ORCID Profile
0000-0002-2471-3828
Current Organisation
Australian National University
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In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Astronomical and Space Sciences | General Relativity and Gravitational Waves | Astronomical and Space Instrumentation | Classical and Physical Optics | Astronomical sciences | Astronomical and Space Sciences not elsewhere classified | Lasers and quantum electronics | General relativity and gravitational waves | Quantum Optics | Lasers and Quantum Electronics | Seismology and Seismic Exploration | Space instrumentation | Astronomical Sciences Not Elsewhere Classified | Synchrotrons; Accelerators; Instruments and Techniques | Optical Technology | Cosmology and extragalactic astronomy | Optical Physics not elsewhere classified | Instruments And Techniques | Other Physical Sciences | Optics And Opto-Electronic Physics
Expanding Knowledge in the Physical Sciences | Expanding Knowledge in Technology | Expanding Knowledge in Engineering | Scientific Instruments | Physical sciences | Expanding Knowledge in the Information and Computing Sciences |
Publisher: IOP Publishing
Date: 11-02-2004
Publisher: The Optical Society
Date: 09-01-2009
DOI: 10.1364/OE.17.000828
Abstract: Digitally enhanced heterodyne interferometry is a laser metrology technique employing pseudo-random codes phase modulated onto an optical carrier. We present the first characterization of the technique's displacement sensitivity. The displacement of an optical cavity was measured using digitally enhanced heterodyne interferometry and compared to a simultaneous readout based on conventional Pound-Drever-Hall locking. The techniques agreed to within 5 pm/ radicalHz at 1 Hz, providing an upper bound to the displacement noise of digitally enhanced heterodyne interferometry. These measurements employed a real-time signal extraction system implemented on a field programmable gate array, suitable for closed-loop control applications. We discuss the applicability of digitally enhanced heterodyne interferometry for lock acquisition of advanced gravitational wave detectors.
Publisher: IOP Publishing
Date: 21-04-2005
Publisher: IOP Publishing
Date: 19-03-2002
Publisher: IOP Publishing
Date: 06-04-2010
Publisher: American Astronomical Society
Date: 18-12-2017
Publisher: The Optical Society
Date: 19-12-2012
DOI: 10.1364/OE.20.000081
Publisher: Springer Science and Business Media LLC
Date: 11-09-2011
DOI: 10.1038/NPHYS2083
Publisher: Springer Science and Business Media LLC
Date: 16-10-2017
DOI: 10.1038/NATURE24471
Abstract: On 17 August 2017, the Advanced LIGO and Virgo detectors observed the gravitational-wave event GW170817-a strong signal from the merger of a binary neutron-star system. Less than two seconds after the merger, a γ-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both gravitational waves and electromagnetic waves represents the first 'multi-messenger' astronomical observation. Such observations enable GW170817 to be used as a 'standard siren' (meaning that the absolute distance to the source can be determined directly from the gravitational-wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic 'distance ladder': the gravitational-wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements, while being completely independent of them. Additional standard siren measurements from future gravitational-wave sources will enable the Hubble constant to be constrained to high precision.
Publisher: AIP Publishing
Date: 23-02-2009
DOI: 10.1063/1.3088850
Abstract: We have observed negative optical torsional rigidity in an 80 m suspended high optical power cavity that would induce the Sidles–Sigg instability as a result of sufficient circulating power. The magnitude of the negative optical spring constant per unit power is a few μN m/W as the result of the optical torsional stiffness in the yaw mode of a suspended mirror Fabry–Pérot cavity. It has been observed to depend on the g-factor of the cavity which is in agreement with the Sidles–Sigg theory.
Publisher: Springer Science and Business Media LLC
Date: 09-2005
Publisher: American Physical Society (APS)
Date: 15-12-2015
Publisher: The Optical Society
Date: 28-11-2012
DOI: 10.1364/OL.37.004952
Publisher: AIP Publishing
Date: 12-2011
DOI: 10.1063/1.3669532
Abstract: We describe the design of a small optic suspension system, referred to as the tip-tilt mirror suspension, used to isolate selected small optics for the interferometer sensing and control beams in the advanced LIGO gravitational wave detectors. The suspended optics are isolated in all 6 degrees of freedom, with eigenmode frequencies between 1.3 Hz and 10 Hz. The suspended optic has voice-coil actuators which provide an angular range of ±4 mrad in the pitch and yaw degrees of freedom.
