature fluctuations within the substrate will cause a change of the refractive index and, consequently, will change the phase of the traveling beam.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Thermorefractive noise of finite-sized cylindrical test masses

et al. 2011

View full text Add to dashboard Cite

We present an analytical solution for the effect of thermorefractive noise considering finite-sized cylindrical test masses. For crystalline materials at low temperatures the effect of finite dimensions becomes important. The calculations are independently performed using the FluctuationDissipation-Theorem and Langevin's approach. Our results are applied to the input test mass of the current and future cryogenic gravitational wave detectors CLIO, LCGT, and ET and are compared to the respective standard quantum limit. For a substrate temperature of 10 K we find that the thermorefractive noise amplitude of the silicon input test mass in ET is only a factor of 2 below the standard quantum limit for frequencies above 500 Hz. Thus, thermorefractive noise of the input test mass could become a severe limitation if one uses techniques to beat the standard quantum limit like, e.g., squeezing. In contrast the effect of thermorefractive noise of the input test mass is negligible for CLIO and LCGT.

show abstract

mentioning

confidence: 99%

“…Our analysis reveals that the effect of the finite size is to be taken into account for cooled and crystalline substrates. Next to ET also CLIO and LCGT [2] exhibit crystalline substrates at low temperatures and are under investigation in this work.…”

mentioning

confidence: 99%

Thermorefractive noise of finite-sized cylindrical test masses

et al. 2011

View full text Add to dashboard Cite

show abstract

“…We used a suspended Fabry-Perot cavity with a length of 300 m and a finesse of 500. This cavity is a part of TAMA300 [6] and enclosed in high-vacuum chambers. The mirrors are suspended by wires, providing a resonant frequency of 1 Hz.…”

Section: Implementation Of the Proposed Scheme A Experimental Arrangmentioning

confidence: 99%

“…For instance, this maximum velocity is 2 μm/s for the Japanese prototype gravitational wave antenna, TAMA300 [6], with the ideal parameters: F 1.8 × 10 −3 N; λ 1064 nm; m 1 kg; and F 500. This is comparable to the rootmean-square (rms) of typical measured velocity.…”

Section: Introductionmentioning

confidence: 99%

Guided lock of a suspended optical cavity enhanced by a higher-order extrapolation

et al. 2017

View full text Add to dashboard Cite

Lock acquisition of a suspended optical cavity can be a highly stochastic process and is therefore nontrivial. Guided lock is a method to make lock acquisition less stochastic by decelerating the motion of the cavity length based on an extrapolation of the motion from an instantaneous velocity measurement. We propose an improved scheme that is less susceptible to seismic disturbances by incorporating the acceleration as a higher-order correction in the extrapolation. We implemented the new scheme in a 300-m suspended Fabry-Perot cavity and improved the success rate of lock acquisition by a factor of 30.

show abstract

“…2.1, we have used a laser interferometer to construct the example of how a GW interacts with matter. This choice is not arbitrary, it is made because interferometers of various design parameters are the most prevalent form of GW detectors [37][38][39][40][41]. We saw from the aforementioned example that GW detection is in essence a length measurement, and it has to be very accurate because the expected strain produced by detectable astronomical sources is of the order 10 −23 , or 0.01…”

Section: A Network Of Ground Based Detectorsmentioning

confidence: 99%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

View full text Add to dashboard Cite

In the centenary year of Einstein's General Theory of Relativity, this paper reviews the current status of gravitational wave astronomy across a spectrum which stretches from attohertz to kilohertz frequencies. Sect. 1 of this paper reviews the historical development of gravitational wave astronomy from Einstein's first prediction to our current understanding the spectrum. It is shown that detection of signals in the audio frequency spectrum can be expected very soon, and that a north-south pair of next generation detectors would provide large scientific benefits. Sect. 2 reviews the theory of gravitational waves and the principles of detection using laser interferometry. The state of the art Advanced LIGO detectors are then described. These detectors have a high chance of detecting the first events in the near future. Sect. 3 reviews the KAGRA detector currently under development in Japan, which will be the first laser interferometer detector to use cryogenic test masses. Sect. 4 of this paper reviews gravitational wave detection in the nanohertz frequency band using the technique of pulsar timing. Sect. 5 reviews the status of gravitational wave detection in the attohertz frequency band, detectable in the polarisation of the cosmic microwave background, and discusses the prospects for detection of primordial waves from the big bang. The techniques described in sects. 1-5 have already placed significant limits on the strength of gravitational wave sources. Sects. 6 and 7 review ambitious plans for future space based gravitational wave detectors in the millihertz frequency band. Sect. 6 presents a roadmap for development of space based gravitational wave detectors by China while sect. 7 discusses a key enabling technology for space interferometry known as time delay interferometry. gravitational waves, ground based detectors, pulsar timing, spaced based detectors, CMB PACS number(s): 04.80. Nn, 07.20.Mc,

show abstract

Status of Japanese gravitational wave detectors

Cited by 24 publications

References 38 publications

Thermorefractive noise of finite-sized cylindrical test masses

Thermorefractive noise of finite-sized cylindrical test masses

Guided lock of a suspended optical cavity enhanced by a higher-order extrapolation

Gravitational wave astronomy: the current status

Contact Info

Product

Resources

About