Modeling the Galactic center emission from GeV to PeV
1 INFN and Dipartimento di Fisica “E. Fermi”, Università di Pisa, Largo B. Pontecorvo 3, I-56127 Pisa, Italy
2 GRAPPA Institute, University of Amsterdam, Science Park 904, 1090 GL Amsterdam, The Netherlands
3 CERN, Theory division, CH-1211 Genève 23, Switzerland
4 Instituto de Fisica Teorica (IFT) UAM/CSIC, calle N. Cabrera 13-15, 28049 Cantoblanco, Madrid, Spain
5 INFN and Dipartimento di Fisica, Università di Roma “la Sapienza”, Largo A. Moro, Roma, Italy
a e-mail: email@example.com
Published online: 23 March 2017
The H.E.S.S. collaboration recently reported a new analysis of the gamma-ray diffuse emission from a “semi-annulus” region of 1.4 × 10−4 steradiants around Sagittarius A*. The gamma-ray spectral energy distribution measured from this region suggests the presence of interacting cosmic rays at PeV energies. This analysis adds a important piece to the previous measurements obtained with Fermi-LAT, H.E.S.S. and VERITAS telescopes in this particular region of the Central Molecular Zone. Here we describe this diffuse gamma-ray emission observed around the galactic center within a comprensive model implying a cosmic-ray population with a harder spectrum in the central part of the galaxy respect to the standard scenarios. With this phenomenological model we obtain the expected diffuse gamma-ray and neutrino components for this target rich region considering the energy range from GeV to PeV. While for the gamma-ray expectations we compare the results with the data of the mentioned experiments, for the expected neutrino spectra we consider the possibility to observe the signal with Cherenkov telescopes.
© The Authors, published by EDP Sciences, 2017
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