Bulletin of the American Physical Society
APS April Meeting 2022
Volume 67, Number 6
Saturday–Tuesday, April 9–12, 2022; New York
Session D17: Gravitational Wave SearchesRecordings Available
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Sponsoring Units: DGRAV DAP Chair: M. Alessandra Papa, Max Planck Inst Room: Sky Lobby |
Saturday, April 9, 2022 1:30PM - 1:42PM |
D17.00001: The International Pulsar Timing Array second data release: search for an isotropic gravitational wave background Paul T Baker We report on the search for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array (IPTA), a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. We find strong evidence for a spectrally-similar, low-frequency, stochastic process with amplitude A = 3.8+6.3-2.5 × 10-15 at f = 1/yr and spectral index α = -0.5 ± 0.5, where uncertainies represent 95% credible intervals. When assuming a spectral index of α = -2/3, as expected from a population of inspiralling supermassive black hole binaries, the recovered amplitude is A = 2.8+1.2-0.8 × 10-15. No significant evidence was found for the Hellings-Downs correlations which would indicate a gravitational wave origin. This combined data set, which was built from older data, produces results in agreement with more recent individual data sets from the NANOGrav, PPTA, and EPTA collaborations. This shows that future IPTA data releases can deliver increased sensitivity to gravitational waves relative to their constituent parts. |
Saturday, April 9, 2022 1:42PM - 1:54PM |
D17.00002: Search for gravitational waves associated with Fast Radio Bursts Detected by CHIME/FRB During the LIGO-Virgo Observing Run O3a. Ryan P Fisher, Eric Howell, Iara Tosta e Melo, Kara Merfeld, Michael A Patel We present the search for gravitational waves associated with fast radio bursts detected by the CHIME/FRB experiment during the LIGO-Virgo Observing Run O3a, from 1 April 2019 15:00 UTC - 1 October 2019 15:00 UTC. Targeted searches for GW events using both modelled compact-binary-coalescence and unmodelled searches were used. We will present results for the exclusion distances generated by the searches in comparison to the fast radio burst events' luminosity distances as well as upper limits on the total amount of energy released in gravitational waves for these events. |
Saturday, April 9, 2022 1:54PM - 2:06PM |
D17.00003: An All-Sky Search for Continuous Gravitational Waves in the LIGO O3a Data Set Aashish Tripathee, Keith Riles The LIGO-Virgo O3 data set offers not only detection of now-familiar compact binary mergers of distant black holes and neutron stars, but potentially the detection of much weaker but continuous radiation from nearby rapidly spinning, non-axisymmetric neutron stars in the galaxy. All-sky searches for such radiation from previously unknown stars using necessarily long data sets (many months) are computationally challenging and have given rise to several different approaches. We describe here the application of the well established PowerFlux program, including the method of loose coherence in its outlier followup, to an all-sky search in the first six months of LIGO data from the O3 observing run. The details of the search and its results will be presented. |
Saturday, April 9, 2022 2:06PM - 2:18PM |
D17.00004: A Semi-Coherent Search for Continuous Waves on Cas A and Vela Jr in the O3a Data Set Jonathan Z Wang The LIGO-Virgo Collaboration (LVC) looks for gravitational waves originating from a broad spectrum of celestial sources. Included among these sources are rapidly spinning neutron stars exhibiting non-axisymmetric deformation, which produce long-lived, well-defined, and roughly monochromatic gravitational waves, or continuous waves. Various search methods are used by the LVC when looking for continuous waves based on what prior information is known about the source. Here we present the results of a Weave implementation of a semi-coherent templated search method using the F-statistic to look for continuous waves in data from the O3a run. |
Saturday, April 9, 2022 2:18PM - 2:30PM |
D17.00005: Continuous gravitational waves from supernova remnants Benjamin J Owen, Lee A Lindblom, Luciano Pinheiro I summarize the results of the Texas Tech group's recent searches of publicly available Advanced LIGO data for continuous gravitational waves from non-pulsing neutron stars in supernova remnants. |
Saturday, April 9, 2022 2:30PM - 2:42PM |
D17.00006: Gravitational Wave Candidate Identification in GWTC-3 Becca Ewing GWTC-3 is the latest version of the LIGO, Virgo, Kagra Collaboration's Gravitational Wave Transient Catalog, comprising compact binary coalescence gravitational wave candidates from the first three observing runs. This latest iteration of the catalog adds 35 candidate gravitational waves from the second part of the third observing run (O3b), bringing the cumulative total to 90 candidates. There are 17 new candidates which were not previously reported as low-latency alerts during O3b. All of the candidates added to the catalog are consistent with either binary black hole coalescences or neutron-star black hole coalescences. Each of these events pass a threshold on the probability of astrophysical origin, p(astro) > 0.50. We additionally publish a list of 7 marginal candidates which fail to meet the p(astro) threshold but pass a false alarm rate (FAR) threshold 2 per year. A bulk data release further includes a deep subthreshold list of triggers which fail to meet the previous two thresholds but have FAR 2 per day. These candidates come from an offline re-analysis of the O3b detector data by four independent search pipelines: cWB, GstLAL, MBTA and PyCBC. We discuss the search methods used in this work as well as an overview of the candidate events found. |
Saturday, April 9, 2022 2:42PM - 2:54PM |
D17.00007: Reassessment of GW170817 and GW190425 using higher order mode models Jacob A Lange, Richard W O'Shaughnessy, Kevin Barkett, Vijay Varma, Scott E Field On August 17, 2017 and April 25, 2019, the LIGO-Virgo Collaboration (LVC) detected its first and second significant binary neutron star systems (BNS) via gravitational wave radiation. The subsequent event and catalog papers used state-of-the-art semi-analytical tidal models that included only the dominant (2,2) mode to estimate the parameters of these systems. Since then, more novel models have been developed to include subdominant modes in their waveform. In this talk, I present the final results of our reanalysis of these two events using two of these models: a hybrid NR surrogate that includes tidal terms (NRHybSur3dq8Tidal) and a newer version of the effective-one-body model for non-precessing and tidal interacting compact binaries (TEOBResumS v2). Similar to previous work on GW170817, I present a mass ejecta calculation and equation of state rankings based off the reanalysis of these two higher order mode models. |
Saturday, April 9, 2022 2:54PM - 3:06PM |
D17.00008: Looking for spin precession and nutation in the gravitational-wave events Daria D Gangardt, Davide Gerosa, Michael Kesden, Nathan A Steinle Spin precession is the phenomena of a binary black hole (BBH) where the angle of the orbital plane tilts due to the entanglement of the orbiting objects' individual spins and the binary's angular momentum. Spin precession modulates the gravitational wave (GW) strain emitted by the binary. Being able to characterise spin precession in BBHs can be used to differentiate between formation channels or reveal insights about the different spin dynamics of a system as it inspirals. We investigate the current catalog of GW events by reformulating the publicly available parameter estimation prior and posteriors into distributions of five new phenomenological parameters. Unlike other parametrisations of spin precession, our parameters split the motion of the orbital angular momentum into its precession and nutation. We condition our priors on well-constrained parameters to establish dependencies and identify notable events. We find that events with high signal to noise ratios, low mass ratios and non-zero values of the effective spin parameter $\chi_{\rm eff}$ have precessional amplitudes constrained away from $0$. We find no evidence of nutation across the catalog, but expect this result to change as GW detectors become more sensitive. |
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