ORCID Profile
0000-0001-7987-295X
Current Organisation
University of Western Australia
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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)
General Relativity and Gravitational Waves | Astronomical and Space Sciences | Signal Processing | Astronomical and Space Instrumentation | Lasers and Quantum Electronics | Adaptive Agents and Intelligent Robotics | Astronomical sciences | Simulation And Modelling | Optical Physics | Artificial Intelligence and Image Processing | Astronomical and Space Sciences not elsewhere classified | Stellar Astronomy and Planetary Systems | Distributed and Grid Systems | Astronomical instrumentation | Image Processing | Signal Processing | Simulation and Modelling | Astronomy And Astrophysics | High Energy Astrophysics; Cosmic Rays | Astronomical sciences not elsewhere classified | Classical and Physical Optics | Cosmology and Extragalactic Astronomy
ANZSRC Socio-Economic Objective (SEO)
Expanding Knowledge in the Physical Sciences | Expanding Knowledge in Technology | Expanding Knowledge in Engineering | Application tools and system utilities | Command, Control and Communications | Higher education | Application Software Packages (excl. Computer Games) | Scientific Instruments | Expanding Knowledge in the Information and Computing Sciences | Computer hardware and electronic equipment not elsewhere classified |
Related Links
Publications
Dependence of the orbital modulation of X-rays from 4U 1820-303 on the accretion rate
Publisher: Oxford University Press (OUP)
Date: 21-05-2007
On the Eccentricity Distribution of Coalescing Black Hole Binaries Driven by the Kozai Mechanism in Globular Clusters
Publisher: American Astronomical Society
Date: 20-11-2003
DOI: 10.1086/378794
Detection and localization of single-source gravitational waves with pulsar timing arrays
Publisher: Oxford University Press (OUP)
Date: 25-03-2015
DOI: 10.1093/MNRAS/STV381
Limits on Gravitational-Wave Emission from Selected Pulsars Using LIGO Data
Publisher: American Physical Society (APS)
Date: 12-05-2005
A method for the detection of gravitational waves from inspiralling compact binaries using a fast chirp transform
Publisher: IOP Publishing
Date: 13-03-2002
DETECTING GRAVITATIONAL WAVES AND THEIR ELECTROMAGNETIC COUNTERPARTS
Publisher: World Scientific Pub Co Pte Lt
Date: 09-2011
DOI: 10.1142/S021827181101989X
Abstract: In the next decade, we expect a first detection of gravitational waves predicted by Einstein's general theory of relativity. A detection of their electromagnetic counterparts will significantly contribute to our confidence in a first time detection and identification of the source. We discuss the challenges in using gravitational-wave events as triggers for prompt follow-up electromagnetic observations. We demonstrate that wide-field cameras are desirable for follow-up observations of gravitational wave sources and that a larger gravitational wave detector network, e.g. adding AIGO detector in Australia, can significantly help pinpoint the direction of gravitational wave sources. We also argue that low-latency real-time detection methods and hardware acceleration using graphics processing units will help generate prompt gravitational-wave triggers within the time frames allowed for electromagnetic follow-ups in the era of advanced detectors.
GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M⊙
Publisher: American Astronomical Society
Date: 19-03-2020
Abstract: On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to ( – if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the in idual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250–2810 .
