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 K09: Gravitational Wave Parameter Estimation |
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Sponsoring Units: DGRAV Chair: Colm Talbot, Massachusetts Institute of Technology Room: Conrad B/C - 2nd Floor |
Sunday, April 16, 2023 3:45PM - 3:57PM |
K09.00001: Testing new methods within RIFT for parameter inference of gravitational waves from NS binaries Anjali Balasaheb Yelikar, Vera E Delfavero, Richard O'Shaughnessy, Jacob A Lange The Rapid Iterative FiTting (RIFT) parameter inference algorithm provides a framework for efficient, highly-parallelized parameter inference for GW sources, including binary neutron stars. In this talk, I will explain new developments for the RIFT pipeline to improve the efficiency and reduce the latency of inference, including tests on BNS sources. I also comment on systematic differences that arise when different waveform models are used for inference for BNS systems. |
Sunday, April 16, 2023 3:57PM - 4:09PM |
K09.00002: A Novel Method for Placement of Numerical Relativity Simulations Informed by NR-based Parameter Estimation Jacob A Lange, Michael Boyle, Manuela Campanelli, Andrea Ceja, Deborah Ferguson, James Healy, Hector Iglesias, Aasim Z Jan, Lawrence E Kidder, Pablo Laguna, Carlos O Lousto, Geoffrey Lovelace, Erick Martinez, Ryan Nowicki, Richard O'Shaughnessy, Harald P Pfeiffer, Mark A Scheel, Deirdre M Shoemaker, Daniel Tellez, Saul A Teukolsky, Yosef Zlochower
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Sunday, April 16, 2023 4:09PM - 4:21PM |
K09.00003: Re-analyzing GWTC-3 events with a numerical relativity surrogate waveform model for precessing spin binary black holes 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 however restrict our analysis only for a set of 47 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. Furthermore, NRSur7dq4 systematically recovers higher signal-to-noise ratio when compared against other models. We finally discuss the astrophysical implication of our results. |
Sunday, April 16, 2023 4:21PM - 4:33PM |
K09.00004: Too small to fail: Measurability of sub-solar mass compact objects with gravitational waves Noah E Wolfe, Salvatore Vitale, Colm Talbot The detection of a sub-solar mass black hole could yield dramatic new insights into the nature of dark matter, as such objects lack a traditional astrophysical formation mechanism. Gravitational waves allow for the direct measurement of compact object masses during compact object mergers, and we expect the gravitational-wave signal from a low-mass coalescence to remain within the LIGO frequency band for thousands of seconds. However, the analysis of such long signals presents new data analysis challenges, and it remains unclear whether we could confidently measure the properties of a sub-solar mass compact object. To this end, we perform Bayesian parameter estimation on gravitational-wave signals from theoretical sub-solar mass compact object mergers to explore the measurability of their source properties. Using recent likelihood approximation techniques, we find that the LIGO/Virgo detectors during the upcoming O4 observing run will be able to confidently measure sub-solar component masses with signal-to-noise ratios as low as 8 and may even measure higher-order effects like spin precession. |
Sunday, April 16, 2023 4:33PM - 4:45PM |
K09.00005: Data-driven tools in gravitational wave parameter estimation and population analysis Kaze W. K. K Wong As gravitational wave (GW) detectors sensitivity improves, the rate we observe GWs increases geometrically. This demands innovations in our data analysis tools that make them capable of handling both the size and complexity of the incoming catalog of GW signals. In this talk, we present a number of new tools for different GW data analysis tasks, including a parameter estimation pipeline that is capable to converge within minutes, a flexible normalizing flow-based population analysis framework, and a code to distill information from flexible population models using symbolic regression. |
Sunday, April 16, 2023 4:45PM - 4:57PM |
K09.00006: Cosmic Explorer: a next-generation ground-based gravitational wave observatory Liu Tao Cosmic Explorer (CE) is a next-generation ground-based gravitational wave observatory envisioned to begin operations in the 2030s. With its spectacular sensitivity in the audio band CE will observe black hole and neutron star systems from the first stars, and nearer-by systems with signal to noise ratios in the thousands, while also opening a wide discovery space to the novel and unknown. The observational science possible with CE will be described, along with some of the key technologies and instrument science targeted to reach the observatory performance goals. |
Sunday, April 16, 2023 4:57PM - 5:09PM |
K09.00007: The impact of confusion noise on golden binary neutron-star events in next-generation gravitational-wave 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. |
Sunday, April 16, 2023 5:09PM - 5:21PM |
K09.00008: Binary Neutron Star Signal Confusion in Third-Generation Ground Based Gravitational Wave Detectors Aaron D Johnson, Katerina Chatziioannou In current ground-based gravitational wave detectors, LIGO, Virgo, and KAGRA, published detections all lasted a finite amount of time. These transient signals appeared at a rate of a few per week in the third observing run with each signal appearing for seconds (BBH) to minutes (BNS) in the LIGO frequency band and are therefore unlikely to overlap. With third-generation (3G) ground-based detectors such as the Einstein Telescope (ET) and Cosmic Explorer (CE), the situation changes drastically with a BNS lasting hours to over a day in 3G detectors depending on low frequency sensitivity. Further, we expect to see a BNS merge at a cadence of about one every 30 seconds, resulting in significant overlap of many signals. In this talk, we explore the overlap of many BNS systems and what implications signal confusion may have for BNS parameter estimation. |
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