%AMacias, Oscar%Avan Leijen, Harm%ASong, Deheng%AAndo, Shin’ichiro%AHoriuchi, Shunsaku%ACrocker, Roland%Anull Ed.%BJournal Name: Monthly Notices of the Royal Astronomical Society; Journal Volume: 506; Journal Issue: 2 %D2021%I %JJournal Name: Monthly Notices of the Royal Astronomical Society; Journal Volume: 506; Journal Issue: 2 %K %MOSTI ID: 10279272 %PMedium: X %TCherenkov Telescope Array sensitivity to the putative millisecond pulsar population responsible for the Galactic Centre excess %XABSTRACT The leading explanation of the Fermi Galactic Centre γ-ray excess is the extended emission from an unresolved population of millisecond pulsars (MSPs) in the Galactic bulge. Such a population would, along with the prompt γ-rays, also inject large quantities of electrons/positrons (e±) into the interstellar medium. These e± could potentially inverse-Compton (IC) scatter ambient photons into γ-rays that fall within the sensitivity range of the upcoming Cherenkov Telescope Array (CTA). In this article, we examine the detection potential of CTA to this signature by making a realistic estimation of the systematic uncertainties on the Galactic diffuse emission model at TeV-scale γ-ray energies. We forecast that, in the event that e± injection spectra are harder than E−2, CTA has the potential to robustly discover the IC signature of a putative Galactic bulge MSP population sufficient to explain the Galactic Centre excess for e± injection efficiencies in the range of ≈2.9–74.1 per cent, or higher, depending on the level of mismodelling of the Galactic diffuse emission components. On the other hand, for spectra softer than E−2.5, a reliable CTA detection would require an unphysically large e± injection efficiency of ${\gtrsim} 158{{\ \rm per\ cent}}$. However, even this pessimistic conclusion may be avoided in the plausible event that MSP observational and/or modelling uncertainties can be reduced. We further find that, in the event that an IC signal were detected, CTA can successfully discriminate between an MSP and a dark matter origin for the radiating e±. %0Journal Article