Status report and near future prospects for the gravitational wave detector AURIGA

Zendri, J.-P.; Baggio, Lucio; Bignotto, M.; Bonaldi, M.; Cerdonio, M.; Conti, L.; Rosa, M. De; Falferi, P.; Fortini, P.; Inguscio, M.; Marin, A.; Marín, F.; Mezzena, R.; Ortolan, A.; Prodi, G. A.; Rocco, Emanuele; Salemi, F.; Soranzo, G.; Taffarello, L.; Vedovato, G.; Vinante, Andrea; Vitale, S.

doi:10.1088/0264-9381/19/7/394

Cited by 45 publications

(25 citation statements)

References 11 publications

(8 reference statements)

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“…On a much larger scale, mechanical resonators are fundamental to many gravitational wave detectors. Bar resonator detectors, from the original Weber bars [59] to the more-recent Nautilus [6] and AURIGA [67] projects, detect displacements of a 1000-kg-scale "antenna" for gravitational waves. Interferometric detectors like GEO [63], LIGO [2], and VIRGO [3] essentially measure the position of the 10-kg-scale mirrors at the ends of their interferometer arms.…”

Section: Introductionmentioning

confidence: 99%

Quantum squeezing of motion in a mechanical resonator

Wollman

Lei

Weinstein

et al. 2015

Science

631

566

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showed patience and understanding. He gave me the opportunity to work on a variety of interesting projects, from graphene, to superconducting amplifiers, to the results discussed here. Most of all, Keith taught me to be more decisive, to take more risks, and to do whatever it takes. Our theory collaborators on the squeezing project, Aashish Clerk, Florian Marquardt, and especially Andreas Kronwald, gave essential support before, during, and after measurement-taking.Although they sometimes seemed puzzled at the number of ways that things can go wrong in experimental work, they showed great patience as we tried to make their proposal a reality.I couldn't have made it through grad school without the support of my friends: Paul, Branimir, Helge, Alice, Tristan, Chris, Kris, Doron, Mo, and Carly. They gave me something to look forward to throughout the week, and something to talk about other than grad school. where an optical or microwave cavity is coupled to the mechanics in order to control and read out the mechanical state. In the proposal, two pump tones are applied to the cavity, each detuned from the cavity resonance by the mechanical frequency. The pump tones establish and couple the mechanics to a squeezed reservoir, producing arbitrarily-large, steady-state squeezing of the mechanical motion.In this dissertation, I describe two experiments related to the implementation of this proposal in an electromechanical system. I also expand on the theory presented in [30] to include the effects of squeezing in the presence of classical microwave noise, and without assumptions of perfect alignment of the pump frequencies.In the first experiment, we produce a squeezed thermal state using the method of Kronwald et. al..We perform back-action evading measurements of the mechanical squeezed state in order to probe the noise in both quadratures of the mechanics. Using this method, we detect single-quadrature fluctuations at the level of 1.09 ± 0.06 times the quantum zero-point motion.In the second experiment, we measure the spectral noise of the microwave cavity in the presence of the squeezing tones and fit a full model to the spectrum in order to deduce a quadrature variance of 0.80 ± 0.03 times the zero-point level. These measurements provide the first evidence of quantum squeezing of motion in a mechanical resonator.

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Section: Introductionmentioning

confidence: 99%

Quantum squeezing of motion in a mechanical resonator

Wollman

Lei

Weinstein

et al. 2015

Science

631

566

View full text Add to dashboard Cite

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“…He was joined in this by research groups at Stanford University [20,21], Louisiana State University (Allegro detector) [21,22], the University of Rome (Explorer and Nautilus detectors) [23,24], the University of Western Australia (Niobe) [25], and more recently a collaboration of the Universities of Trento and Padua (Auriga) [26]. Bars were of the order of a ton in weight and with the exception of the UWA bar were aluminium.…”

Section: Low Temperature Resonant Barsmentioning

confidence: 99%

“…The Auriga detector at Legnaro (Trento/Padua) is shown in figure 3(b). A number of experiments have been carried out over the last twenty-five years with these bar detectors, there being long periods where they were working together -sometimes in pairs, sometimes with more detectors -and many papers have been published, [21][22][23][24][25][26][27] for example. However despite occasional reports that some coincident events had been observed by a number of groups no definitive evidence for the existence of gravitational waves has yet been put forward.…”

Section: Low Temperature Resonant Barsmentioning

confidence: 99%

The search for gravitational waves

Rowan

Sathyaprakash

2005

J. Phys. B: At. Mol. Opt. Phys.

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Experiments aimed at searching for gravitational waves from astrophysical sources have been under development for the last 40 years, but only now are sensitivities reaching the level where there is a real possibility of detections being made within the next five years. In this article a history of detector development will be followed by a description of current detectors such as LIGO, VIRGO, GEO 600, TAMA 300, Nautilus and Auriga. Preliminary results from these detectors will be discussed and related to predicted detection rates for some types of sources. Experimental challenges for detector design are introduced and discussed in the context of detector developments for the future.2

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“…The gravitational wave detector AURIGA, which is operating at the National Laboratories of Legnaro (Italy), is essentially an aluminum cylinder equipped with a resonant capacitive transducer which is coupled to a high sensitivity dc-squid amplifier [4]. Due to the combination of the Earth's rotation and the antenna pattern, two times a day AU-RIGA is much more sensitive to the gw flux from the Galactic Center (see Figure 1).…”

Section: Description Of the Measurementmentioning

confidence: 99%

Gravitational Waves and GRBs from Tidal Disruption of Stars in the Center of Galaxies

Fortini

Ortolan

2004

AIP Conference Proceedings

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Abstract. Recent measurements by the Chandra satellite have shown that a supermassive black hole of M = 2.6 × 10 6 M ⊙ is located in the Galactic Center; it seems probable from other observations that this fact is common in the majority of galaxies. On the other hand, GRB explosions are typical phenomena linked to galactic dynamics. In the present paper we discuss the possibility that GRBs are tidal disruption of stars by supermassive black holes located in the center of galaxies. This conjecture can be tested by a gravitational wave detector of the class of AURIGA.

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Status report and near future prospects for the gravitational wave detector AURIGA

Cited by 45 publications

References 11 publications

Quantum squeezing of motion in a mechanical resonator

Quantum squeezing of motion in a mechanical resonator

The search for gravitational waves

Gravitational Waves and GRBs from Tidal Disruption of Stars in the Center of Galaxies

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