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Challenges in Explaining the Galactic Center Gamma-Ray Excess with Millisecond Pulsars
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Challenges in Explaining the Galactic Center Gamma-Ray Excess with Millisecond Pulsars
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Millisecond pulsars have been discussed as a possible source of the gamma-ray excess observed from the region surrounding the Galactic Center. With this in mind, we use the observed population of bright low-mass X-ray binaries to estimate the number of millisecond pulsars in the Inner Galaxy. This calculation suggests that only ~1-5% of the excess is produced by millisecond pulsars. We also use the luminosity function derived from local measurements of millisecond pulsars, along with the number of point sources resolved by Fermi, to calculate an upper limit for the diffuse emission from such a population. While this limit is compatible with the millisecond pulsar population implied by the number of low-mass X-ray binaries, it strongly excludes the possibility that most of the excess originates from such objects.
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Cited by 1 Pith paper
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Galactic Center gamma-ray excess from a generic triaxial halo
Fermi-LAT fits show the Galactic Center gamma-ray excess keeps its spectrum and cuspiness under triaxial/tilted dark matter halo templates, but its morphology prefers a flipped-tilt halo and disfavors a stellar-halo profile.
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