Journal
PHYSICAL REVIEW D
Volume 96, Issue 2, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.96.024058
Keywords
-
Funding
- Sherman Fairchild Foundation
- NSF [CAREER PHY-1151197, PHY-1404569, AST-1333129, PHY-1606654, PHY-0960291]
- NSF XSEDE network [TG-PHY100033]
- Direct For Computer & Info Scie & Enginr
- Office of Advanced Cyberinfrastructure (OAC) [1440050] Funding Source: National Science Foundation
- Direct For Computer & Info Scie & Enginr
- Office of Advanced Cyberinfrastructure (OAC) [1440083] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1333520] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1151197, 1404569] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1606654] Funding Source: National Science Foundation
Ask authors/readers for more resources
A generic, noneccentric binary black hole (BBH) system emits gravitational waves (GWs) that are completely described by seven intrinsic parameters: the black hole spin vectors and the ratio of their masses. Simulating a BBH coalescence by solving Einstein's equations numerically is computationally expensive, requiring days to months of computing resources for a single set of parameter values. Since theoretical predictions of the GWs are often needed for many different source parameters, a fast and accurate model is essential. We present the first surrogate model for GWs from the coalescence of BBHs including all seven dimensions of the intrinsic noneccentric parameter space. The surrogate model, which we call NRSur7dq2, is built from the results of 744 numerical relativity simulations. NRSur7dq2 covers spin magnitudes up to 0.8 and mass ratios up to 2, includes all l <= 4 modes, begins about 20 orbits before merger, and can be evaluated in similar to 50 ms. We find the largest NRSur7dq2 errors to be comparable to the largest errors in the numerical relativity simulations, and more than an order of magnitude smaller than the errors of other waveform models. Our model, and more broadly the methods developed here, will enable studies that were not previously possible when using highly accurate waveforms, such as parameter inference and tests of general relativity with GW observations.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available