Extended Data Fig. 6: Identification of quadruple-image SLGWs in 30 years.
From: An interference-based method for the detection of strongly lensed gravitational waves
This figure shows the match between cWB’s maximum likelihood waveform and Bilby’s posterior results, as a function of SNR for quadruple-image systems. The shaded areas in grey delineate the envelope of the lower matching value between the maximum likelihood waveform of cWB and the posterior results from Bilby across all unlensed events (false positive samples). The black error bars (representing the 90% confidence interval) along with the blue pentagrams (indicating the mean value) represent the match results of SLGWs. This plot employs a cut-off of detector frame chirp mass \({{\mathcal{M}}}_{z}\ge 20M\odot\).