Publisher: IOP Publishing
Date: 29-07-2020
Publisher: American Astronomical Society
Date: 16-10-2017
Publisher: AIP Publishing
Date: 09-01-2023
DOI: 10.1063/5.0131984
Abstract: We present a direct measurement of the displacement noise spectrum of a macroscopic silicon flexure at room temperature. A cantilever attached to the 100 μm thick flexure holds a mirror which forms part of an optical cavity to enhance the displacement sensitivity to thermal noise. We predict the displacement noise spectrum using a simple model that assumes the dominant source of frequency-dependent loss is thermo-elastic d ing and find good agreement with the experimental data. The measurement is consistent with a frequency-independent loss of ϕ0,fi=1.6×10−5 combined with frequency-dependent thermo-elastic d ing as the dominant losses. A crossover between the two that occurs well above the flexure resonant frequency allows a broadband measurement of the thermal noise of the silicon flexure. The flexure material, geometry, and measurement band are similar to those of planned future gravitational wave detectors.
Publisher: IOP Publishing
Date: 20-09-2001
Publisher: IOP Publishing
Date: 05-2016
Publisher: The Optical Society
Date: 07-01-2009
DOI: 10.1364/AO.48.000355
Abstract: Wavefront distortion due to absorption in the substrates and coatings of mirrors in advanced gravitational wave interferometers has the potential to compromise the operation and sensitivity of these interferometers [Opt. Lett.29, 2635-2637 (2004)]. We report the first direct spatially-resolved measurement, to our knowledge, of such wavefront distortion in a high optical power cavity. The measurement was made using an ultrahigh sensitivity Hartmann wavefront sensor on a dedicated test facility. The sensitivity of the sensor was lambda/730, where lambda=800 nm.
Publisher: IOP Publishing
Date: 26-11-2014
Publisher: Wiley
Date: 04-10-2016
Publisher: Springer Science and Business Media LLC
Date: 09-2005
Publisher: Elsevier BV
Date: 07-2002
Publisher: American Physical Society (APS)
Date: 21-06-2021
Publisher: AIP Publishing
Date: 15-05-2023
DOI: 10.1063/5.0145092
Abstract: We present a torsion pendulum dual oscillator sensor designed toward the direct detection of Newtonian noise. We discuss the sensitivity limitations of the system, experimental performance characterization results, and prospectives to improve performance. The sensor is being developed to contribute to the mitigation of Newtonian noise impacts in the sensitivities of next generation terrestrial gravitational-wave detectors.
Publisher: IOP Publishing
Date: 05-03-2020
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 08-2010
Publisher: American Astronomical Society
Date: 07-04-2017
Publisher: American Physical Society (APS)
Date: 10-03-2008
Publisher: IOP Publishing
Date: 05-06-2017
Publisher: American Physical Society (APS)
Date: 10-03-2008
Publisher: American Physical Society (APS)
Date: 10-03-2008
Publisher: American Physical Society (APS)
Date: 10-03-2008
Publisher: AIP Publishing
Date: 12-2017
DOI: 10.1063/1.5000264
Abstract: This paper presents an analysis of the transient behavior of the Advanced LIGO (Laser Interferometer Gravitational-wave Observatory) suspensions used to seismically isolate the optics. We have characterized the transients in the longitudinal motion of the quadruple suspensions during Advanced LIGO’s first observing run. Propagation of transients between stages is consistent with modeled transfer functions, such that transient motion originating at the top of the suspension chain is significantly reduced in litude at the test mass. We find that there are transients seen by the longitudinal motion monitors of quadruple suspensions, but they are not significantly correlated with transient motion above the noise floor in the gravitational wave strain data, and therefore do not present a dominant source of background noise in the searches for transient gravitational wave signals. Using the suspension transfer functions, we compared the transients in a week of gravitational wave strain data with transients from a quadruple suspension. Of the strain transients between 10 and 60 Hz, 84% are loud enough that they would have appeared above the sensor noise in the top stage quadruple suspension monitors if they had originated at that stage at the same frequencies. We find no significant temporal correlation with the suspension transients in that stage, so we can rule out suspension motion originating at the top stage as the cause of those transients. However, only 3.2% of the gravitational wave strain transients are loud enough that they would have been seen by the second stage suspension sensors, and none of them are above the sensor noise levels of the penultimate stage. Therefore, we cannot eliminate the possibility of transient noise in the detectors originating in the intermediate stages of the suspension below the sensing noise.
