Abstract
In the recent paper of Hooper and Goodenough (2010) [10] it was reported that γ-ray emission from the Galactic Center region contains an excess compared to the contributions from the large-scale diffuse emission and known point sources. This excess was argued to be consistent with a signal from annihilation of Dark Matter with a power law density profile. We reanalyze the Fermi data and find instead that it is consistent with the “standard model” of diffuse emission and of known point sources. The main reason for the discrepancy with the interpretation of Hooper and Goodenough (2010) [10] is different (as compared to the previous works) spectrum of the point source at the Galactic Center assumed by Hooper and Goodenough (2010) [10]. We discuss possible reasons for such an interpretation.
Highlights
The origin of the emission from the Galactic Center (GC) at keV–TeV energies has been extensively discussed in the literature over last few years
We fix the positions of the sources to coordinates given in the catalog. We model their spectra as power law
The spectrum of the central point source (1FGL J1745.62900c, probably associated with the Galactic black hole Sgr A∗) was taken in HG10 to be a featureless power-law starting from energies about 10 TeV (results of HESS measurements, blue points with error bars in Fig. 2, (Aharonian et al 2004; van Eldik et al 2008)) and continuing all the way down to ∼ 1 GeV
Summary
The origin of the emission from the Galactic Center (GC) at keV–TeV energies has been extensively discussed in the literature over last few years. To describe the diffuse component of emission, we use the models for the Galactic diffuse emission (gll iem v02.fit) and isotropic (isotropic iem v002.txt) backgrounds that were developed by the LAT team and recommended for the high-level analysis (Abdo et al 2010b). To describe the diffuse component of emission, we use the models for the Galactic diffuse emission (gll iem v02.fit) and isotropic (isotropic iem v002.txt) backgrounds that were developed by the LAT team and recommended for the high-level analysis (Abdo et al 2010b)2 These models describe contributions from galactic and extragalactic diffuse. Continuation of the HESS data (van Eldik et al 2008; Aharonian et al 2004) (blue points) data with a power law is shown with dashed black line
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