The ultracryogenic gravitational-wave detector AURIGA

Cerdonio, M.; Bonaldi, M.; Carlesso, D; Cavallini, Enrico; Caruso, Stefano; Colombo, A.; Falferi, P.; Fontana, G.; Fortini, P.; Mezzena, R.; Ortolan, A.; Prodi, G. A.; Taffarello, L.; Vedovato, G.; Vitale, S.; Zendri, J. P.

doi:10.1088/0264-9381/14/6/016

Cited by 79 publications

(61 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…the detection principle was based on the GW-induced resonant excitation of vibrational modes of metal cylinders. cryogenically cooled devices reached strain sensitivities of about h = 10 − 18 around a kilohertz, over a band width of a few Hz, in the 1990s and have been further improved since then [89][90][91][92] . today, the most sensitive instruments are laser interferometers with kilometre size arm lengths.…”

Section: Box 1 Past and Present Gw Detectorsmentioning

confidence: 99%

Quantum metrology for gravitational wave astronomy

et al. 2010

View full text Add to dashboard Cite

einstein's general theory of relativity predicts that accelerating mass distributions produce gravitational radiation, analogous to electromagnetic radiation from accelerating charges. these gravitational waves (GWs) have not been directly detected to date, but are expected to open a new window to the universe once the detectors, kilometre-scale laser interferometers measuring the distance between quasi-free-falling mirrors, have achieved adequate sensitivity. recent advances in quantum metrology may now contribute to provide the required sensitivity boost. the so-called squeezed light is able to quantum entangle the high-power laser fields in the interferometer arms, and could have a key role in the realization of GW astronomy. When Galileo Galilei pointed his telescope towards the sky 400 years ago, he discovered events that had never been seen before. In subsequent centuries, a variety of telescopes were invented, covering a large part of the electromagnetic spectrum. These telescopes enabled observations that now form the basis of our understanding of the origin and the evolution of the Universe. Einstein's general theory of relativity, quite often simply 'general relativity' 1 , predicts the existence of a completely different kind of radiation, the so-called gravitational waves (GWs). As electromagnetic radiation is generated by acceleration of charges, so are GWs produced by accelerating mass distributions, such as supernova explosions or binary neutron stars that spiral into each other. GWs may also be emitted by objects that are electromagnetically dark, black holes, for example. Instruments that can directly observe GWs may well be able to 'light up' the dark side of our Universe. The analysis of the waves' spectrum and their time evolution will provide information about the nature of astrophysical and cosmological events that produced the waves. So far, GWs have not been directly observed.Suitable telescopes for GW astronomy are kilometre-scale laser interferometers that measure the distance between quasi-free-falling mirrors. This measurement can be used to infer changes of spacetime curvature. Current GW detectors are already able to measure extremely small changes of distance with strain sensitivity down to the order of 10 − 22. However, quantum physics imposes a fundamental limit on measurement sensitivity, in particular, in terms of photon-counting noise. In the past, the GW signal with respect to the photon-counting noise could only be increased by increasing the light power. Unfortunately, increasing light power will eventually produce measurable quantum radiation pressure noise. In addition it also increases the thermal load inside the detector and is problematic with respect to the concept of overall low noise. Squeezed light avoids these problems by increasing the measurement sensitivity without increasing the light power. The application of squeezed light is a quantum technology. Injected into an interferometer, it entangles the high-power laser fields in the interferometer arms. The photon...

show abstract

Section: Box 1 Past and Present Gw Detectorsmentioning

confidence: 99%

Quantum metrology for gravitational wave astronomy

et al. 2010

View full text Add to dashboard Cite

show abstract

“…We are only just now learning to exploit the opportunities it is creating for us. Within the next year, several large ground-based interferometric detectors will begin full operation [15][16][17], and existing cryogenic acoustic detectors [18][19][20][21] will see significant improvements in sensitivity. Within the next decade we should see further enhancements in the capability of all these instruments [22][23][24], and the deployment of the space-based interferometric detector LISA (Laser Interferometer Space Antenna) [25,26].…”

Section: Binary Pulsarsmentioning

confidence: 99%

Bounding the mass of the graviton using binary pulsar observations

2002

View full text Add to dashboard Cite

The close agreement between the predictions of dynamical general relativity for the radiated power of a compact binary system and the observed orbital decay of the binary pulsars PSR B1913+16 and PSR B1534+12 allows us to bound the graviton mass to be less than 7.6 × 10 −20 eV with 90% confidence. This bound is the first to be obtained from dynamic, as opposed to staticfield, relativity. The resulting limit on the graviton mass is within two orders of magnitude of that from solar system measurements, and can be expected to improve with further observations. Typeset using REVT E X

show abstract

“…Various resonant mass detectors are now operating [21][22][23][24][25]. In [38], the first experiment of cross-correlation…”

Section: A Gw Detectors and Bbn Boundmentioning

confidence: 99%

“…The experimental efforts are converging towards the possibility of direct detection of stochastically distributed gravitational waves [19,20]. Various resonant mass detectors are now operating at a typical frequency of the order of kHz (Allegro [21], Auriga [22], Explorer [23], Nautilus [24], Niobe [25]) and four Michelson interferometers (GEO-600 [26],TAMA-400 [27], LIGO [29] and VIRGO [28]) will soon be operating in a wide frequency band from a few Hz up to 10 kHz. It is interesting, in the context of ABBN, to elaborate on the possibility that the additional relativistic species are of gravitational origin.…”

Section: Introductionmentioning

confidence: 99%

Big bang nucleosynthesis, matter-antimatter regions, extra relativistic species, and relic gravitational waves

2002

View full text Add to dashboard Cite

Provided that matter-antimatter domains are present at the onset of big bang nucleosynthesis (BBN), the number of allowed additional relativistic species increases, compared to the standard scenario when matter-antimatter domains are absent. The extra relativistic species may take the form of massless fermions or even massless bosons, like relic gravitons. The number of additional degrees of freedom compatible with BBN depends, in this framework, upon the typical scale of the domains and the antimatter fraction. Since the presence of matter-antimatter domains allows a reduction of the neutron to proton ratio prior to the formation of 4 He, large amounts of radiation-like energy density are allowed. Our results are compared with other constraints on the number of supplementary relativistic degrees of freedom and with different nonstandard BBN scenarios where the reduction of the neutron to proton ratio occurs via a different physical mechanism. The implications of our considerations for the upper limits on stochastic gravitational waves backgrounds of cosmological origin are outlined.

show abstract

The ultracryogenic gravitational-wave detector AURIGA

Cited by 79 publications

References 11 publications

Quantum metrology for gravitational wave astronomy

Quantum metrology for gravitational wave astronomy

Bounding the mass of the graviton using binary pulsar observations

Big bang nucleosynthesis, matter-antimatter regions, extra relativistic species, and relic gravitational waves

Contact Info

Product

Resources

About