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A cryogenic payload for the 3rd generation of gravitational wave interferometers

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TLDR
In this article, a prototype of a last stage payload suspended within a dedicated cryostat with the same technique adopted for the VIRGO payload and making use of two thin wires in a cradle configuration to support a mirror made of silicon is presented.
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This article is published in Astroparticle Physics.The article was published on 2011-09-01 and is currently open access. It has received 4 citations till now. The article focuses on the topics: Payload & Gravitational-wave observatory.

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Citations
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Research Facilities for Europe’s Next Generation Gravitational-Wave Detector Einstein Telescope

TL;DR: The Amaldi Research Center (ARC) in Rome (Italy), ETpathfinder in Maastricht (The Netherlands), SarGrav in the Sos Enattos mines on Sardinia (Italy) and E-TEST in Liége (Belgium) and its surroundings as mentioned in this paper .
Journal ArticleDOI

Calculation of thermal radiation input via funneling through a duct shield with baffles for KAGRA

TL;DR: In this paper, a duct shield with baffles was installed to reduce the thermal radiation caused by the presence of the hole, and the authors applied a ray trace model to calculate the heat input through the duct shield.
Dissertation

Computational Modelling of Amorphous mirror coatings for use in Advanced Gravitational wave detectors

TL;DR: In this article, the effect of TiO2 doping and heat treatment of Ta2O5 has been investigated and it has been shown that a TiO 2 doping of Ta 2O5 reduces the mechanical loss and that, that reduction is at a maximum at 30%TiO2.

Cryogenic payloads for the Einstein Telescope - Baseline design with heat extraction, suspension thermal noise modelling and sensitivity analyses

TL;DR: In this paper , a new baseline design for the cryogenic payload that is thermally and mechanically consistent and compatible with the design sensitivity curve of the Einstein Telescope (ET) is presented.
References
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Journal ArticleDOI

The status of LCGT

TL;DR: The current status of LCGT is described in this article, where two independent sets of interferometers are installed in a common vacuum system to assure the reliable detection, and the physical target is to detect every year at least one event of gravitational wave signal produced at the coalescence of a binary neutron star.
Journal ArticleDOI

Suspension last stages for the mirrors of the Virgo interferometric gravitational wave antenna

TL;DR: In this paper, the last stage suspension for the mirrors of the Virgo gravitational wave detector is described, in particular its key mechanical elements: the marionette and the reaction mass.
Journal ArticleDOI

Aspects of the suspension system for GEO 600

TL;DR: In this article, a double pendulum is used for the final stage of a triple pendulum from an isolation stack consisting of layers of stainless steel masses and graphite loaded silicone rubber.
Journal ArticleDOI

Acoustic quality factor of copper, brass and beryllium copper from 50 mK to 300 K

TL;DR: In this article, the amplitude-independent background mechanical quality factors (reciprocal internal frictions) of oxygen-free electronic (OFE) copper (C 10100), free-turning brass (C36000) and beryllium copper (17200) were measured in the temperature range 50 mk -300 K.
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Frequently Asked Questions (17)
Q1. What have the authors contributed in "A cryogenic payload for the 3rd generation of gravitational wave interferometers" ?

The cooling strategy, the thermal behaviour and the system mechanical response have been deeply studied while a measurement characterization campaign has been performed both at room temperature and at cryogenic temperature. In this paper, the preliminary results obtained together with the first cooling down of the 300 kg overal mass payload at about 25 K, are reported. This study will play a driving role in the design of the third generation Gravitational Wave detector. 

The first prototype has been built with the aim to study the mechanical, cooling and control strategy for the optimization of this crucial element of a typical seismic isolation chain included in the ground based interferometric detector. These promising results represent the starting point for the development of next generation payload that will be integrated in a more complex detector working at cryogenic temperature and avoiding potential problem coming from the pulse tube cryocooler. 

The reflected cone is differentially subtended as a function of the object distance and, as a consequence, monitoring the power variation detected by the photo sensor a very precise displacement measurement can be performed. 

Moreover the importance of a good thermal link between the payload and the cooling system has a fundamental role in the design optimization, taking care of having links as short as possible and good thermal couplings, so to avoid refrigeration power losses. 

The goal of their design was the optimization of the payload geometry and the construction materials choice having a mirror with a final temperature around 10 K, a temperature value for which the thermal conductivity of copper wires is close to its maximum. 

The use of cryogenic techniques in the development of future GW detectors is also connected to the reduction of the thermal lensing due to the temperature gradients within the mirror substrate and coating. 

Since the interconnection elements made of wires and rods of different material, play a crucial role in determining the thermal behavior of the system, their design has been developed with the help of a thermal model described in the next section. 

The behavior of a 350 mm diameter mirror hung to a marionette by means of two thin copper wires (1 mm diameter) has been studied starting from a stationary state at 4K up to a new thermodynamic equilibrium reached after the switching on of the laser light. 

Mode Simulation [Hz] Frequency at 30 K [Hz] z1 0.48 0.49 z2 0.65 0.62 z3 0.71 0.75 z4 1.01 0.96 x1 0.47 0.50 x2 0.68 0.63 ∗x3 0.74 – x4 1.0 1.1 θx2 0.89 0.98 θx3 2.27 2.3 θx4 4.0 4.0 θy3 1.02 1.21 θy4 1.46 1.47 θz1 0.59 0.58 θz2 2.14 2.6 ∗Table 2: Mode assignment of the mechanical resonance frequencies measured at low temperature compared with the ANSYS simulation results. 

At the beginning of the run the Pulse Tube cryo-coolers were stopped many times, because of failure in the water refrigeration system of their compressors. 

This contribution depends on the materials elastic expansion coefficient and it is proportional to the second power of temperature. 

In order to fulfill the requirement on the resonance frequencies of each payload element, the authors have studied the mechanical behavior of the mirror reaction mass, the marionette and the new MRM element developing a finite element model for each of them based on the ANSYS software. 

The frequency response of the system at cryogenic temperature demonstrated the very low influence of the thermal links on the dynamic of the mechanical system. 

This is a direct consequence of the change in the elastic material properties at low temperature, a well known phenomena affecting in particular the Cu Be3 strips of the mirror suspension [14] . 

It is important to stress that this thermal response can be achieved when the liquid helium is in thermal contact with the marionette, while in their experimental set-up the payload is hosted in a large vacuum chamber (a large cryostat) kept at low temperature by means of a pulse tube cryo-cooler. 

This is partially due to the quasi-degeneracy of x and z mode frequencies and to the limited information provided by the two selective fiber bundle sensors 3. 

Substrate absorption rate 1 ppm/cm Coating absorption rate 1 ppmPower in the Fabry-Perot cavities 1 MW Light Power crossing the mirror bulk 9 kW Power absorbed by mirror substrate 100 mW Power absorbed by mirror coating 900 mWTable 1: Simulation hypothesisLooking at the plot reported in figure 6, it should be noted that the laser light does not change significantly the mirror temperature: in fact after a steep temperature increase of the mirror center a new steady state at ∼ 7.2 K is reached within ∼ 60 s.