ACIGA's high optical power test facility

Li, Ju; Aoun, M; Barriga, P.; Blair, David; Brooks, A. F.; Burman, R.; Burston, Raymond; Chin, X T; Chin, E J; Lee, C Y; Coward, D. M.; Cusack, B. J.; Vine, Glenn de; Degallaix, J.; Dumas, J. C.; Garoi, F.; Gras, S.; Gray, Malcolm B.; Hosken, David J.; Howell, E. J.; Jacob, J; Kelly, Thu‐Lan; Lee, B; Lee, K T; Lun, Tian Le Tim; McClelland, D. E.; Mow–Lowry, C. M.; Mudge, D.; Münch, J.; Schediwy, Sascha; Scott, S. M.; Searle, A. S.; Sheard, Benjamin; Slagmolen, B. J. J.; Veitch, P. J.; Winterflood, John; Woolley, Andrew; Yan, Z.; Zhao, C.

doi:10.1088/0264-9381/21/5/077

Cited by 19 publications

(10 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…On this site the Australian International Gravitational Observatory (AIGO) research facility has been developed [27]. It includes an 80 m research interferometer with high performance vibration isolators.…”

Section: Advanced Ligo and Advanced Techniques For Future Enhancementmentioning

confidence: 99%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

View full text Add to dashboard Cite

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,

show abstract

Section: Advanced Ligo and Advanced Techniques For Future Enhancementmentioning

confidence: 99%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

View full text Add to dashboard Cite

show abstract

“…The general principle is to use an auxiliary source of heat for heating the cold parts of the mirror in order to achieve a more homogeneous temperature distribution. The source of heat may be a classical radiator able to radiate infrared energy in a vacuum, for instance, a hot ring near the rear face of the mirror [30, 25, 13, 14, 22, 43]. It may also be an auxiliary laser projector, which can be programmed to scan the mirror surface to produce a given power mask [42].…”

Section: On Thermal Compensation Systemsmentioning

confidence: 99%

On Special Optical Modes and Thermal Issues in Advanced Gravitational Wave Interferometric Detectors

Vinet

2009

Living Rev. Relativ.

View full text Add to dashboard Cite

The sensitivity of present ground-based gravitational wave antennas is too low to detect many events per year. It has, therefore, been planned for years to build advanced detectors allowing actual astrophysical observations and investigations. In such advanced detectors, one major issue is to increase the laser power in order to reduce shot noise. However, this is useless if the thermal noise remains at the current level in the 100 Hz spectral region, where mirrors are the main contributors. Moreover, increasing the laser power gives rise to various spurious thermal effects in the same mirrors. The main goal of the present study is to discuss these issues versus the transverse structure of the readout beam, in order to allow comparison. A number of theoretical studies and experiments have been carried out, regarding thermal noise and thermal effects. We do not discuss experimental problems, but rather focus on some theoretical results in this context about arbitrary order Laguerre-Gauss beams, and other “exotic” beams.

show abstract

“…The radiation pressure force created by the transfer of momentum from photons will be of the order of 1.3 mN [18]. This is enough to cause the suspension pendulum to be deflected by 20 µm, about 40 times the cavity free spectral range [19]. This mirror displacement will modulate the light intensity inside the cavity changing the radiation pressure force.…”

Section: Radiation Pressure and Optical Spring Effectmentioning

confidence: 99%

Technology developments for ACIGA high power test facility for advanced interferometry

Barriga

Barton

Blair

et al. 2005

Class. Quantum Grav.

Self Cite

View full text Add to dashboard Cite

The High Optical Power Test Facility for Advanced Interferometry has been built by the Australian Consortium for Interferometric Gravitational Astronomy north of Perth in Western Australia. An 80 m suspended cavity has been prepared in collaboration with LIGO, where a set of experiments to test suspension control and thermal compensation will soon take place. Future experiments will investigate radiation pressure instabilities and optical spring effects in a high power optical cavity with ∼200 kW circulating power. The facility combines research and development undertaken by all consortium members, whose latest results are presented.

show abstract

ACIGA's high optical power test facility

Cited by 19 publications

References 23 publications

Gravitational wave astronomy: the current status

Gravitational wave astronomy: the current status

On Special Optical Modes and Thermal Issues in Advanced Gravitational Wave Interferometric Detectors

Technology developments for ACIGA high power test facility for advanced interferometry

Contact Info

Product

Resources

About