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The Big Bang Observer (BBO) is a proposed space-based gravitational-wave (GW)mission designed primarily to search for an inflation-generated GW backgroundin the frequency range 0.1-1 Hz. The major astrophysical foreground in thisrange is gravitational radiation from inspiraling compact binaries. Thisforeground is expected to be much larger than the inflation-generatedbackground, so to accomplish its main goal, BBO must be sensitive enough toidentify and subtract out practically all such binaries in the observableuniverse. It is somewhat subtle to decide whether BBO's current baseline designis sufficiently sensitive for this task, since, at least initially, thedominant noise source impeding identification of any one binary is confusionnoise from all the others. Here we present a self-consistent scheme fordeciding whether BBO's baseline design is indeed adequate for subtracting outthe binary foreground. We conclude that the current baseline should besufficient. However if BBO's instrumental sensitivity were degraded by a factor2-4, it could no longer perform its main mission. It is impossible to perfectlysubtract out each of the binary inspiral waveforms, so an important question ishow to deal with the "residual" errors in the post-subtraction data stream. Wesketch a strategy of "projecting out" these residual errors, at the cost ofsome effective bandwidth. We also provide estimates of the sizes of variouspost-Newtonian effects in the inspiral waveforms that must be accounted for inthe BBO analysis.Comment: corrects some errors in figure captions that are present in the  published versio

Big Bang Observer and the neutron-star-binary subtraction problem