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- W4384156056 abstract "ABSTRACT We use Fermi-LAT data to analyse the faint gamma-ray source located at the centre of the Sagittarius (Sgr) dwarf spheroidal galaxy. In the 4FGL-DR3 catalogue, this source is associated with the globular cluster, M54. We investigate the spectral energy distribution and spatial extension of this source, with the goal of testing two hypotheses: (1) the emission is due to millisecond pulsars within M54, or (2) the emission is due to annihilating dark matter from the Sgr halo. For the pulsar interpretation, we consider a two-component model which describes both the lower-energy magnetospheric emission and possible high-energy emission arising from inverse Compton scattering. We find that this source has a point-like morphology at low energies, consistent with magnetospheric emission, and find no evidence for a higher-energy component. For the dark matter interpretation, we find the signal favours a dark matter mass of mχ = 29.6 ± 5.8 GeV and an annihilation cross section of $sigma v = (2.1 pm 0.59) times 10^{-26} , text{cm}^3$ s−1 for the $b bar{b}$ channel (or mχ = 8.3 ± 3.8 GeV and $sigma v = (0.90 pm 0.25) times 10^{-26} , text{cm}^3$ s−1 for the τ+τ− channel), when adopting a J-factor of $J=10^{19.6} , text{GeV}^2 , text{cm}^{-5}$. This parameter space is consistent with gamma-ray constraints from other dwarf galaxies and with dark matter interpretations of the Galactic Centre Gamma-Ray Excess." @default.
- W4384156056 created "2023-07-14" @default.
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- W4384156056 date "2023-07-13" @default.
- W4384156056 modified "2023-09-27" @default.
- W4384156056 title "On the gamma-ray emission from the core of the Sagittarius dwarf galaxy" @default.
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- W4384156056 doi "https://doi.org/10.1093/mnras/stad2074" @default.
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