Detection and localization of continuous gravitational waves with pulsar timing arrays: the role of pulsar terms
Publisher: Oxford University Press (OUP)
Date: 16-06-2016
An assessment of the association between a fast radio burst and binary neutron star merger
Publisher: Springer Science and Business Media LLC
Date: 27-03-2023
An all-sky search for continuous gravitational waves in the Parkes Pulsar Timing Array data set
Publisher: Oxford University Press (OUP)
Date: 17-09-2014
Geometrical expression for the angular resolution of a network of gravitational-wave detectors
Publisher: American Physical Society (APS)
Date: 08-04-2010
Search for the isotropic stochastic background using data from Advanced LIGO’s second observing run
Publisher: American Physical Society (APS)
Date: 04-09-2019
Parkes Pulsar Timing Array constraints on ultralight scalar-field dark matter
Publisher: American Physical Society (APS)
Date: 05-11-2018
Geometrical expression of the angular resolution of a network of gravitational-wave detectors and improved localization methods
Publisher: IOP Publishing
Date: 07-2008
Search for intermediate mass black hole binaries in the first and second observing runs of the Advanced LIGO and Virgo network
Publisher: American Physical Society (APS)
Date: 30-09-2019
Time-frequency analysis of extreme-mass-ratio inspiral signals in mock LISA data
Publisher: IOP Publishing
Date: 07-2008
The Mock LISA Data Challenges: from Challenge 1B to Challenge 3
Publisher: IOP Publishing
Date: 02-09-2008
Search for Eccentric Binary Black Hole Mergers with Advanced LIGO and Advanced Virgo during Their First and Second Observing Runs
Publisher: American Astronomical Society
Date: 30-09-2019
Abstract: When formed through dynamical interactions, stellar-mass binary black holes (BBHs) may retain eccentric orbits ( e 0.1 at 10 Hz) detectable by ground-based gravitational-wave detectors. Eccentricity can therefore be used to differentiate dynamically formed binaries from isolated BBH mergers. Current template-based gravitational-wave searches do not use waveform models associated with eccentric orbits, rendering the search less efficient for eccentric binary systems. Here we present the results of a search for BBH mergers that inspiral in eccentric orbits using data from the first and second observing runs (O1 and O2) of Advanced LIGO and Advanced Virgo. We carried out the search with the coherent WaveBurst algorithm, which uses minimal assumptions on the signal morphology and does not rely on binary waveform templates. We show that it is sensitive to binary mergers with a detection range that is weakly dependent on eccentricity for all bound systems. Our search did not identify any new binary merger candidates. We interpret these results in light of eccentric binary formation models. We rule out formation channels with rates ≳100 Gpc −3 yr −1 for e 0.1, assuming a black hole mass spectrum with a power-law index ≲2.
The most probable host of CHIME FRB 190425A, associated with binary neutron star merger GW190425, and a late-time transient search
Publisher: Oxford University Press (OUP)
Date: 09-12-2022
Abstract: The identification and localization of fast radio bursts (FRBs) to their host galaxies have revealed important details about the progenitors of these mysterious, millisecond-long bursts of coherent radio emission. In this work, we study the most probable host galaxy of the apparently non-repeating CHIME/FRB event FRB 20190425A – a particularly high-luminosity, low-dispersion measure event that was demonstrated in a recent paper to be temporally and spatially coincident with the LIGO-Virgo-KAGRA binary neutron star merger GW190425, suggesting an astrophysical association (p-value 0.0052). In this paper, we remain agnostic to this result, and we confirm UGC10667 as the most probable host galaxy of FRB 20190425A, demonstrating that the host galaxies of low-dispersion measure, one-off CHIME FRBs can be plausibly identified. We then perform multiwavelength observations to characterize the galaxy and search for any afterglow emission associated with the FRB and its putative GW counterpart. We find no radio or optical transient emission in our observations $2.5\\, \\mathrm{yr}$ post-burst. UGC10667 is a spiral galaxy at z ∼ 0.03, dominated by an old stellar population. We find no evidence of a large population of young stars, with nebular emission dominated by star formation at a rate of $1\\!-\\!2\\, ~\\mathrm{M_\\odot \\, yr^{-1}}$. While we cannot rule out a young magnetar as the origin of FRB 20190425A, our observations are consistent with an origin in a long delay-time neutron star binary merger.
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo
Publisher: American Astronomical Society
Date: 11-09-2019
Improved time–frequency analysis of extreme-mass-ratio inspiral signals in mock LISA data
Publisher: IOP Publishing
Date: 02-09-2008
Wide-band profile domain pulsar timing analysis
Publisher: Oxford University Press (OUP)
Date: 24-12-2017
Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3
Publisher: American Physical Society (APS)
Date: 29-03-2023
GW190412: Observation of a binary-black-hole coalescence with asymmetric masses
Publisher: American Physical Society (APS)
Date: 24-08-2020
Summed parallel infinite impulse response filters for low-latency detection of chirping gravitational waves
Publisher: American Physical Society (APS)
Date: 05-07-2012
The basic physics of the binary black hole merger GW150914
Publisher: Wiley
Date: 04-10-2016
Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology
Publisher: American Physical Society (APS)
Date: 26-03-2018
EARLY DETECTION AND LOCALIZATION OF GRAVITATIONAL WAVES FROM COMPACT BINARY COALESCENCES
Publisher: World Scientific Pub Co Pte Lt
Date: 09-2013
DOI: 10.1142/S0218271813600110
Abstract: With the first detection of gravitational waves expected in the next decade, increasing efforts are made toward the electromagnetic follow-up observations of gravitational wave events. In this paper, I discuss the prospect of real-time detection and source localization for gravitational waves from neutron star–neutron star binary or neutron star–black hole binary coalescences before their merger. I show that several low-latency search pipelines are already under intensive development with the aim to provide real-time detections of these events. There will also be fast responding and/or wide-field electromagnetic telescopes available to help catch the electromagnetic or particle flashes possibly occurring during or immediately after their merger. It has been shown that a few coalescence events per year can be detected by advanced LIGO-VIRGO detector network tens of seconds before their merger. However, most of these events will have poor sky direction localization for the existing gravitational-wave detector network, making it extremely challenging for follow up observations by astronomical telescopes aiming at catching events around the merger time. A larger detector network including the planned detectors in Japan and in India will play an important role in improving the angular resolution and making prompt follow up observations much more realistic. A new detector at the Southern Hemisphere AIGO will further contribute significantly to this aspect.
