English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The detection of gravitational waves and the extraction of physicalinformation from them requires the prediction of accurate waveforms to be usedin template banks. For that purpose, the accuracy of effective-one-body (EOB)waveforms has been improved over the last years by calibrating them tonumerical-relativity (NR) waveforms. So far, the calibration has employed ahandful of NR waveforms with a total length of ~30 cycles, the length beinglimited by the computational cost of NR simulations. Here we address theoutstanding problem of the stability of the EOB calibration with respect to thelength of NR waveforms. Performing calibration studies against NR waveforms ofnonspinning black-hole binaries with mass ratios 1, 1.5, 5, and 8, and with atotal length of ~60 cycles, we find that EOB waveforms calibrated againsteither 30 or 60 cycles will be indistinguishable by the advanced detectors LIGOand Virgo when the signal-to-noise ratio (SNR) is below 110. When extrapolatingto a very large number of cycles, using very conservative assumptions, we canconclude that state-of-the-art nonspinning EOB waveforms of any length aresufficiently accurate for parameter estimation with advanced detectors when theSNR is below 20, the mass ratio is below 5 and total mass is above 20 Msun. Theresults are not conclusive for the entire parameter space because of current NRerrors.

Stability of nonspinning effective-one-body model in approximating two-body dynamics and gravitational-wave emission