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Fig. 6


Orbital period (left panels) and spin-down power distribution (right panels) of a random sample of 105 systems. Top panels show the full population as a light blue histogram with the line-filled fraction showing the distribution of the binaries that are accreting according to Eq. (4). The bottom panels zoom in to highlight the systems detected in any of the present-day surveys (combining the H.E.S.S., 3FGL, and FAVA-like surveys; medium blue histogram) or any of the future surveys (combining the full CTA, extended 3FGL, and HAWC-like surveys, dark blue histogram). The latter essentially shows the systems detected in any survey since a binary detected in one of the present-day surveys has a nearly >99% chance of being re-detected in one of the future surveys.

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