Diffuse Galactic gamma-ray emission

There are two main ideas to explain the origin of these flares: (i) ‘late internal shocks’ (Burrows et al. 2006) associated with a long-lived central engine and (ii)

Since the later time afterglow is radiated from a shocked ambient medium (i.e., a blast wave), rather than the original ejecta from the central engine which powers GRB events, it

An example of a future gamma-ray astronomy analysis that pursues this approach is provided by combining uniformed high-level data from a gamma-ray satellite and four

In this report, we consider a model of the Fermi bubbles at low latitudes derived with the assumption that their spectrum is the same at low latitudes as at high latitudes and

The radio pulse components of millisecond pulsars, which lag the main high-energy peak, or roughly coincide with it, are suggested to result from induced scattering of the pulsar

For three hard X-ray diffuse source categories, namely non-thermal X- ray filaments (§5), molecular clouds (§6) and the cen- tral 10 parsec region around Sgr A* (§7), we present

Top row: data points show the separately fitted spectra for the bubble interior and outer shell templates (as defined in Figure 15 ), with the template for the disk IC emission given

Abstract —The GAMMA-400 γ-ray telescope installed at the Russian space observatory is intended for precision measurements in the energy range of 20 MeV–1000 GeV of γ-ray emission