Figure 1:
Light from a laser is split into two beams, each injected into an arm formed by pairs of freefalling mirrors. Since the length of the two arms, and , are different, now the light beams from the two arms are not recombined at one photo detector. Instead each is separately made to interfere with the light that is injected into the arms. Two distinct photo detectors are now used, and phase (or frequency) fluctuations are then monitored and recorded there. 

Figure 2:
Schematic LISA configuration. The spacecraft are labeled 1, 2, and 3. The optical paths are denoted by , where the index corresponds to the opposite spacecraft. The unit vectors point between pairs of spacecraft, with the orientation indicated. 

Figure 3:
Schematic diagram of proofmassesplusopticalbenches for a LISA spacecraft. The lefthand bench reads out the phase signals and . The righthand bench analogously reads out and . The random displacements of the two proof masses and two optical benches are indicated (lower case for the proof masses, upper case for the optical benches). 

Figure 4:
Schematic diagram of the unequalarm Michelson interferometer. The beam shown corresponds to the term in which is first sent around arm 1 followed by arm 2. The second beam (not shown) is first sent around arm 2 and then through arm 1. The difference in these two beams constitutes . 

Figure 5:
Schematic diagrams of the unequalarm Michelson, Monitor, Beacon, and Relay combinations. These TDI combinations rely only on four of the six oneway Doppler measurements, as illustrated here. 

Figure 6:
The LISA Michelson sensitivity curve (SNR = 5) and the sensitivity curve for the optimal combination of the data, both as a function of Fourier frequency. The integration time is equal to one year, and LISA is assumed to have a nominal armlength . 

Figure 7:
The optimal SNR divided by the SNR of a single Michelson interferometer, as a function of the Fourier frequency . The sensitivity gain in the lowfrequency band is equal to , while it can get larger than 2 at selected frequencies in the highfrequency region of the accessible band. The integration time has been assumed to be one year, and the proof mass and optical path noise spectra are the nominal ones. See the main body of the paper for a quantitative discussion of this point. 

Figure 8:
The SNRs of the three combinations and their sum as a function of the Fourier frequency . The SNRs of and are equal over the entire frequency band. The SNR of is significantly smaller than the other two in the low part of the frequency band, while is comparable to (and at times larger than) the SNR of the other two in the highfrequency region. See text for a complete discussion. 

Figure 9:
Apparent position of the source in the sky as seen from LISA frame for . The track of the source for a period of one year is shown on the unit sphere in the LISA reference frame. 

Figure 10:
Sensitivity curves for the observables: Michelson, , , and network for the source direction (, ). 

Figure 11:
Ratios of the sensitivities of the observables network, with for the source direction , . 
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