SIGNAL ANALYSIS OF GRAVITATIONAL-WAVE TAILS

The tails of gravitational waves result from the non-linear interactio n between the usual quadrupole radiation generated by an isolated syst em (with total mass-energy M), and the static monopole field associate d with M. Their contributions to the field at large distances from the system include a particular effect of modulation of the phase in the Fourier domain, having M as a factor and depending on the frequency as similar to omega ln omega . In this paper we investigate the level at which this tail effect could be detected in future laser interferomet ric detectors. We consider a family of matched filters of inspiralling compact binary signals, allowing for this effect and parametrized by a family of independent 'test' parameters including M. Detecting the e ffect is equivalent to attributing, by optimal signal processing, a no n-zero value to M. The 1-sigma error bar in the measurement of M is co mputed by analytical and numerical methods as a function of the optima l signal-to-noise ratio (SNR). We find that the minimal values of the SNR for detection of the tail effect at the 1-sigma level range from s imilar to 100 to similar to 2800 for neutron-star binaries (depending on the type of noise in the detector and on our a priori knowledge of the binary), and from similar to 15 to similar to 400 for a black-hole binary with M = 20M.. It is argued that some of these values, at leas t for black-hole binaries, could be achieved in future generations of detectors, following the currently planned VIRGO and LIGO detectors.