Abstract
We present the gravitational-wave background and its properties focusing on the background from compact binary coalescences in terrestrial detectors. We also introduce the standard data analysis method used to search for this background and discuss its detectability with second and third generation networks of detectors. To illustrate, we first use simple models and then discuss more realistic models based on simulations.
Highlights
Gravitational waves (GWs) were predicted by the theory of General Relativity of Albert Einstein
The analogy stops here and whether there is an orchestra conductor is another story. When people gave this definition of the gravitational-wave background, they were essentially thinking of the primordial background from inflation where a very large number of events overlap when they reach our detectors
Future CMB experiments on Earth or in space will be able to reach values of the tensor to scalar ratio of the order of r∼10−4, i.e., a gain of 2–3 orders of magnitudes compared to the current upper limit of r < 0.032 given by Planck 2018+BICEP+Keck [101]
Summary
Gravitational waves (GWs) were predicted by the theory of General Relativity of Albert Einstein. The analogy stops here and whether there is an orchestra conductor is another story When people gave this definition of the gravitational-wave background, they were essentially thinking of the primordial background from inflation where a very large number of events overlap when they reach our detectors. In this case, even if you had perfect detectors, sensitive enough to observe the small amplitude of faint and distant events, you will still never be able to resolve them individually because of the overlap. As we will see later, this is the case for the background from CBCs which is not stochastic and whose level depends on the sensitivity of the detectors
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