DATA ANALYSIS OF GRAVITATIONAL WAVES USING A NETWORK OF DETECTORS
Publisher: World Scientific Pub Co Pte Lt
Date: 07-2008
DOI: 10.1142/S0218271808012723
Abstract: Several large-scale gravitational wave (GW) interferometers have achieved long term operation at design sensitivity. Questions arise on how to best combine all available data from detectors of different sensitivities for detection, consistency check or veto, localization and waveform extraction. We show that these problems can be formulated using the singular value decomposition (SVD) 1 method. We present techniques based on the SVD method for (1) detection statistic, (2) stable solutions to waveforms, (3) null-stream construction for an arbitrary number of detectors, and (4) source localization for GWs of unknown waveforms.
First upper limits from LIGO on gravitational wave bursts
Publisher: American Physical Society (APS)
Date: 07-05-2004
First Search for Gravitational Waves from Known Pulsars with Advanced LIGO
Publisher: American Astronomical Society
Date: 07-04-2017
Analysis of first LIGO science data for stochastic gravitational waves
Publisher: American Physical Society (APS)
Date: 06-2004
Localizations of 13 Gamma‐Ray Bursts by the All‐Sky Monitor on theRossi X‐Ray Timing Explorer
Publisher: American Astronomical Society
Date: 12-1999
DOI: 10.1086/308029
Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO
Publisher: American Astronomical Society
Date: 28-07-2023
Abstract: The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at gwosc.org . The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages.
Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network
Publisher: Cambridge University Press (CUP)
Date: 2020
DOI: 10.1017/PASA.2020.39
Abstract: Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly rotating remnant neutron stars that emit gravitational waves. These will provide clues to the extremely hot post-merger environment. This signature of nuclear matter in gravitational waves contains most information in the 2–4 kHz frequency band, which is outside of the most sensitive band of current detectors. We present the design concept and science case for a Neutron Star Extreme Matter Observatory (NEMO): a gravitational-wave interferometer optimised to study nuclear physics with merging neutron stars. The concept uses high-circulating laser power, quantum squeezing, and a detector topology specifically designed to achieve the high-frequency sensitivity necessary to probe nuclear matter using gravitational waves. Above 1 kHz, the proposed strain sensitivity is comparable to full third-generation detectors at a fraction of the cost. Such sensitivity changes expected event rates for detection of post-merger remnants from approximately one per few decades with two A+ detectors to a few per year and potentially allow for the first gravitational-wave observations of supernovae, isolated neutron stars, and other exotica.
Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA
Publisher: Springer Science and Business Media LLC
Date: 28-09-2020
DOI: 10.1007/S41114-020-00026-9
Abstract: We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star–black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of $$10^{5}, 10^{6}, 10^{7}\\mathrm {\\ Mpc}^3$$ 10 5 , 10 6 , 10 7 Mpc 3 for binary neutron star, neutron star–black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of $$1^{+12}_{-1}$$ 1 - 1 + 12 ( $$10^{+52}_{-10}$$ 10 - 10 + 52 ) for binary neutron star mergers, of $$0^{+19}_{-0}$$ 0 - 0 + 19 ( $$1^{+91}_{-1}$$ 1 - 1 + 91 ) for neutron star–black hole mergers, and $$17^{+22}_{-11}$$ 17 - 11 + 22 ( $$79^{+89}_{-44}$$ 79 - 44 + 89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.
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.
