7.4 The detectors

As we have mentioned earlier in Section 5, there are techniques available for the extraction of the QNM signal from the noise of the detectors [839091]. But there are still issues related to the sensitivity of the planned detectors in parts of the spectrum. For example, the QNM frequencies of stellar black holes (10 –100 M ⊙) will be of around 100 – 1000 Hz, i.e. in the frequencies where the laser interferometers are sensitive. The QNM frequencies of galactic size black holes will be detectable only from space (LISA) since their frequencies will be in the mHz regime. For the QNM frequencies of stars, there is a lack of appropriate detectors. Laser interferometers will be sensitive enough in the frequency regime of the f-mode but it will be very hard to detect signals in the frequencies of the p- and w-modes. Nevertheless, from the discussion in Section 5 it is apparent that there is a wealth of information in the signal of oscillating neutron stars, and in order to extract this information we need the p- or/and w-modes. This suggests that the ideas considering detectors, or arrays of detectors, in this high frequency regime [92] should be considered more seriously.


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