(ed.). Gravitational waves (IOP, 2001)(422s).

40 Gravitational-wave detectorsLISA and Binaries in the Galaxygravitational wave amplitude10 -2010 -2110 -2210 -2310 -2310 -24Closest resolved binariesResolved binaries at GC4U1820-30confusion noise threshold (est.)LISA instrumental noise threshold(1 yr observationat S/N = 5)known close binariesknown IWDB's10 -4 10 -3 10 -2 10 -1 10 0frequency (Hz)LISA and Massive Black Holes at z=1Effective amplitudes for filtered signals from coalescing binary sytemseffective gravitational wave amplitude10 -1910 -2010 -2110 -2210 -232 x 10 7 M o2 x 10 6 M o2 x 10 5 M o2 x 10 4 M oconfusion noise threshold (est.)10 M o + 10 6 M o BH10 -4 10 -3 10 -2 10 -1 10 0frequency (Hz)LISA instrumental noise threshold(1 yr observation at S/N = 5)Figure 3.5. LISA sensitivity to binary systems in the Galaxy (top) and to massive blackhole coalescences (bottom). The top figure is calibrated in the intrinsic amplitude of thesignal, and the noise curve shows the detection threshold (5σ ) for a one-year observation.It also shows the confusion limit due to unresolved binary systems. The bottom panelshows the effective amplitude of signals from coalescences of massive black holes. Sincesome such events last less than one year, what is shown is the expected signal-to-noise ratioof the observation.polarization and amplitude of sources entirely from its own observations. Belowabout 1 mHz, this information weakens, because the wavelength of the radiationbecomes comparable to or greater than the radius of LISA’s orbit. The amplitudemodulation is the only directional information in this frequency range.