Performance test of pipe-shaped radiation shields for cryogenic interferometric gravitational wave detectors

Sakakibara, Yusuke; Kimura, N.; Akutsu, T.; Suzuki, Toshikazu; Kuroda, K.

doi:10.1088/0264-9381/32/15/155011

Cited by 19 publications

(11 citation statements)

References 21 publications

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“…Cold Shields To minimize the radiative heat load from the 300 K beam tube, the radiation shield will need to include a cylindrical piece which extends into the beam tube. The inside of the shield will require baffles, as in the KAGRA design, to reduce multiple reflection paths from the 300 K environment [132]. The inside of the long shield should be coated with a high emissivity black coating to maximize the radiative coupling to the test mass.…”

Section: A2 Radiative Cooling Of the Test Massmentioning

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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Section: A2 Radiative Cooling Of the Test Massmentioning

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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“…Moreover, in order to accelerate the cooling time, it is planned to coat all the payload (with the exception of the mirror, of course) with diamond like carbon (DLC). According to the simulations this solution allows increasing the radiation cooling efficiency and thus reducing the total cooling time from nearly two months to 39 d. Experimental tests done with a half size prototype of the payload coated with DLC confirmed the validity of the simulation [129].…”

Section: The Kagra Solutionsmentioning

confidence: 59%

“…This design should allow to extract the amount of power deposited by the laser in the mirrors and cool down the mirror to 20 K provided a sufficiently heat conduction path is made between the mirror and the cryo-coolers. In addition two 5 m long cryogenic ducts allow the laser beam to enter the cryostat and while reducing the 300 K radiation input to the mirror by a factor of a thousand compared to the input one would have from the tube in the absence of the ducts [129].…”

Section: The Kagra Solutionsmentioning

confidence: 99%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

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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,

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“…The cryostat for the test masses also have various kinds of baffles for absorbing stray light inside the cavity, and duct shields at both sides for absorbing the room temperature thermal radiation from vacuum ducts [23,24]. We use four low vibration double-stage pulse-tube cryocoolers for each cryostat [25,26].…”

Section: Interferometer Configuration Of Bkagramentioning

confidence: 99%

First cryogenic test operation of underground km-scale gravitational-wave observatory KAGRA

Akutsu¹,

Ando²,

Arai³

et al. 2019

Class. Quantum Grav.

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KAGRA is a second-generation interferometric gravitational-wave detector with 3 km arms constructed at Kamioka, Gifu, Japan. It is now in its final installation phase, which we call bKAGRA (baseline KAGRA), with scientific observations expected to begin in late 2019. One of the advantages of KAGRA is its underground location of at least 200 m below the ground surface, which reduces seismic motion at low frequencies and increases the stability of the detector. Another advantage is that it cools down the sapphire test mass mirrors to cryogenic temperatures to reduce thermal noise. In April-May 2018, we operated a 3 km Michelson interferometer with a cryogenic test mass for 10 d, which was the first time that km-scale interferometer was operated at cryogenic temperatures. In this article, we report the results of this 'bKAGRA Phase 1' operation. We have demonstrated the feasibility of 3 km interferometer alignment and control with cryogenic mirrors.

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Performance test of pipe-shaped radiation shields for cryogenic interferometric gravitational wave detectors

Cited by 19 publications

References 21 publications

A cryogenic silicon interferometer for gravitational-wave detection

A cryogenic silicon interferometer for gravitational-wave detection

Gravitational wave astronomy: the current status

First cryogenic test operation of underground km-scale gravitational-wave observatory KAGRA

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