Bulletin of the American Physical Society
APS April Meeting 2023
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session SS04: V: Gravitational Waves |
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Sponsoring Units: DGRAV Chair: Jolien Creighton, University of Wisconsin - Milwaukee Room: Virtual Room 4 |
Tuesday, April 25, 2023 2:30PM - 2:42PM |
SS04.00001: Cross-correlation analysis of data from a network of gravitational-wave detectors. Sergey G Klimenko Model-independent detection of a transient gravitational wave (GW) signal requires time-frequency (TF) data analysis from multiple GW detectors. Usually, the signal is identified with the excess-power statistic extracting the TF data amplitudes above the fluctuations of the detector noise. Such a detection approach is affected by the temporal |
Tuesday, April 25, 2023 2:42PM - 2:54PM |
SS04.00002: Preparing for the fourth observing run of advanced LIGO-Virgo: Search for binary black hole mergers with the updated Coherent WaveBurst pipeline Tanmaya Mishra, Marek Szczepanczyk, Sergey G Klimenko The advanced LIGO-Virgo detectors have discovered gravitational wave (GW) signals from over 90 binary black hole mergers (BBH). With improved sensitivities of the advanced LIGO-Virgo detectors in the upcoming LIGO-Virgo-KAGRA (LVK) fourth observing run (O4), many more GW events are expected to be detected. In particular, we are interested in detecting exceptional high-mass BBH mergers, similar to the GW190521 event discovered in 2021 that provided the first direct evidence of an intermediate-mass black hole (IMBH). Since the signals from unprecedented events may not be well-modeled, template-independent search methods like the Coherent WaveBurst (cWB) are used in LVK data analysis. cWB can identify generic GW signals in the LIGO-Virgo data with minimal assumptions on the signal model. The cWB algorithm looks for excess power events in the time-frequency domain and uses a machine learning (ML) method to enhance the signal-noise classification of the identified events. For the O4 run, the cWB search was upgraded with a new time-frequency transform called wavescan that provides high-resolution time-frequency distributions for efficient recovery of transient GW signals. The upgraded cWB search allows for precise estimation of the signal properties, consequently improving the sensitivity of the ML-enhanced cWB search to BBH mergers. This study discusses the results of the proposed O4 cWB search on LIGO-Virgo data from the third LVK observing run (O3). We report GW detections with higher significance and demonstrate improvement in the detection efficiency by approximately 40% for simulated BBH events at a false alarm rate of less than one per year. |
Tuesday, April 25, 2023 2:54PM - 3:06PM |
SS04.00003: An Optically Targeted Search for Gravitational Waves emitted by Core-Collapse Supernovae during the Third Observing Run of LIGO and Virgo Marek Szczepanczyk Core-collapse supernovae (CCSNe) are violent explosions of massive stars and multimessenger astrophysical sources. Detecting gravitational waves (GWs) from these sources will allow direct probing of the engine driving explosion's dynamics. So far, no GWs from these explosions have been observed. The recent optically targeted search with the data from the first and second observing runs of LIGO and Virgo constrained the CCSN engine for the first time. In my talk, I will present the search results with the data from the third observing run of LIGO and Virgo, where we analyzed CCSN up to 30 Mpc. I will briefly describe the method and the GW candidates. In our analysis, we continue constraining the properties of the CCSN engine. I will report the upper limits on GW emission energy and power. I will provide an interpretation in terms of the core deformation. Finally, I will present the probabilities of excluding the extreme emission models. |
Tuesday, April 25, 2023 3:06PM - 3:18PM |
SS04.00004: Probing fundamental physics with multiband and multimessenger observations of compact binaries with fast-radio-burst emitters Kent Yagi, Zhen Pan, Huan Yang Recent observations indicate that magnetars, strong candidates for at least a part of fast radio bursts (FRBs), commonly reside in merging compact binaries. If an FRB-emitting neutron star is in a binary with another neutron star, one can probe the early part of the inspiral with radio observations while the late part of the same binary can be studied through gravitational-wave observations (thus multiband and multimessenger observations of binary neutron stars). Based on several mock observations of FRB pulsars, we find that physical quantities of neutron stars, like quadrupole moment, can be measured with an error of ~10% through radio observations. Combined with gravitational-wave observations, one can probe fundamental physics, including nuclear and gravitational physics. For example, the effect of gravitational parity violation can be probed much more accurately than existing observations/experiments through universal relations between the quadrupole moment and tidal deformability that do not depend sensitively on the equations of state. |
Tuesday, April 25, 2023 3:18PM - 3:30PM |
SS04.00005: Bayesian Time Delay Interferometry for Orbiting LISA Jessica Page Previous work demonstrated effective laser frequency noise (LFN) suppression for LISA data from raw phasemeter measurements using a Markov Chain Monte Carlo (MCMC) algorithm with fractional delay interpolation (FDI) techniques to estimate the spacecraft separation parameters required for time-delay interferometry (TDI) under the assumption of a rigidly rotating LISA configuration. Including TDI parameters in the LISA data model as part of a global fit analysis pipeline produces gravitational wave inferences that are marginalized over uncertainty in the spacecraft separations. Here we extend the algorithm's capability to perform data-driven TDI on LISA in orbit which introduces a time-dependence in the arm-length parameters and at least O(L) times greater computational cost since the filter must be applied for every sample in the time series of size L. We find feasibility of arm-length estimation on ~ day-long time scales by using a restructured time-varying FDI LaGrange filter that allows half of the filter computation to be constant for all proposed parameters in the MCMC and requires shorter filter lengths than previously reported. We demonstrate LFN suppression for orbiting LISA using accurate arm-length estimates parameterized by Keplerian orbital parameters under the assumption of unperturbed analytical Keplerian orbits, and explore the potential extension of these methods to arbitrary numerical orbits. |
Tuesday, April 25, 2023 3:30PM - 3:42PM |
SS04.00006: Detecting and Mitigating Instrumental Glitches in LISA Data Orion E Sauter, Peter J Wass, Henri Inchauspé, Wiler A Sanchez The space-based gravitational wave observatory LISA has been designed to sense waves at millihertz frequencies coming from galactic binaries and extreme mass-ratio inspirals, among other sources. A technology-demonstration mission, LISA Pathfinder, was launched in 2015 and observed several unexpected changes in test mass acceleration, or "glitches." Due to the small amplitude of gravitational waves, extreme stability of the test masses is needed, so it is important to assess how similar glitches on LISA will affect our measurements. Time Delay Interferometry (TDI) is the primary data product of the observatory which combines interferometric signals on-board and between the three spacecraft to maximize sensitivity to gravitational waves. We present simulations of the detector's TDI response to similar glitches, and propose a method for detecting and removing the effects from TDI data. As a test case, we apply the technique to the LISA Data Challenge, a simulated dataset containing glitches. |
Tuesday, April 25, 2023 3:42PM - 3:54PM |
SS04.00007: Determining the individual masses of accreting white dwarf binaries Sophia Yi, Kent Yagi, Phil Arras, Shu Yan Lau Accreting binary white dwarf systems are among the sources expected to emanate gravitational waves that will be detectable by LISA. We attempt to ascertain whether the individual masses of such a binary can be determined from LISA's measurements of the frequency and frequency time derivative of gravitational waves emanated by the binary. We present analytic expressions for the gravitational wave frequency and its derivative in terms of the individual masses, which we derive using prior knowledge of mass accreting mechanisms for low-mass helium core white dwarfs. We then perform a Fisher analysis to reveal the accuracy with which we expect to be able to constrain the individual masses given LISA's measurements. |
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