Bulletin of the American Physical Society
Mid-Atlantic Section 2022 Meeting
Volume 67, Number 20
Friday–Sunday, December 2–4, 2022; University Park, PA, Pennsylvania State University
Session B04: Gravitational Physics and Cosmology I |
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Chair: Monica Tatiana Rincon Ramirez, Pennsylvania State University Room: Pennsylvania State University Thomas 119 |
Friday, December 2, 2022 5:00PM - 5:12PM |
B04.00001: Characterizing the performance of low-latency gravitational wave detection algorithms Becca Ewing In the LIGO, Virgo, KAGRA (LVK) Collaboration there are multiple independent detection algorithms for gravitational wave signals. In order to enable rapid electromagnetic follow-up of gravitational wave candidates we must rely on detection pipelines to provide accurate results in low latency. In this context, it is important that we are able to fully characterize the performance of these searches. I will present my work in developing an integrated system to provide consistency checks on search data products using simulated signals. The system provides real time feedback on search sensitivity, accuracy of inferred signal parameters, source classification, and sky localization all conveniently visualized through web-based dashboards. I will show results of these tests on one month of replayed strain data from the third observing run using the GstLAL search pipeline. |
Friday, December 2, 2022 5:12PM - 5:24PM |
B04.00002: Thermal effects of the nuclear equation of state on binary neutron star mergers Jacob Fields Binary neutron star merger calculations often rely on a zero-temperature approximation to the equation of state. While this approximation holds well during the inspiral phase, it breaks down during the merger. Using the numerical relativity code THC_M1, we study thermal effects in binary neutron star mergers using full microphysical equations of state which differ only by their finite-temperature behavior. We present preliminary results, including gravitational waveforms and an ejecta analysis, and highlight potential observational consequences. |
Friday, December 2, 2022 5:24PM - 5:36PM |
B04.00003: Statistical Data Quality Information of LIGO Detectors and Incorporation into the Low-Latency GstLAL Analysis Rachael Huxford, Patrick Godwin, Chad R Hanna We present updates to iDQ, a statistical data quality pipeline which monitors the auxiliary states of gravitational-wave interferometers to predict the presence of transient noise in the data. We discuss the impact of incorporation of iDQ into the low-latency GstLAL analysis, a matched filter gravitational-wave search pipeline used in LIGO's third observing run. |
Friday, December 2, 2022 5:36PM - 5:48PM |
B04.00004: Metric Assisted Sampling (MASS) search for gravitational waves from binary black hole mergers Prathamesh Joshi, Chad R Hanna We present a novel gravitational wave detection algorithm that conducts a hierarchical matched filter search across the compact binary parameter space rather than relying on a fixed bank of template waveforms. This technique is competitive with standard template-bank-driven pipelines in both computational cost and sensitivity. However, the complexity of the analysis is simpler allowing for easy configuration and horizontal scaling across heterogeneous grids of computers. |
Friday, December 2, 2022 5:48PM - 6:00PM |
B04.00005: QCD Phase Transitions in Binary Neutron Star Mergers Aviral Prakash We report on signatures of high-density QCD phase transition to deconfined quarks in the context of binary neutron star mergers. We employ state-of-the-art, general relativistic hydrodynamics simulations of neutron star binaries in quasi-circular and nearly parabolic orbits. We also consider a host of equations of state that model different treatments of both hadronic matter and a 1st order phase transition to quark matter to compute gravitational wave signatures of the deconfined quark phase. |
Friday, December 2, 2022 6:00PM - 6:12PM |
B04.00006: A new AMR method in GR-Athena++ Alireza Rashti, Maitraya K Bhattacharyya, David Radice Finding analytical solution of the coupled Einstein-Euler equations in highly nonlinear regimes, for instance, around the moment of merger of two compact objects, is infeasible. As such, numerical relativity codes, like, the GR-Athena++ code, among others, are required to find the answer and get insight into the physics of these astrophysical systems. Additionally, resolving more physical features in greater details are expected from these codes, owing to enhancements in sensitivity and advent of new detectors. However, the computational resources are limited; hence, during the solve, we must adaptively decide how well different regions of the computational domain should be resolved. In other words, a good criterion for adaptive mesh refinement (AMR) is desired in order to efficiently use the resources and resolve the physics of interest. To achieve this goal, we look at the truncation error of the finite difference derivative in the GR-Athena++ code. In this method, refinement or de-refinement of a region is taking place according to this error. Here, we present some preliminary results of the new AMR for a single black hole system. |
Friday, December 2, 2022 6:12PM - 6:24PM |
B04.00007: Template bank for searches of compact binary coalesences with LIGO/VIRGO/KAGRA Shio Sakon, Leo Tsukada, Heather Fong, Chad R Hanna Matched-filtering is optimized for signal detection and is implemented in many gravitational wave (GW) detection and data analysis pipelines, including GstLAL. |
Friday, December 2, 2022 6:24PM - 6:36PM |
B04.00008: The impact of confusion noise on golden binary neutron star events in next-generation GW observatories. Luca Reali, Andrea Antonelli, Roberto Cotesta, Ssohrab Borhanian, Mesut Çaliskan, Emanuele Berti, Bangalore S Sathyaprakash Next-generation terrestrial gravitational-wave observatories will detect hundreds of thousands of signals from compact binary coalescences every year. These signals can last for several hours in the detectors' sensitivity band and they will be affected by multiple unresolved sources contributing to a confusion-noise background in the data. Using an information-matrix formalism, we estimate the impact of the confusion noise power spectral density in broadening the parameter estimates of a GW170817-like event. If our estimate of the confusion noise power spectral density is neglected, we find that masses, spins, and distance are biased in about half of our simulations under realistic circumstances. The sky localization, while still precise, can be biased in up to 80% of our simulations, potentially posing a problem in follow-up searches for electromagnetic counterparts. |
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