Cherenkov Telescope Array sensitivity to the putative millisecond pulsar population responsible for the Galactic Centre excess

Macias, Oscar; van Leijen, Harm; Song, Deheng; Ando, Shin’ichiro; Horiuchi, Shunsaku; Crocker, Roland M.

doi:10.1093/mnras/stab1450

Title: Cherenkov Telescope Array sensitivity to the putative millisecond pulsar population responsible for the Galactic Centre excess

Journal Article · Fri May 21 00:00:00 EDT 2021 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stab1450· OSTI ID:1808354

^[1]; van Leijen, Harm ^[2];

^[3]; Ando, Shin’ichiro ^[1]; Horiuchi, Shunsaku ^[3];

^[4]

Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa, Chiba 277-8583, Japan, GRAPPA Institute, Institute of Physics, University of Amsterdam, NL-1098 XH Amsterdam, the Netherlands
GRAPPA Institute, Institute of Physics, University of Amsterdam, NL-1098 XH Amsterdam, the Netherlands
Center for Neutrino Physics, Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA
Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia

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. Furthermore, 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 ≳158 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^±.

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Research Organization:: Virginia Polytechnic Inst. and State Univ. (Virginia Tech), Blacksburg, VA (United States)

Sponsoring Organization:: USDOE

Grant/Contract Number:: SC0020262

OSTI ID:: 1808354

Alternate ID(s):: OSTI ID: 1837492

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Vol. 506 Journal Issue: 2; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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