Impact of Relativistic Fireballs on External Matter: Numerical Models of Cosmological Gamma‐Ray Bursts
Publisher: American Astronomical Society
Date: 20-06-1997
DOI: 10.1086/304185
Limitations in timing precision due to single-pulse shape variability in millisecond pulsars
Publisher: Oxford University Press (OUP)
Date: 21-07-2014
Gravitational Waves and Gravitational-wave Sourcestwo
Publisher: Elsevier BV
Date: 10-2018
Extraction of binary black hole gravitational wave signals from detector data using deep learning
Publisher: American Physical Society (APS)
Date: 16-09-2021
Gravitational-wave Constraints on the Equatorial Ellipticity of Millisecond Pulsars
Publisher: American Astronomical Society
Date: 10-2020
Abstract: We present a search for continuous gravitational waves from five radio pulsars, comprising three recycled pulsars (PSR J0437−4715, PSR J0711−6830, and PSR J0737−3039A) and two young pulsars: the Crab pulsar (J0534+2200) and the Vela pulsar (J0835−4510). We use data from the third observing run of Advanced LIGO and Virgo combined with data from their first and second observing runs. For the first time, we are able to match (for PSR J0437−4715) or surpass (for PSR J0711−6830) the indirect limits on gravitational-wave emission from recycled pulsars inferred from their observed spin-downs, and constrain their equatorial ellipticities to be less than 10 −8 . For each of the five pulsars, we perform targeted searches that assume a tight coupling between the gravitational-wave and electromagnetic signal phase evolution. We also present constraints on PSR J0711−6830, the Crab pulsar, and the Vela pulsar from a search that relaxes this assumption, allowing the gravitational-wave signal to vary from the electromagnetic expectation within a narrow band of frequencies and frequency derivatives.
Effects of waveform model systematics on the interpretation of GW150914
Publisher: IOP Publishing
Date: 12-04-2017
Gravitational wave astronomy: the current status
Publisher: Springer Science and Business Media LLC
Date: 12-2015
Search for gravitational waves from primordial black hole binary coalescences in the galactic halo
Publisher: American Physical Society (APS)
Date: 25-10-2005
Search for gravitational waves from galactic and extra-galactic binary neutron stars
Publisher: American Physical Society (APS)
Date: 25-10-2005
Early Warnings of Binary Neutron Star Coalescence Using the SPIIR Search
Publisher: American Astronomical Society
Date: 03-2022
Abstract: Gravitational waves from binary neutron star mergers can be used as alerts to enable prompt follow-up observations. In particular, capturing prompt electromagnetic and astroparticle emissions from the moment of a binary merger presents unique constraints on the timescale and sky localization for online gravitational-wave detection. Here we present the expected performance of the SPIIR online detection pipeline that is designed for this purpose in the upcoming international LIGO–Virgo’s 4th Science Run (O4). Using simulated Gaussian data for the two LIGO observatories with expected O4 sensitivity, we demonstrate that there is a nonnegligible opportunity to deliver premerger warnings at least 10 s before the final plunge. These alerts are expected to be issued at a nominal rate of one binary neutron star coalescence per year and localized within a median searched area of 300 deg 2 . We envision such detection to be extremely useful for follow-up observatories with a large field of view such as the Murchison Widefield Array radio facility in Western Australia.
Gravitational wave astrophysics, data analysis and multimessenger astronomy
Publisher: Springer Science and Business Media LLC
Date: 12-2015
Analysis of LIGO data for gravitational waves from binary neutron stars
Publisher: American Physical Society (APS)
Date: 02-06-2004
Extracting Information about EMRIs using Time-Frequency Methods
Publisher: AIP
Date: 2006
DOI: 10.1063/1.2405105
Capturing the electromagnetic counterparts of binary neutron star mergers through low-latency gravitational wave triggers
Publisher: Oxford University Press (OUP)
Date: 11-03-2016
DOI: 10.1093/MNRAS/STW576
An ultra-wide bandwidth (704 to 4 032 MHz) receiver for the Parkes radio telescope
Publisher: Cambridge University Press (CUP)
Date: 2020
DOI: 10.1017/PASA.2020.2
Abstract: We describe an ultra-wide-bandwidth, low-frequency receiver recently installed on the Parkes radio telescope. The receiver system provides continuous frequency coverage from 704 to 4032 MHz. For much of the band ( ${\\sim}60\\%$ ), the system temperature is approximately 22 K and the receiver system remains in a linear regime even in the presence of strong mobile phone transmissions. We discuss the scientific and technical aspects of the new receiver, including its astronomical objectives, as well as the feed, receiver, digitiser, and signal processor design. We describe the pipeline routines that form the archive-ready data products and how those data files can be accessed from the archives. The system performance is quantified, including the system noise and linearity, beam shape, antenna efficiency, polarisation calibration, and timing stability.
