The SXS collaboration catalog of binary black hole simulations

Accurate models of gravitational waves from merging black holes are necessary for detectors to observe as many events as possible while extracting the maximum science. Near the time of merger, the gravitational waves from merging black holes can be computed only using numerical relativity. In this p...

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Bibliographic Details
Published in:Classical and quantum gravity 2019-10, Vol.36 (19), p.195006
Main Authors: Boyle, Michael, Hemberger, Daniel, Iozzo, Dante A B, Lovelace, Geoffrey, Ossokine, Serguei, Pfeiffer, Harald P, Scheel, Mark A, Stein, Leo C, Woodford, Charles J, Zimmerman, Aaron B, Afshari, Nousha, Barkett, Kevin, Blackman, Jonathan, Chatziioannou, Katerina, Chu, Tony, Demos, Nicholas, Deppe, Nils, Field, Scott E, Fischer, Nils L, Foley, Evan, Fong, Heather, Garcia, Alyssa, Giesler, Matthew, Hebert, Francois, Hinder, Ian, Katebi, Reza, Khan, Haroon, Kidder, Lawrence E, Kumar, Prayush, Kuper, Kevin, Lim, Halston, Okounkova, Maria, Ramirez, Teresita, Rodriguez, Samuel, Rüter, Hannes R, Schmidt, Patricia, Szilagyi, Bela, Teukolsky, Saul A, Varma, Vijay, Walker, Marissa
Format: Article
Language:English
Subjects:
black holes
gravitational waves
numerical relativity
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Summary:Accurate models of gravitational waves from merging black holes are necessary for detectors to observe as many events as possible while extracting the maximum science. Near the time of merger, the gravitational waves from merging black holes can be computed only using numerical relativity. In this paper, we present a major update of the Simulating eXtreme Spacetimes (SXS) Collaboration catalog of numerical simulations for merging black holes. The catalog contains 2018 distinct configurations (a factor of 11 increase compared to the 2013 SXS catalog), including 1426 spin-precessing configurations, with mass ratios between 1 and 10, and spin magnitudes up to 0.998. The median length of a waveform in the catalog is 39 cycles of the dominant gravitational-wave mode, with the shortest waveform containing 7.0 cycles and the longest 351.3 cycles. We discuss improvements such as correcting for moving centers of mass and extended coverage of the parameter space. We also present a thorough analysis of numerical errors, finding typical truncation errors corresponding to a waveform mismatch of   10−4. The simulations provide remnant masses and spins with uncertainties of 0.03% and 0.1% (90th percentile), about an order of magnitude better than analytical models for remnant properties. The full catalog is publicly available at www.black-holes.org/waveforms.
ISSN:0264-9381
1361-6382
DOI:10.1088/1361-6382/ab34e2