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 [83,
90,
91]. 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 () 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.