Searching for gravitational wave memory bursts with the Parkes Pulsar Timing Array
Publisher: Oxford University Press (OUP)
Date: 20-11-2014
THE AIGO PROJECT
Publisher: World Scientific Pub Co Pte Lt
Date: 09-2011
DOI: 10.1142/S0218271811020226
Abstract: The AIGO project is the proposed southern hemisphere advanced large scale gravitational wave detector. With this southern hemisphere detector, the global array of ground based gravitational wave detectors will be substantially improved. Here we summarize the current plans for the AIGO detector.
Model-independent test of the parity symmetry of gravity with gravitational waves
Publisher: Springer Science and Business Media LLC
Date: 07-2020
DOI: 10.1140/EPJC/S10052-020-8211-4
Abstract: Gravitational wave (GW) data can be used to test the parity symmetry of gravity by investigating the difference between left-hand and right-hand circular polarization modes. In this article, we develop a method to decompose the circular polarizations of GWs produced during the inspiralling stage of compact binaries, with the help of stationary phase approximation. The foremost advantage is that this method is simple, clean, independent of GW waveform, and is applicable to the existing detector network. Applying it to the mock data, we test the parity symmetry of gravity by constraining the velocity birefringence of GWs. If a nearly edge-on binary neutron-stars with observed electromagnetic counterparts at 40 Mpc is detected by the second-generation detector network, one could derive the model-independent test on the parity symmetry in gravity: the lower limit of the energy scale of parity violation can be constrained within $$\\mathcal {O}(10^4\\mathrm{eV})$$ O ( 10 4 eV ) .
Model-based Cross-correlation Search for Gravitational Waves from the Low-mass X-Ray Binary Scorpius X-1 in LIGO O3 Data
Publisher: American Astronomical Society
Date: 12-2022
Abstract: We present the results of a model-based search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1 using LIGO detector data from the third observing run of Advanced LIGO and Advanced Virgo. This is a semicoherent search that uses details of the signal model to coherently combine data separated by less than a specified coherence time, which can be adjusted to balance sensitivity with computing cost. The search covered a range of gravitational-wave frequencies from 25 to 1600 Hz, as well as ranges in orbital speed, frequency, and phase determined from observational constraints. No significant detection candidates were found, and upper limits were set as a function of frequency. The most stringent limits, between 100 and 200 Hz, correspond to an litude h 0 of about 10 −25 when marginalized isotropically over the unknown inclination angle of the neutron star’s rotation axis, or less than 4 × 10 −26 assuming the optimal orientation. The sensitivity of this search is now probing litudes predicted by models of torque balance equilibrium. For the usual conservative model assuming accretion at the surface of the neutron star, our isotropically marginalized upper limits are close to the predicted litude from about 70 to 100 Hz the limits assuming that the neutron star spin is aligned with the most likely orbital angular momentum are below the conservative torque balance predictions from 40 to 200 Hz. Assuming a broader range of accretion models, our direct limits on gravitational-wave litude delve into the relevant parameter space over a wide range of frequencies, to 500 Hz or more.
