Detection, measurement and gravitational radiation
Jul, 199230 pages
Published in:
- Phys.Rev.D 46 (1992) 5236-5249
e-Print:
- gr-qc/9209010 [gr-qc]
Report number:
- PRINT-93-0128 (NORTHWESTERN)
View in:
Citations per year
Abstract: (arXiv)
Here I examine how to determine the sensitivity of the LIGO, VIRGO, and LAGOS gravitational wave detectors to sources of gravitational radiation by considering the process by which data are analyzed in a noisy detector. By constructing the probability that the detector output is consistent with the presence of a signal, I show how to (1) quantify the uncertainty that the output contains a signal and is not simply noise, and (2) construct the probability distribution that the signal parameterization has a certain value. From the distribution and its mode I determine volumes in parameter space such that actual signal parameters are in with probability . If we are {\em designing} a detector, or determining the suitability of an existing detector for observing a new source, then we don't have detector output to analyze but are interested in the ``most likely'' response of the detector to a signal. I exploit the techniques just described to determine the ``most likely'' volumes for detector output corresponding to the source. Finally, as an example, I apply these techniques to anticipate the sensitivity of the LIGO and LAGOS detectors to the gravitational radiation from a perturbed Kerr black hole.- gravitational radiation: measurement
- counters and detectors
- cosmological model
- numerical calculations
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