Fig. 2: Identification of SLGW events.
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. The grey-shaded areas 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 (90% confidence interval) with blue pentagrams (mean value) represent the match results of SLGWs. The graphs show the results without (top) and with (bottom) detector frame chirp mass \({{\mathcal{M}}}_{z}\ge 20\,\rm{{M}}_{\odot }\) cut. Our simulation is conducted by assuming three Cosmic Explorer detectors over 3 years.