Directional limits on persistent gravitational waves using data from Advanced LIGO’s first two observing runs
Publisher: American Physical Society (APS)
Date: 04-09-2019
Comparison of pulsar positions from timing and very long baseline astrometry
Publisher: Oxford University Press (OUP)
Date: 05-04-2017
DOI: 10.1093/MNRAS/STX837
All-sky search for short gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run
Publisher: American Physical Society (APS)
Date: 23-12-2021
GPU-acceleration on a low-latency binary-coalescence gravitational wave search pipeline
Publisher: Elsevier BV
Date: 10-2018
Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data
Publisher: American Astronomical Society
Date: 26-06-2019
The Science benefits and preliminary design of the southern hemisphere gravitational wave detector AIGO
Publisher: IOP Publishing
Date: 07-2008
Summary of session C1: pulsar timing arrays
Publisher: Springer Science and Business Media LLC
Date: 09-07-2014
Understanding the Long‐Term Spectral Variability of Cygnus X‐1 with Burst and Transient Source Experiment and All‐Sky Monitor Observations
Publisher: American Astronomical Society
Date: 10-10-2002
DOI: 10.1086/342402
Gravitational waves: search results, data analysis and parameter estimation
Publisher: Springer Science and Business Media LLC
Date: 22-01-2015
The International Pulsar Timing Array: First data release
Publisher: Oxford University Press (OUP)
Date: 15-02-2016
DOI: 10.1093/MNRAS/STW347
Search for Gravitational Waves Associated with Fast Radio Bursts Detected by CHIME/FRB during the LIGO–Virgo Observing Run O3a
Publisher: American Astronomical Society
Date: 28-09-2023
The superorbital variability and triple nature of the X-ray source 4U 1820-303
Publisher: Oxford University Press (OUP)
Date: 21-05-2007
Search for Subsolar Mass Ultracompact Binaries in Advanced LIGO’s Second Observing Run
Publisher: American Physical Society (APS)
Date: 18-10-2019
Setting upper limits on the strength of periodic gravitational waves from PSRJ 1<
Publisher: American Physical Society (APS)
Date: 30-04-2004
Semianalytical approach for sky localization of gravitational waves
Publisher: American Physical Society (APS)
Date: 03-11-2021
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
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
Constraints on the Cosmic Expansion History from GWTC–3
Publisher: American Astronomical Society
Date: 06-2023
Abstract: We use 47 gravitational wave sources from the Third LIGO–Virgo–Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC–3) to estimate the Hubble parameter H ( z ), including its current value, the Hubble constant H 0 . Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H ( z ). The source mass distribution displays a peak around 34 M ⊙ , followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H ( z ) measurement, yielding H 0 = 68 − 8 + 12 km s − 1 Mpc − 1 (68% credible interval) when combined with the H 0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H 0 estimate from GWTC–1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+ , statistically marginalizing over the redshifts of each event’s potential hosts. Assuming a fixed BBH population, we estimate a value of H 0 = 68 − 6 + 8 km s − 1 Mpc − 1 with the galaxy catalog method, an improvement of 42% with respect to our GWTC–1 result and 20% with respect to recent H 0 studies using GWTC–2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution the only event which is not strongly impacted by such assumptions (and is thus informative about H 0 ) is the well-localized event GW190814.
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.
Search for gravitational waves associated with the gamma ray burst GRB030329 using the LIGO detectors
Publisher: American Physical Society (APS)
Date: 12-08-2005
The next detectors for gravitational wave astronomy
Publisher: Springer Science and Business Media LLC
Date: 12-2015
Constraining the Properties of Supermassive Black Hole Systems Using Pulsar Timing: Application to 3C 66B
Publisher: American Astronomical Society
Date: 10-05-2004
DOI: 10.1086/383020
Search for gravitational waves from Scorpius X-1 with a hidden Markov model in O3 LIGO data
Publisher: American Physical Society (APS)
Date: 21-09-2022
A study of multifrequency polarization pulse profiles of millisecond pulsars
Publisher: Oxford University Press (OUP)
Date: 29-08-2015
DOI: 10.1093/MNRAS/STV508
Progress on the Low-Latency Inspiral Gravitational Wave Detection algorithm known as SPIIR
Publisher: IOP Publishing
Date: 06-2012
Scientific Benefit of Enlarging Gravitational Wave Detector Networks
Publisher: IOP Publishing
Date: 06-2012
Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A
Publisher: American Astronomical Society
Date: 16-10-2017
Gravitational waves from binary supermassive black holes missing in pulsar observations
Publisher: American Association for the Advancement of Science (AAAS)
Date: 25-09-2015
Abstract: Gravitational waves are expected to be generated by the interaction of the massive bodies in black-hole binary systems. As gravitational waves distort spacetime, it should be possible to verify their existence as they interfere with the pulses emitted by millisecond pulsars. However, after monitoring 24 pulsars with the Parkes radio telescope for 12 years, Shannon et al. found no detectable variation in pulsar records. This nondetection result indicates that a new detection strategy for gravitational waves is needed. Science , this issue p. 1522
GPU accelerated low latency gravitational wave data processing
Publisher: Science China Press., Co. Ltd.
