Bulletin of the American Physical Society
APS April Meeting 2021
Volume 66, Number 5
Saturday–Tuesday, April 17–20, 2021; Virtual; Time Zone: Central Daylight Time, USA
Session Z16: Gravitational Wave Data Analysis Methods IIILive
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Sponsoring Units: DGRAV Chair: Benjamin Owen, Texas Tech University |
Tuesday, April 20, 2021 3:45PM - 3:57PM Live |
Z16.00001: Galactic white dwarf binary population from LISA Data Challenge Radler data set Kristen Lackeos, Tyson Littenberg, Neil Cornish, James Thorpe Here we present an analysis of a simulated Laser Interferometer Space Antenna data stream from one year's worth of observing time. The data stream is comprised entirely of white dwarf galactic binaries, generated as part of the LISA Data Challenges ${\it Radler}$ data set. We use the end-to-end analysis pipeline presented in Littenberg et al. 2020 to resolve thousands of galactic binaries and characterize the residual of the unresolved galactic foreground. The analysis is done successively for segments of one, 3, 6 and finally 12 months of observing time. Each analysis builds on the proposal distributions constructed from a catalog of resolved binaries produced from analysis results immediately preceding. The catalog for each observation time is presented along with quantification of the detection efficacy of the pipeline and the robustness of parameter estimation over time. We discuss and compare our results to those inferred from galactic binary population statistics extracted from the same ${\it Radler}$ data set and statistics found in the literature. [Preview Abstract] |
Tuesday, April 20, 2021 3:57PM - 4:09PM Live |
Z16.00002: Exploring the impact of higher-order modes on inferring source properties from gravitational-wave observations Jennifer Sanchez, Alan J. Weinstein, Colm Talbot Advanced LIGO and Advanced Virgo have confidently detected a number of gravitational wave signals, including waves from dozens of binary black hole mergers and two mergers of binary neutron stars. Each observation contains encoded information about the physical properties of the binary system. As gravitational-wave detectors continue to improve their sensitivity and thus their astronomical reach, the improvements will allow us to detect rarer systems and make more confident statements regarding their source properties. In order to fully characterize the gravitational wave observations, we rely on numerical and analytical models that approximate the signal waveforms from the emitted source as specified by the source parameters (e.g. masses, spins, sky location, etc). The dominant emission frequency of gravitational waves from compact binary coalescence is at twice the orbital frequency; however, recently published events (e.g. GW190412) have demonstrated evidence of subdominant, higher-order harmonic contributions. In this talk, I will discuss a study exploring the impact of including (using newly improved signal models) or neglecting these higher-order modes in gravitational wave signals on the signals' sources' inferred physical properties. [Preview Abstract] |
Tuesday, April 20, 2021 4:09PM - 4:21PM Live |
Z16.00003: Maximum likelihood methods for detecting the stochastic gravitational wave background and its anisotropies Arianna Renzini Current gravitational-wave detectors are only able to resolve a tiny fraction of all gravitational-wave signals in the Universe; the collection of unresolved signals is referred to as the gravitational-wave background and is expected to be a stochastic signal, hard to distinguish from detector noise. In this talk, I will present maximum likelihood estimators for this background and its anisotropies on the sky, tailored to different observatories such as LIGO and LISA. I will showcase the importance of having a network of multiple detectors for background characterisation, in particular in the case of anisotropic backgrounds. Finally, I will present mock-data tests for LISA, detailing the expected sensitivity and sky resolution. [Preview Abstract] |
Tuesday, April 20, 2021 4:21PM - 4:33PM Live |
Z16.00004: A Bayesian Statistical Framework for Identifying Strongly Lensed Gravitational-Wave Signals Rico Ka Lok Lo, Ignacio MagaƱa Hernandez It is expected that gravitational waves, similar to electromagnetic waves, can be gravitationally lensed by intervening matters, producing multiple instances of the same signal arriving at different times and apparent luminosity distances with different phase shifts compared to the un-lensed signal due to lensing. If unaccounted for, these lensed signals will masquerade as separate systems with higher mass and lower redshift. In this talk, we present a Bayesian statistical framework to identify strongly-lensed gravitational-wave signals that incorporates source population information and accounts for selection effect. If confirmed, lensed gravitational waves will allow us to probe the Universe at higher redshift, and to constrain the polarization contents of the waves with fewer number of detectors. [Preview Abstract] |
Tuesday, April 20, 2021 4:33PM - 4:45PM Live |
Z16.00005: Fast Parameter Estimation of Binary Mergers for Multimessenger Follow-up Daniel Finstad, Duncan Brown Significant observational resources have been dedicated to electromagnetic follow-up of gravitational-wave events detected by Advanced LIGO and Virgo. As the sensitivity of LIGO and Virgo improves, the rate of sources detected will increase. Margalit & Metzger (2019) have suggested that it may be necessary to prioritize observations of future events. Optimal prioritization requires a rapid measurement of a gravitational-wave event's masses and spins, as these can determine the nature of any electromagnetic emission. We extend the relative binning method of Cornish (2013) and Zackay et al. (2018) to a coherent detector-network statistic. We show that the method can be seeded from a matched-filter search and used in a Bayesian parameter measurement framework to produce marginalized posterior probability densities for the source's parameters within 20 minutes of detection on 32 CPU cores. We demonstrate that this algorithm produces unbiased estimates of the parameters with the same accuracy as running parameter estimation using the standard gravitational-wave likelihood. We encourage the adoption of this method in future LIGO--Virgo observing runs to allow fast dissemination of the parameters of detected events so that the observing community can make best use of its resources. [Preview Abstract] |
