  This article analyzes the data for the five gravitational wave (GW) events
detected in Hanford(H1), Livingston(L1) and Virgo(V1) detectors by the LIGO
collaboration. It is shown that GW170814, GW170817, GW151226 and GW170104 are
very weak signals whose amplitude does not rise significantly during the GW
event, and they are indistinguishable from non-stationary detector noise. LIGO
software implements cross-correlation funcion(CCF) of H1/L1 signals with the
template reference signal, in frequency domain, in a matched filter, using 32
second windows. It is shown that this matched filter misfires with high SNR/CCF
peaks, even for very low-amplitude, short bursts of sine wave signals and
additive white gaussian noise(AWGN), all the time. It is shown that this
erratic behaviour of the matched filter, is due to the error in signal
processing operations, such as lack of cyclic prefix necessary to account for
circular convolution. It is also shown that normalized CCF method implemented
in time domain using short windows, does not have false CCF peaks for sine wave
and noise bursts. It is shown that the normalized CCF for GW151226 and
GW170104, when correlating H1/L1 and template, is indistinguishable from
correlating detector noise and the template. It is also shown that the
normalized CCF for GW151226 and GW170104, when correlating H1/L1 and template,
is indistinguishable from correlating H1/L1 and bogus chirp templates which are
frequency modulated(FM) waveforms which differ significantly from ideal
templates. Similar results are shown with LIGO matched filter, which misfires
with high Signal to Noise Ratio(SNR) for bogus chirp templates.