Publisher: Springer Science and Business Media LLC
Date: 26-04-2018
DOI: 10.1007/S41114-018-0012-9
Abstract: We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and $$90\\%$$ 90 % credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5– $$20~\\mathrm {deg}^2$$ 20 deg 2 requires at least three detectors of sensitivity within a factor of $$\\sim 2$$ ∼ 2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 11-2002
Publisher: American Physical Society (APS)
Date: 05-08-2022
Publisher: American Astronomical Society
Date: 06-11-2009
Publisher: American Physical Society (APS)
Date: 13-12-2013
Publisher: IOP Publishing
Date: 06-04-2010
Publisher: IOP Publishing
Date: 12-04-2017
Publisher: Springer Science and Business Media LLC
Date: 06-11-2017
DOI: 10.1038/S41598-017-15179-X
Abstract: Precise optical control of microscopic particles has been mastered over the past three decades, with atoms, molecules and nano-particles now routinely trapped and cooled with extraordinary precision, enabling rapid progress in the study of quantum phenomena. Achieving the same level of control over macroscopic objects is expected to bring further advances in precision measurement, quantum information processing and fundamental tests of quantum mechanics. However, cavity optomechanical systems dominated by radiation pressure – so-called ‘optical springs’ – are inherently unstable due to the delayed dynamical response of the cavity. Here we demonstrate a fully stable, single-beam optical trap for a gram-scale mechanical oscillator. The interaction of radiation pressure with thermo-optic feedback generates d ing that exceeds the mechanical loss by four orders of magnitude. The stability of the resultant spring is robust to changes in laser power and detuning, and allows purely passive self-locking of the cavity. Our results open up a new way of trapping and cooling macroscopic objects for optomechanical experiments.
Publisher: American Physical Society (APS)
Date: 28-10-2021
Publisher: The Optical Society
Date: 20-07-2000
DOI: 10.1364/AO.39.003638
Abstract: Using a radio frequency coherent modulation and demodulation technique, we explicitly measure both the litude and the phase response of Fabry-Perot interferometers in reflection. This allows us to differentiate clearly between overcoupled and undercoupled cavities and allows a detailed measurement of the full width at half-maximum, the free spectral range, and the finesse of the cavities.
Publisher: IOP Publishing
Date: 24-10-2007
Publisher: American Physical Society (APS)
Date: 16-12-2011
Publisher: Geological Society of America
Date: 20-10-2016
DOI: 10.1130/G38242.1
Publisher: American Physical Society (APS)
Date: 05-05-2020
Publisher: SPIE
Date: 29-09-2004
DOI: 10.1117/12.581300
Publisher: American Physical Society (APS)
Date: 28-11-2018
Publisher: Cambridge University Press (CUP)
Date: 2003
DOI: 10.1071/AS03036
Abstract: An enormous effort is underway worldwide to attempt to detect gravitational waves. If successful, this will open a new frontier in astronomy. An essential portion of this effort is being carried out in Australia by the Australian Consortium for Interferometric Gravitational Astronomy (ACIGA), with research teams working at the Australia National University, University of Western Australia, and University of Adelaide involving scientists and students representing many more institutions and nations. ACIGA is developing ultrastable high-power continuous-wave lasers for the next generation interferometric gravity wave detectors researching the problems associated with high optical power in resonant cavities opening frontiers in advanced interferometry configurations, quantum optics, and signal extraction and is the world's leader in high-performance vibration isolation and suspension design. ACIGA has also been active in theoretical research and modelling of potential astronomical gravitational wave sources, and in developing data analysis detection algorithms. ACIGA has opened a research facility north of Perth, Western Australia, which will be the culmination of these efforts. This paper briefly reviews ACIGA's research activities and the prospects for gravitational wave astronomy in the southern hemisphere.
Publisher: American Astronomical Society
Date: 20-04-2007
DOI: 10.1086/511329
Publisher: IOP Publishing
Date: 15-03-2002
Publisher: AIP Publishing
Date: 06-2016
DOI: 10.1063/1.4953326
Abstract: With the recent detection of gravitational waves, non-classical light sources are likely to become an essential element of future detectors engaged in gravitational wave astronomy and cosmology. Operating a squeezed light source under high vacuum has the advantages of reducing optical losses and phase noise compared to techniques where the squeezed light is introduced from outside the vacuum. This will ultimately provide enhanced sensitivity for modern interferometric gravitational wave detectors that will soon become limited by quantum noise across much of the detection bandwidth. Here we describe the optomechanical design choices and construction techniques of a near monolithic glass optical parametric oscillator that has been operated under a vacuum of 10−6 mbar. The optical parametric oscillator described here has been shown to produce 8.6 dB of quadrature squeezed light in the audio frequency band down to 10 Hz. This performance has been maintained for periods of around an hour and the system has been under vacuum continuously for several months without a degradation of this performance.