Tuesday, April 20, 2021 4:45PM - 4:57PM Live |
Z16.00006: The Method for Targeted Search for Long-duration Transients From Glitching Pulsars Liudmila Fesik, Maria Alessandra Papa We propose a method for identifying continuous waves (CWs) from spinning neutron stars. We focus on glitching pulsars with abrupt spin-ups and long term spin-down, which imprint in CWs as long-duration transients from weeks to months. The main principle of the method is the combination of a coherent detection statistics over time intervals of different duration. We characterize the method by determining the false alarm and false dismissal probabilities for different signal strengths, and appropriate choices of the relative detection thresholds. We compare the sensitivity of this method with the standart match-filtering. [Preview Abstract] |
Tuesday, April 20, 2021 4:57PM - 5:09PM Live |
Z16.00007: Prospects for Reconstructing the Gravitational Wave Signal from Core-Collapse Supernovae in the Advanced Detector Era Nayyer Raza, Jess McIver Our current understanding of the core-collapse supernova explosion mechanism is incomplete, with multiple viable models for how the initial shock wave might be energized enough to lead to a successful explosion. Detection of a gravitational wave (GW) signal emitted in the initial few seconds after core-collapse would provide unique and crucial insight into this process. With the Advanced LIGO and Advanced Virgo gravitational wave detectors expected to soon approach their design sensitivity, we could potentially detect this GW emission from most core-collapse supernovae within our galaxy. But once identified, how well can we recover the signal from these detectors? Here we use the BayesWave algorithm to maximize our ability to accurately recover GW signals from core-collapse supernovae. Using the expected design sensitivity noise curves of the advanced global detector network, we inject and recover supernova waveforms modeled with different explosion mechanisms into simulated noise, tuning the algorithm to extract as much of the signal as possible. We report the preliminary results of this work, including how the reconstruction is affected by the model and what we can hope to learn from the next galactic supernova. [Preview Abstract] |
Tuesday, April 20, 2021 5:09PM - 5:21PM On Demand |
Z16.00008: Surrogate Model for Gravitational Wave Signals From Large-mass-ratio Black Hole Binaries With Aligned Spin Nur Rifat, Gaurav Khanna, Scott Field Gravitational wave signals from compact astrophysical sources such as those observed by LIGO and Virgo require a high-accuracy waveform model for the analysis of the recorded signal. Current inspiral-merger-ringdown (IMR) models are calibrated only up to moderate mass ratios, thereby limiting their applicability to signals from high-mass ratio binary systems. In recent work, we described a reduced-order surrogate model for gravitational waveforms including several harmonic modes and with mass-ratios up to 10,000. This surrogate model was trained on waveform data generated by point-particle black hole perturbation theory. In this talk, we present extensions of this model to include spin on the primary black hole up to 0.8. To handle the increased dimensionality of the parameter space and hard-to-model features in the ringdown signal we have pursued methodological improvements including Gaussian process regression fits, a parametric domain decomposition strategy, and modifications to the reduced-order modeling step. We find that the resulting surrogate model is nearly as accurate as the underlying training data. We also discuss comparisons to numerical relativity in the comparable mass ratio limit. [Preview Abstract] |
Tuesday, April 20, 2021 5:21PM - 5:33PM Live |
Z16.00009: From Scattering in Quantum Field Theory to Gravitational Waves in Kerr Alfredo Guevara Recently a remarkable map between classical black holes and gravitational scattering amplitudes in QFT has been proposed in the Post-Minkowskian framework of GR. Here we extend it by studying low-frequency scattering of massless waves in a Kerr background. The classical amplitudes obtained from the Teukolsky formalism are found to coincide with four-point amplitudes in QFT provided 1) a precise classical limit is implemented on the QFT side, 2) the black hole is modelled as an interacting massive particle with large spin S, 3) the wave is modelled by a massless particle of helicity $h\leq 2$. For $h$=2 we bootstrap the general form of QFT amplitudes for spin-S particles coupled to gravitons (representing Gravitational Waves). Using the new massive spinor-helicity technique we obtain the partial wave amplitudes and check unitarity of the process. Then, matching to the classical Teukolsky analysis reveals that the corresponding QFT amplitudes are fixed by a novel notion of minimal-coupling, i.e. by imposing a suitable high-energy behaviour. These GW amplitudes exponentiate in the spin parameter, reminiscent of the classical Newman-Janis construction. We use this to derive new results for binary BH emission of GWs. Previous classical results in the eikonal limit are recovered. [Preview Abstract] |
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