Sensitivity of a Two-Hundred-Pulsar Array to a Bounce-Frame Background

This paper asks a single question: What background amplitude could a larger, longer, quieter array reach, and would a bounce-frame contribution predicted here become detectable? Working from the published common-process amplitude of 2.4e-15 in characteristic strain at one cycle per year and the standard binary spectral index of thirteen thirds, the study computes the relevant quantities by a forecast combining pair count, span, cadence and white-noise level in the weak-signal detection integral. The headline computed values are snr_largest_array = 546.3515351859095, snr_reference_array = 28.317838900594094, gain_factor = 19.29354627320969. These values are compared throughout with the published pulsar-timing values from the North American, European, Parkes and Chinese arrays. The calculation is fully reproducible from the deposited code, and every headline number appears in the accompanying results file. This study is simulated and computed from stated assumptions; it is not a measurement, and no new timing data are presented.