Date: 2017
Gravitational wave astronomy
Publisher: Springer Science and Business Media LLC
Date: 25-05-2013
Detector description and performance for the first coincidence observations between LIGO and GEO
Publisher: Elsevier BV
Date: 2004
Detecting extreme mass ratio inspirals with LISA using time–frequency methods
Publisher: IOP Publishing
Date: 28-04-2005
Photons with sub-Planckian energy cannot efficiently probe space-time foam
Publisher: American Physical Society (APS)
Date: 24-09-2014
First all-sky upper limits from LIGO on the strength of periodic gravitational waves using the Hough transform
Publisher: American Physical Society (APS)
Date: 28-11-2005
The development of ground based gravitational wave astronomy and opportunities for Australia-China collaboration
Publisher: World Scientific Pub Co Pte Lt
Date: 20-10-2015
DOI: 10.1142/S0217751X15450190
Abstract: This paper begins by reviewing the development of gravitational wave astronomy from the first predictions of gravitational waves to development of technologies across the entire gravitational wave spectrum, and then focuses on the current status of ground based gravitational wave detectors. With substantial improvements already demonstrated in early commissioning it is emphasised that Advanced detectors are on track for first detection of gravitational waves. The importance of a worldwide array of detectors is emphasised, and recent results are shown that demonstrate the continued advantage of a southern hemisphere detector. Finally it is shown that a north–south pair of 8 km arm length detectors would give rise to a dramatic improvement in event rate, enabling a pair of detectors to encompass a 64-times larger volume of the universe, to conduct a census on all stellar mass black hole mergers to [Formula: see text] and to observe neutron star mergers to a distance of [Formula: see text][Formula: see text]800 Mpc.
The Data Analysis in Gravitational Wave Detection
Publisher: Elsevier BV
Date: 2017
Upper limits on gravitational wave bursts in LIGO’s second science run
Publisher: American Physical Society (APS)
Date: 08-09-2005
Towards low-latency real-time detection of gravitational waves from compact binary coalescences in the era of advanced detectors
Publisher: American Physical Society (APS)
Date: 14-05-2012
The superorbital variability and triple nature of the X-ray source 4U 1820–303
Publisher: AIP
Date: 2008
DOI: 10.1063/1.2840406
The GEO-HF project
Publisher: IOP Publishing
Date: 29-03-2006
A Systematic Search for Periodicities inRXTEASM Data
Publisher: American Astronomical Society
Date: 04-2006
DOI: 10.1086/500648
Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO-Virgo data
Publisher: American Physical Society (APS)
Date: 09-08-2022
The Correlated Intensity and Spectral Evolution of Cygnus X-1 During State Transitions
Publisher: American Astronomical Society
Date: 10-01-2001
DOI: 10.1086/318862
Low-Latency Detection of Gravitational Waves
Publisher: AIP
Date: 2010
DOI: 10.1063/1.3460207
Accelerated Searches of Gravitational Waves Using Graphics Processing Units
Publisher: AIP
Date: 2010
DOI: 10.1063/1.3460206
A Shock‐patching Code for Ultrarelativistic Fluid Flows
Publisher: American Astronomical Society
Date: 10-09-1997
DOI: 10.1086/304547
GPU-Optimised Low-Latency Online Search for Gravitational Waves from Binary Coalescences
Publisher: IEEE
Date: 09-2018
Coherent network detection of gravitational waves: the redundancy veto
Publisher: IOP Publishing
Date: 06-09-2005
First Demonstration of Early Warning Gravitational-wave Alerts
Publisher: American Astronomical Society
Date: 04-2021
Abstract: Gravitational-wave observations became commonplace in Advanced LIGO-Virgo’s recently concluded third observing run. 56 nonretracted candidates were identified and publicly announced in near real time. Gravitational waves from binary neutron star mergers, however, remain of special interest since they can be precursors to high-energy astrophysical phenomena like γ -ray bursts and kilonovae. While late-time electromagnetic emissions provide important information about the astrophysical processes within, the prompt emission along with gravitational waves uniquely reveals the extreme matter and gravity during—and in the seconds following—merger. Rapid communication of source location and properties from the gravitational-wave data is crucial to facilitate multimessenger follow-up of such sources. This is especially enabled if the partner facilities are forewarned via an early warning (pre-merger) alert. Here we describe the commissioning and performance of such a low-latency infrastructure within LIGO-Virgo. We present results from an end-to-end mock data challenge that detects binary neutron star mergers and alerts partner facilities before merger. We set expectations for these alerts in future observing runs.
