Bulletin of the American Physical Society
APS April Meeting 2022
Volume 67, Number 6
Saturday–Tuesday, April 9–12, 2022; New York
Session L16: Advances in Gravitational Waveform ModelingRecordings Available
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Sponsoring Units: DGRAV Chair: Raul Kashyap, Pennsylvania State University Room: Sky Lobby |
Sunday, April 10, 2022 3:45PM - 3:57PM |
L16.00001: \title{Building Surrogate Model for Cauchy-characteristic extraction (CCE) Waveforms} Jooheon Yoo, Keefe Mitman, Vijay Varma With recent improvements in the Cauchy-characteristic evolution (CCE) procedure, the CCE waveforms could soon become the new standard method of extracting gravitational waveforms at $\mathcal{I}^+$ from numerical relativity simulations. The CCE waveforms are gauge-invariant (up to BMS transformations). Unlike extrapolated waveforms, they include memory effects, which could be observed with the next-generation detectors. In this talk, we present the first surrogate model built with CCE waveforms, NRSur3dq8\_CCE. This aligned spin model is trained over the same 3-dimensional parameter space as previous model NRSur3dq8, but now with new CCE waveforms: $q \leq 8 \text{ and } \vert\chi_{1z}\vert,~ \vert\chi_{2z}\vert \leq 0.8$. To ensure that waveforms start in the same frame, we have performed BMS frame fixing on the CCE waveforms. |
Sunday, April 10, 2022 3:57PM - 4:09PM |
L16.00002: A Computationally Efficient Surrogate Model for Generating High-Accuracy Intermediate to High Mass-Ratio Inspiral Waveforms Katie Rink, Scott E Field, Kevin Gonzalez-Quesada, Tousif Islam, Gaurav Khanna, Nur-E-Mohammad Rifat, Vijay Varma Gravitational wave signals from compact astrophysical sources such as those observed by LIGO and Virgo require a high-accuracy waveform model for signal analysis. 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. We introduce reduced-order surrogate models for gravitational waveforms including several harmonic modes and with mass-ratios varying from 3 to 10,000 and with spin up to 0.8 on the primary black hole, thus vastly expanding the parameter range beyond current surrogate IMR models. Our model is trained on waveforms generated by point-particle black hole perturbation theory (ppBHPT) both for large and comparable mass-ratio binaries. We calibrate the model to spin-aligned numerical relativity simulations in the comparable mass-ratio regime. Our waveforms in the comparable mass-ratio regime agree surprisingly well with those from full numerical relativity after this calibration step. These results will enable data analysis studies in the high-mass ratio regime, including potential intermediate mass-ratio signals from LIGO/Virgo and extreme-mass ratio events of interest to the future space-based observatory LISA. |
Sunday, April 10, 2022 4:09PM - 4:21PM |
L16.00003: Error estimation and bounds for gravitational-wave surrogate models Feroz H Shaik, Scott E Field The upcoming era of high-precision gravitational wave (GW) astronomy will allow us to more accurately probe the regime of strong-field gravity from massive compact object binary systems. As the sensitivity of GW detectors continues to improve, it is expected that waveform modeling errors will begin to dominate over statistical errors. Therefore, it will be important for GW models to provide uncertainty estimates across the parameter space, thus leading to improved parameter estimation studies and more confidence in our analysis. In this talk, I will present an error estimator for surrogate models built on non-spinning numerical relativity waveforms. Our estimator accounts for the impact of noisy training data and helps identify the steps of the surrogate modeling process responsible for noise amplification. We quantify the sharpness of our error estimator through numerical examples. |
Sunday, April 10, 2022 4:21PM - 4:33PM |
L16.00004: Re-analyzing GWTC-3 events with a numerical relativity surrogate waveform model Tousif Islam, Feroz H Shaik, Carl-Johan O Haster, Vijay Varma, Scott E Field, Jacob A Lange, Richard O’Shaughnessy, Rory Smith, Avi Vajpeyi The third Gravitational-wave Transient Catalog (GWTC-3) presents a total of 90 signals detected by LIGO-Virgo Collaboration (LVC) up to the end of their third observing run. The source properties of most of the binary black holes (BBH) events have been inferred using either Numerical Relativity (NR) tuned phenomenological waveform models or NR tuned effective one-body (EOB) waveforms. We provide a re-analysis of these BBH events using a precessing numerical-relativity surrogate model, NRSur7dq4. This model is the most accurate waveform model when the analysis is restricted to the NRSur7dq4's training domain. Due to the shorter length of NRSur7dq4 waveforms, we restrict our analysis only for events that have a total mass of greater than 60 solar mass in the detector frame and mass ratios smaller than 6. While for most of the events, inferred source properties using NRSur7dq4 matches with Phenom and EOB results, we do find a handful events where NRSur7dq4 model provides tighter constrained measurements of masses and spins of the black holes, and narrower sky localization. For these events, NRSur7dq4 also recovers higher signal-to-noise ratio when compared against other models. We finally discuss the astrophysical implication of our results. |
