2015/02/28 by Jonathan Blackman, Scott E. Field, Chad R. Galley +4
Physics and Astronomy · Computer Science · #gr-qc #astro-ph.HE #cs.CE #physics.data-an
paper · pdf · doi:10.1103/physrevlett.115.121102
published as Phys. Rev. Lett. 115, 121102 (2015) · Updated to published version, which includes a section comparing the surrogate and effective-one-body models. The surrogate is publicly available for download at http://www.black-holes.org/surrogates/ . 6 pages, 6 figures
arxiv created 2015/10/07 · arxiv updated 2015/10/09
Simulating a binary black hole (BBH) coalescence by solving Einstein's equations is computationally expensive, requiring days to months of supercomputing time. Using reduced order modeling techniques, we construct an accurate surrogate model, which is evaluated in a millisecond to a second, for numerical relativity (NR) waveforms from non-spinning BBH coalescences with mass ratios in [1, 10] and durations corresponding to about 15 orbits before merger. We assess the model's uncertainty and show that our modeling strategy predicts NR waveforms \em not used for the surrogate's training with errors nearly as small as the numerical error of the NR code. Our model includes all spherical-harmonic -2Yℓ m waveform modes resolved by the NR code up to ℓ=8. We compare our surrogate model to Effective One Body waveforms from 50-300 M_\odot for advanced LIGO detectors and find that the surrogate is always more faithful (by at least an order of magnitude in most cases).