Detecting extreme mass ratio inspirals with LISA using time–frequency methods: II. Search characterization
Publisher: IOP Publishing
Date: 06-09-2005
Network analysis and multi-messenger astronomy
Publisher: Cambridge University Press
Date: 16-02-2012
BENEFIT OF A LARGER DETECTOR ARRAY FOR PROMPT GRAVITATIONAL WAVE DETECTION
Publisher: WORLD SCIENTIFIC
Date: 29-01-2015
Timing analysis for 20 millisecond pulsars in the Parkes Pulsar Timing Array
Publisher: Oxford University Press (OUP)
Date: 18-11-2015
SPIIR online coherent pipeline to search for gravitational waves from compact binary coalescences
Publisher: American Physical Society (APS)
Date: 06-01-2022
All-sky search for continuous gravitational waves from isolated neutron stars using Advanced LIGO and Advanced Virgo O3 data
Publisher: American Physical Society (APS)
Date: 28-11-2022
Using negative-latency gravitational wave alerts to detect prompt radio bursts from binary neutron star mergers with the Murchison Widefield Array
Publisher: Oxford University Press (OUP)
Date: 21-08-2019
Abstract: We examine how fast radio burst (FRB)-like signals predicted to be generated during the merger of a binary neutron star (BNS) may be detected in low-frequency radio observations triggered by the aLIGO/Virgo gravitational-wave detectors. The rapidity, directional accuracy, and sensitivity of follow-up observations with the Murchison Widefield Array (MWA) are considered. We show that with current methodology, the rapidity criterion fails for triggered MWA observations above 136 MHz for BNS mergers within the aLIGO/Virgo horizon, for which little dispersive delay is expected. A calculation of the expected reduction in response time by triggering on ‘negative latency’ alerts from aLIGO/Virgo observations of gravitational waves generated by the BNS inspiral is presented. This allows for observations up to 300 MHz where the radio signal is expected to be stronger. To compensate for the poor positional accuracy expected from these alerts, we propose a new MWA observational mode that is capable of viewing one-quarter of the sky. We show the sensitivity of this mode is sufficient to detect an FRB-like burst from an event similar to GW 170817 if it occurred during the ongoing aLIGO/Virgo third science run (O3).
GW190521: A Binary Black Hole Merger with a Total Mass of
150 <
Publisher: American Physical Society (APS)
Date: 02-09-2020
Upper limits on the strength of periodic gravitational waves from PSR J1939+2134
Publisher: IOP Publishing
Date: 09-02-2004
All-sky search for short gravitational-wave bursts in the second Advanced LIGO and Advanced Virgo run
Publisher: American Physical Society (APS)
Date: 11-07-2019
Search for gravitational waves from binary black hole inspirals in LIGO data
Publisher: American Physical Society (APS)
Date: 07-03-2006
Fast response electromagnetic follow-ups from low latency GW triggers
Publisher: IOP Publishing
Date: 05-2016
Report on the second Mock LISA data challenge
Publisher: IOP Publishing
Date: 15-05-2008
GPU-accelerated low-latency real-time searches for gravitational waves from compact binary coalescence
Publisher: IOP Publishing
Date: 02-11-2012
PULSAR OBSERVATIONS OF EXTREME SCATTERING EVENTS
Publisher: American Astronomical Society
Date: 27-07-2015
Search for Subsolar-Mass Binaries in the First Half of Advanced LIGO’s and Advanced Virgo’s Third Observing Run
Publisher: American Physical Society (APS)
Date: 05-08-2022
Status of the GEO600 detector
Publisher: IOP Publishing
Date: 24-03-2006
Versatile directional searches for gravitational waves with Pulsar Timing Arrays
Publisher: Oxford University Press (OUP)
Date: 12-2015
Synthesis of yttria nanopowders for transparent yttria ceramics
Publisher: Elsevier BV
Date: 11-2006
THE LIGO GRAVITATIONAL WAVE OBSERVATORIES: RECENT RESULTS AND FUTURE PLANS
Publisher: World Scientific Publishing Company
Date: 02-2006
Using deep learning to localize gravitational wave sources
Publisher: American Physical Society (APS)
Date: 26-11-2019
THE DISTURBANCE OF A MILLISECOND PULSAR MAGNETOSPHERE
Publisher: American Astronomical Society
Date: 22-08-2016
Gravitational-Wave Cosmology across 29 Decades in Frequency
Publisher: American Physical Society (APS)
Date: 31-03-2016
Application of graphics processing units to search pipelines for gravitational waves from coalescing binaries of compact objects
Publisher: IOP Publishing
Date: 14-05-2010
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Massachusetts Institute Of Technology
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