Publisher: American Physical Society (APS)
Date: 06-08-2008
Publisher: IOP Publishing
Date: 24-03-2006
Publisher: IOP Publishing
Date: 05-09-2014
Publisher: American Physical Society (APS)
Date: 23-12-2009
Publisher: The Optical Society
Date: 26-02-2010
DOI: 10.1364/OE.18.005213
Publisher: AIP Publishing
Date: 06-2022
DOI: 10.1063/5.0082970
Abstract: We present a free-space optical displacement sensor for measuring geological slip event displacements within a laboratory setting. This sensor utilizes a fiberized Mach-Zehnder based optical heterodyne system coupled with a digital phase lock loop, providing a large dynamic range (multiple centimeters), high displacement resolution (with an litude spectral density of & −10 m/Hz for frequencies above 100 Hz), and high velocity tracking capabilities (up to 4.96 m/s). This displacement sensor is used to increase the displacement and the time sensitivity for measuring laboratory-scale earthquakes induced in geological s les by using a triaxial compression apparatus. The sensor architecture provides an improved displacement and time resolution for the millisecond-duration slip events, at high containment and loading pressure and high temperatures. Alternatively, the sensor implementation can be used for other non-contact displacement readouts that required high velocity tracking with low noise and large dynamic range sensing. We use 13 high-velocity slip events in Fontainebleau sandstone to show the large dynamic range displacement tracking ability and displacement litude spectral densities to demonstrate the optical readout’s unique sensing capabilities.
Publisher: American Physical Society (APS)
Date: 18-12-2020
Publisher: IOP Publishing
Date: 02-03-2011
Publisher: IOP Publishing
Date: 23-02-2012
Publisher: IOP Publishing
Date: 02-03-2006
Publisher: IOP Publishing
Date: 15-05-2008
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 03-2005
Publisher: American Physical Society (APS)
Date: 09-08-2017
Publisher: American Physical Society (APS)
Date: 30-07-2007
Publisher: American Physical Society (APS)
Date: 12-06-2006
Publisher: American Physical Society (APS)
Date: 17-05-2018
Publisher: AIP Publishing
Date: 10-2008
DOI: 10.1063/1.2982239
Abstract: This paper reports automatic compensation of strong thermal lensing in a suspended 80 m optical cavity with sapphire test mass mirrors. Variation of the transmitted beam spot size is used to obtain an error signal to control the heating power applied to the cylindrical surface of an intracavity compensation plate. The negative thermal lens created in the compensation plate compensates the positive thermal lens in the sapphire test mass, which was caused by the absorption of the high intracavity optical power. The results show that feedback control is feasible to compensate the strong thermal lensing expected to occur in advanced laser interferometric gravitational wave detectors. Compensation allows the cavity resonance to be maintained at the fundamental mode, but the long thermal time constant for thermal lensing control in fused silica could cause difficulties with the control of parametric instabilities.
Start Date: 06-2020
End Date: 06-2021
Amount: $700,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 09-2021
End Date: 08-2025
Amount: $3,000,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 05-2017
End Date: 05-2021
Amount: $850,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2013
End Date: 03-2017
Amount: $990,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 07-2016
End Date: 12-2017
Amount: $650,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2015
End Date: 2017
Amount: $470,800.00
Funder: Australian Research Council
View Funded ActivityStart Date: 05-2011
End Date: 12-2012
Amount: $550,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2007
End Date: 12-2010
Amount: $810,090.00
Funder: Australian Research Council
View Funded ActivityStart Date: 03-2014
End Date: 02-2018
Amount: $752,111.00
Funder: Australian Research Council
View Funded ActivityStart Date: 04-2017
End Date: 03-2024
Amount: $31,300,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 07-2022
End Date: 06-2023
Amount: $385,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 01-2024
End Date: 01-2025
Amount: $460,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 04-2024
End Date: 03-2031
Amount: $35,000,000.00
Funder: Australian Research Council
View Funded Activity