Figure 15: Strain amplitude as a function of the frequency for the model populations of resolved
DDs (left panel, 10,700 objects) and AM CVn systems (right panel, 11,000 objects.). The
gray shades give the density distribution of the resolved systems normalized to the maximum density
in each panel (1,548 and 1,823 per “cell” for the double white dwarfs and AM CVn-stars panels,
respectively). The 200 strongest sources in each sample are shown as dots to enhance their visibility.
In the AM CVn panel the periods of several observed short period systems are indicated by the
vertical dotted lines. The solid line shows the average background noise due to detached white dwarfs.
The LISA sensitivities for an integration time of one year and a signal-to-noise ratio of 1 and 5 are
indicated by the dashed lines [212]. (Figure from [287].)
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