On the Dilution Refrigerator Thermal Connection for the SCHENBERG Gravitational Wave Detector

Bortoli, Fábio da Silva; Frajuca, Carlos; Magalhães, Nadja S.; Souza, S T de; Silva, Wilson Carlos da

doi:10.1007/s13538-020-00778-3

Cited by 21 publications

(10 citation statements)

References 24 publications

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“…The instrument will be maintained at low temperatures (∼ 4 K) by cryogenic chambers (dewars), cooled down by a He flow [9]. The antenna is coupled to parametric transducers that will monitor the vibrations of the quadrupolar/monopolar normal modes of the sphere [10][11][12][13][14]. One of the main advantages of a GW spherical resonant antenna is its omnidirectional sensitivity, which makes it equally responsive to all wave directions and polarizations [15].…”

Section: Introductionmentioning

confidence: 99%

The Design Strain Sensitivity of the Schenberg Spherical Resonant Antenna for Gravitational Waves

Liccardo

Lenzi

Marinho

et al. 2023

Preprint

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The main purpose of this study is to review the Schenberg resonant antenna transfer function and to recalculate the antenna design strain sensitivity for gravitational waves. We consider the spherical antenna with six transducers in the semi dodecahedral configuration. When coupled to the antenna, the transducer-sphere system will work as a mass-spring system with three masses. The first one is the antenna effective mass for each quadrupolemode, the second one is the mass of the mechanical structure of the transducer first mechanical mode and the third one is the effective mass of the transducer membrane that makes one of the transducer microwave cavity walls. All the calculations are done for the degenerate (all the sphere quadrupole mode frequencies equal) and non-degenerate sphere cases. We have come to the conclusion that the “ultimate” sensitivity of an advanced version of Schenberg antenna (aSchenberg) is around the standard quantum limit (although the parametric transducers used could, in principle, surpass this limit). However, this sensitivity, in the frequency range where Schenberg operates, has already been achieved by the two aLIGOs in the O3 run, therefore, the only reasonable justification for remounting the Schenberg antenna and trying to place it in the sensitivity of the standard quantum limit would be to detect gravitational waves with another physical principle, different from the one used by laser interferometers. This other physical principle would be the absorption of the gravitational wave energy by a resonant mass like Schenberg.

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Section: Introductionmentioning

confidence: 99%

The Design Strain Sensitivity of the Schenberg Spherical Resonant Antenna for Gravitational Waves

Liccardo

Lenzi

Marinho

et al. 2023

Preprint

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“…When the detector is in operation, the motion of the antenna's surface is monitored by six parametric microwave transducers with their distribution on the shape of half a dodecahedron circumscribed to the antenna sphere (Frajuca et al 2008). More details on the SCHENBERG detector and on spherical resonant‐mass GW detectors can be found in Aguiar et al 2002; Bortoli et al 2016; Bortoli et al 2019; Bortoli et al 2020; Bortoli et al 2010; Costa et al 2004; Frajuca et al 2018; Magalhaes et al 1995.…”

Section: Introductionmentioning

confidence: 99%

Coherent quantum states in resonant‐mass gravitational wave detectors

et al. 2023

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“…When operational, its surface was monitored by six microwave parametric transducers (Frajuca et al 2008) in a half dodecahedron distribution circumscribed to the sphere. Spherical resonant-mass GW detectors like this have been studied by the authors for quite some time now, particularly SCHENBERG (Bortoli et al 2016(Bortoli et al , 2019(Bortoli et al , 2020Costa et al 2004;Magalhaes et al 1995).…”

Section: Introductionmentioning

confidence: 99%

The challenge of calibrating a laser‐interferometric gravitational wave detector

et al. 2021

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In 2015, the first direct detection of gravitational waves was reported. Data analysis indicated that the waves had originated from the violent collision of two black holes, which scattered them through space-time as Einstein predicted. That detection was made possible by many advances in measurement technology, mainly vibration isolation of the detector optics, since, at 10 Hz, the motion of the laser-interferometric detector mirrors is at least one billion times smaller than the seismic motion of the ground. As well, it is difficult to lock the laser in the detection configuration in a large band of the spectrum; this was made possible by using many feedback and feed-forward control loops. However, in order to meet the many demanding requirements, more than a hundred of such active systems are included in a detector to allow locked acquisition and locked stability to, eventually, reach the desired sensitivity. In this work, challenges faced to reach some of these requirements will be described and we analyze how this scenario impacts the calibration of such detectors. In order to help reduce false alarm rates and provide data for veto systems, in this work we propose a specific kind of resonant-mass detector to operate in coincidence with laser-interferometric ones.

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On the Dilution Refrigerator Thermal Connection for the SCHENBERG Gravitational Wave Detector

Cited by 21 publications

References 24 publications

The Design Strain Sensitivity of the Schenberg Spherical Resonant Antenna for Gravitational Waves

The Design Strain Sensitivity of the Schenberg Spherical Resonant Antenna for Gravitational Waves

Coherent quantum states in resonant‐mass gravitational wave detectors

The challenge of calibrating a laser‐interferometric gravitational wave detector

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