Pre-Phase A Report - Lisa - Nasa
Pre-Phase A Report - Lisa - Nasa
Pre-Phase A Report - Lisa - Nasa
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108 Chapter 4 Measurement Sensitivity<br />
Figure 4.8 Annual revolution of LISA configuration around the Sun, describing<br />
a cone with 60 ◦ half opening angle. One selected 2-arm interferometer is<br />
highlighted by heavier interconnecting laser beams. The “tumbling” motion<br />
of a single LISA interferometer allows the determination of the position of the<br />
source as well as of the polarisation of the wave. The (heavier) trajectory of<br />
one individual spacecraft is shown, inclined with respect to the (fainter) Earth<br />
orbit.<br />
modulation and Doppler modulation will spread a sharply peaked monochromatic signal<br />
into a set of sidebands separated from the carrier at integer multiples of the fundamental<br />
frequency (1 year) −1 . It is easy to see that the effects of the beam-pattern modulation and<br />
Doppler modulation are of roughly the same size. Consider a monochromatic signal with<br />
frequency f0. In Fourier space, the effect of the beam-pattern modulation is to spread<br />
the measured power over (roughly) a range f0 ± 2/T ,whereT is one year. (The factor<br />
of 2 arises because the beam pattern is quadrupolar.) The effect of the periodic Doppler<br />
shift coming from the detector’s center-of-mass motion is to spread the power over a<br />
range f0(1 ± v/c), where v/c ∼ 10 −4 . These two effects are therefore of roughly equal size<br />
at f0 ∼ 10 −3 Hz, which is near the center of the LISA band; beam-pattern modulation is<br />
more significant at lower frequencies and Doppler modulation is more significant at higher<br />
frequencies.<br />
In the following chapters we review the way the source position, polarisation and intrinsic<br />
amplitude are encoded in the LISA datastream. After reviewing some standard methods of<br />
parameter estimation, we then present results on how accurately these physical parameters<br />
can be determined for two LISA sources of particular interest: stellar-mass binaries and<br />
merging MBH binaries. We refer the reader to [112, 113] for more details.<br />
The beam-pattern modulation. The beam-pattern modulation can be calculated by<br />
transforming the metric-tensors<br />
h× := h×<br />
⎛<br />
⎝<br />
0 1 0<br />
1 0 0<br />
0 0 0<br />
⎞<br />
⎛<br />
⎠ and h+ := h+ ⎝<br />
1 0 0<br />
0 −1 0<br />
0 0 0<br />
⎞<br />
⎠ (4.60)<br />
3-3-1999 9:33 Corrected version 2.08