ORCID Profile
0000-0002-2471-3828
Current Organisation
Australian National University
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Research Topics
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.
Top 5 Research Topics
ANZSRC Field of Research (FoR)
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
ANZSRC Socio-Economic Objective (SEO)
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 |
Related Links
Publications
ACIGA's high optical power test facility
Publisher: IOP Publishing
Date: 11-02-2004
Picometer level displacement metrology with digitally enhanced heterodyne interferometry
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.
Technology developments for ACIGA high power test facility for advanced interferometry
Publisher: IOP Publishing
Date: 21-04-2005
Double pass locking and spatial mode locking for gravitational wave detectors
Publisher: IOP Publishing
Date: 19-03-2002
AIGO: a southern hemisphere detector for the worldwide array of ground-based interferometric gravitational wave detectors
Publisher: IOP Publishing
Date: 06-04-2010
GW170608: Observation of a 19 Solar-mass Binary Black Hole Coalescence
Publisher: American Astronomical Society
Date: 18-12-2017
Arm-length stabilisation for interferometric gravitational-wave detectors using frequency-doubled auxiliary lasers
Publisher: The Optical Society
Date: 19-12-2012
DOI: 10.1364/OE.20.000081
A gravitational wave observatory operating beyond the quantum shot-noise limit
Publisher: Springer Science and Business Media LLC
Date: 11-09-2011
DOI: 10.1038/NPHYS2083
A gravitational-wave standard siren measurement of the Hubble constant
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.
Observation of optical torsional stiffness in a high optical power cavity
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.
Thermal lensing compensation principle for the ACIGA's High Optical Power Test Facility Test 1
Publisher: Springer Science and Business Media LLC
Date: 09-2005
Frequency dependence of thermal noise in gram-scale cantilever flexures
Publisher: American Physical Society (APS)
Date: 15-12-2015
Control and tuning of a suspended Fabry-Perot cavity using digitally enhanced heterodyne interferometry
Publisher: The Optical Society
Date: 28-11-2012
DOI: 10.1364/OL.37.004952
Tip-tilt mirror suspension: Beam steering for advanced laser interferometer gravitational wave observatory sensing and control signals
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.
A cryogenic silicon interferometer for gravitational-wave detection
Publisher: IOP Publishing
Date: 29-07-2020
Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A
Publisher: American Astronomical Society
Date: 16-10-2017
Direct observation of the thermal noise spectrum of a silicon flexure membrane
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.
Second-generation laser interferometry for gravitational wave detection: ACIGA progress
Publisher: IOP Publishing
Date: 20-09-2001
TorPeDO: A Low Frequency Gravitational Force Sensor
Publisher: IOP Publishing
Date: 05-2016
Direct measurement of absorption-induced wavefront distortion in high optical power systems
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.
Achieving resonance in the Advanced LIGO gravitational-wave interferometer
Publisher: IOP Publishing
Date: 26-11-2014
The basic physics of the binary black hole merger GW150914
Publisher: Wiley
Date: 04-10-2016
Alignment locking to suspended Fabry-Perot cavity
Publisher: Springer Science and Business Media LLC
Date: 09-2005
High performance vibration isolation using springs in Euler column buckling mode
Publisher: Elsevier BV
Date: 07-2002
Gravitational-wave physics with Cosmic Explorer: Limits to low-frequency sensitivity
Publisher: American Physical Society (APS)
Date: 21-06-2021
The torsion pendulum dual oscillator for low-frequency Newtonian noise detection
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.
Quantum enhanced kHz gravitational wave detector with internal squeezing
Publisher: IOP Publishing
Date: 05-03-2020
Digital laser frequency stabilization using an optical cavity
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 08-2010
First Search for Gravitational Waves from Known Pulsars with Advanced LIGO
Publisher: American Astronomical Society
Date: 07-04-2017
Publisher’s Note: First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds [Phys. Rev. D76, 022001 (2007)]
Publisher: American Physical Society (APS)
Date: 10-03-2008
Mechanical characterisation of the TorPeDO: A low frequency gravitational force sensor
Publisher: IOP Publishing
Date: 05-06-2017
Publisher’s Note: Upper limits on gravitational wave emission from 78 radio pulsars [Phys. Rev. D76, 042001 (2007)]
Publisher: American Physical Society (APS)
Date: 10-03-2008
Publisher’s Note: All-sky search for periodic gravitational waves in LIGO S4 data [Phys. Rev. D77, 022001 (2008)]
Publisher: American Physical Society (APS)
Date: 10-03-2008
Publisher’s Note: Upper limit map of a background of gravitational waves [Phys. Rev. D76, 082003 (2007)]
Publisher: American Physical Society (APS)
Date: 10-03-2008
Effects of transients in LIGO suspensions on searches for gravitational waves
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.
Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA
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.
Frequency stability of spatial mode interference (tilt) locking
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 11-2002
Nondegenerate internal squeezing: An all-optical, loss-resistant quantum technique for gravitational-wave detection
Publisher: American Physical Society (APS)
Date: 05-08-2022
ERRATUM: “BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE CRAB PULSAR” (2008, ApJ, 683, L45)
Publisher: American Astronomical Society
Date: 06-11-2009
Low-frequency terrestrial gravitational-wave detectors
Publisher: American Physical Society (APS)
Date: 13-12-2013
Testing the suppression of opto-acoustic parametric interactions using optical feedback control
Publisher: IOP Publishing
Date: 06-04-2010
Effects of waveform model systematics on the interpretation of GW150914
Publisher: IOP Publishing
Date: 12-04-2017
A robust single-beam optical trap for a gram-scale mechanical oscillator
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.
Optimal quantum noise cancellation with an entangled witness channel
Publisher: American Physical Society (APS)
Date: 28-10-2021
Phase-sensitive reflection technique for characterization of a fabry-perot interferometer
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.
Search for gravitational-wave bursts in LIGO data from the fourth science run
Publisher: IOP Publishing
Date: 24-10-2007
High-sensitivity three-mode optomechanical transducer
Publisher: American Physical Society (APS)
Date: 16-12-2011
Mechanical amorphization, flash heating, and frictional melting: Dramatic changes to fault surfaces during the first millisecond of earthquake slip
Publisher: Geological Society of America
Date: 20-10-2016
DOI: 10.1130/G38242.1
Observation of a potential future sensitivity limitation from ground motion at LIGO Hanford
Publisher: American Physical Society (APS)
Date: 05-05-2020
Status of ACIGA High Power Test Facility for advanced interferometry
Publisher: SPIE
Date: 29-09-2004
DOI: 10.1117/12.581300
Implications of Dedicated Seismometer Measurements on Newtonian-Noise Cancellation for Advanced LIGO
Publisher: American Physical Society (APS)
Date: 28-11-2018
Australia's Role in Gravitational Wave Detection
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.
Searching for a Stochastic Background of Gravitational Waves with the Laser Interferometer Gravitational-Wave Observatory
Publisher: American Astronomical Society
Date: 20-04-2007
DOI: 10.1086/511329
High dynamic range flexure transfer function measurement
Publisher: IOP Publishing
Date: 15-03-2002
Optomechanical design and construction of a vacuum-compatible optical parametric oscillator for generation of squeezed light
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.
Observation of three-mode parametric interactions in long optical cavities
Publisher: American Physical Society (APS)
Date: 06-08-2008
Status of the Australian Consortium for Interferometric Gravitational Astronomy
Publisher: IOP Publishing
Date: 24-03-2006
Quantum squeezed light in gravitational-wave detectors
Publisher: IOP Publishing
Date: 05-09-2014
Erratum: All-sky search for periodic gravitational waves in LIGO S4 data [Phys. Rev. D77, 022001 (2008)]
Publisher: American Physical Society (APS)
Date: 23-12-2009
Stable transfer of an optical frequency standard via a 4.6 km optical fiber
Publisher: The Optical Society
Date: 26-02-2010
DOI: 10.1364/OE.18.005213
Large dynamic range, high resolution optical heterodyne readout for high velocity slip events
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.
Practical test mass and suspension configuration for a cryogenic kilohertz gravitational wave detector
Publisher: American Physical Society (APS)
Date: 18-12-2020
Towards the SQL: Status of the direct thermal-noise measurements at the ANU
Publisher: IOP Publishing
Date: 02-03-2011
DC readout experiment in Enhanced LIGO
Publisher: IOP Publishing
Date: 23-02-2012
Gingin High Optical Power Test Facility
Publisher: IOP Publishing
Date: 02-03-2006
Dc readout experiment at the Caltech 40m prototype interferometer
Publisher: IOP Publishing
Date: 15-05-2008
Experimental demonstration of in-loop intracavity intensity-noise suppression
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 03-2005
Measurable signatures of quantum mechanics in a classical spacetime
Publisher: American Physical Society (APS)
Date: 09-08-2017
Publisher’s Note: First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds [Phys. Rev. DPRVDAQ0556-282176, 022001 (2007)]
Publisher: American Physical Society (APS)
Date: 30-07-2007
Compensation of Strong Thermal Lensing in High-Optical-Power Cavities
Publisher: American Physical Society (APS)
Date: 12-06-2006
Observation of Squeezed Light in the 2 μ m Region
Publisher: American Physical Society (APS)
Date: 17-05-2018
Feedback control of thermal lensing in a high optical power cavity
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.
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