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The Fermi Galactic Center GeV Excess and Implications for Dark Matter
Vise andre og tillknytning
2017 (engelsk)Inngår i: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 840, nr 1, artikkel-id 43Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

The region around the Galactic Center (GC) is now well established to be brighter at energies of a few GeV than what is expected from conventional models of diffuse gamma-ray emission and catalogs of known gamma-ray sources. We study the GeV excess using 6.5 yr of data from the Fermi Large Area Telescope. We characterize the uncertainty of the GC excess spectrum and morphology due to uncertainties in cosmic-ray source distributions and propagation, uncertainties in the distribution of interstellar gas in the Milky Way, and uncertainties due to a potential contribution from the Fermi bubbles. We also evaluate uncertainties in the excess properties due to resolved point sources of gamma rays. The GC is of particular interest, as it would be expected to have the brightest signal from annihilation of weakly interacting massive dark matter (DM) particles. However, control regions along the Galactic plane, where a DM signal is not expected, show excesses of similar amplitude relative to the local background. Based on the magnitude of the systematic uncertainties, we conservatively report upper limits for the annihilation cross-section as a function of particle mass and annihilation channel.

sted, utgiver, år, opplag, sider
Institute of Physics Publishing , 2017. Vol. 840, nr 1, artikkel-id 43
Emneord [en]
cosmic rays, Galaxy: bulge, Galaxy: center, Galaxy: halo, gamma rays: general, ISM: general
HSV kategori
Identifikatorer
URN: urn:nbn:se:kth:diva-216505DOI: 10.3847/1538-4357/aa6cabISI: 000403223600002Scopus ID: 2-s2.0-85019104376OAI: oai:DiVA.org:kth-216505DiVA, id: diva2:1165152
Merknad

Funding details: NNH13ZDA001N, NASA, National Aeronautics and Space Administration; Funding details: NNX14AQ37G, NASA, National Aeronautics and Space Administration; Funding text: This work was partially funded by NASA grants NNX14AQ37G and NNH13ZDA001N.

QC 20171212

Tilgjengelig fra: 2017-12-12 Laget: 2017-12-12 Sist oppdatert: 2017-12-12bibliografisk kontrollert

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