Sunday, April 10, 2022 4:33PM - 4:45PM |
L16.00005: Advanced methods for parameter estimation of gravitational wave sources Javier Roulet Following recent developments in waveform modeling, state-of-the-art models of compact binary coalescences now incorporate higher order harmonics and generically oriented spins. These improvements increased the diversity of waveform morphologies and the parameter space dimensionality, rendering computational cost a major hurdle for parameter estimation studies. |
Sunday, April 10, 2022 4:45PM - 4:57PM |
L16.00006: A non-orthogonal wavelet transformation for reconstructing gravitational wave signals Soumen Roy Detections of gravitational-wave signals from compact binary coalescences have enabled us to study extreme astrophysical phenomena and explore fundamental physics. A crucial requisite for these studies is to have accurate signal models with characteristic morphologies, which have been challenging for many decades and are still endeavoring to incorporate important physics. Thereby, morphology-independent methods have been developed for identifying a signal and its reconstruction. The reconstructed signal allows us to test the agreement between the observed signal and the estimated theoretical waveform. These methods model observed signals using a tightest (nearly orthogonal basis) set of wavelets in the frame of continuous wavelet transformation. Here, we propose log-uniform scales to construct the wavelets, which are highly redundant (non-orthogonal) compared to the conventional octave scales but more efficient in reconstructing the signals at high frequencies. We also introduce a semi-model-dependent method for reconstructing the signals using the Gabor-Morlet wavelets with log-uniform scales. We demonstrate the ability to detect deviation using a numerical simulation of eccentric binary black holes merger, where the signal in the data does not belong to the search template waveform manifold. Finally, we apply this method to each binary black hole merger event in GWTC-1. We have found that the signal produced by the GW150914 event and its estimated theoretical waveform has an agreement at ∽ 96% level. As the detector sensitivity improves and the detected population of black hole mergers grows, we expect the proposed method will provide even stronger tests. |
Sunday, April 10, 2022 4:57PM - 5:09PM |
L16.00007: Expanding RIFT Richard W O'Shaughnessy, Jacob A Lange, Jared Wofford, Daniel Wysocki, Elizabeth Champion, Vera E Delfavero, Hannah M Gallagher The RIFT parameter inference engine provides a low-coast, iterative, scalable method to infer parameters of gravitational wave sources. In this talk, we describe and assess several updates to RIFT, several of which have already been widely applied to interpret gravitational wave observations. We discuss challenges and opportunities in using RIFT within the larger software ecosystem of gravitational wave science, including low-latency analysis, multi-stage analyses with revised data and/or multiple models, and population inference. We comment on ongoing improvements being developed in preparation for the next observing run. |
Sunday, April 10, 2022 5:09PM - 5:21PM |
L16.00008: Implementation of a generalized precession parameter in the RIFT parameter estimation algorithm Chad Henshaw Since the discovery of gravitational waves in 2015, major developments have been made towards waveform interpretation and estimation of compact binary source parameters. We discuss the implementation of the generalized precession parameter $\langle \chi_p \rangle$ within the Rapid Iterative FiTting (RIFT) parameter estimation framework. While the original precession parameter $\chi_p$ characterizes the single largest dynamical spin in a binary, $\langle \chi_p \rangle$ preserves misalignment information from both objects in the binary by averaging over all angular variations on the precession timescale. Additionally, $\langle \chi_p \rangle$ has a unique domain $1 < \langle \chi_p \rangle < 2$, which is exclusive to binaries with two precessing spins. We review the physical differences between these two parameters, and apply this new statistic to the 36 events from the second half of LIGO's third operating run (O3b). Of these, ten events show significant precession, with $\langle \chi_p \rangle > 0.5$. Of particular interest is GW191109\_010717, with a $\sim28\%$ probability that the originating system necessarily contains two misaligned spins. |
Sunday, April 10, 2022 5:21PM - 5:33PM |
L16.00009: Implementing a Dynamic Polytrope Model of Neutron Star Equation of State in BILBY Jeremy G Baier, Leslie E Wade
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