Synchrotron-supported cascade spectra, including the proton synchrotron radiation components, arriving at Earth without (thin lines) and including absorption in the EBL (thick lines) for u B = 10u t (solid line), u B = 10 2 u t (dotted line), u B = 10 3 u t (dashed line), τ γγ,max = 10 −6 , and D = 10. The data points are the same as shown in Fig. 2. This figure is adapted from [6].

Contexts in source publication

Context 1

... optically thin case the standard synchrotron cooled spectra for a two-component (meson-decay and the lower energy Bethe-Heitler pairs) pair population is recovered. Changing the magnetization in the emission region has only a mild effect on the cascade fluxes, however, strongly alters the contribution from proton synchrotron radiation (see e.g., Fig. 4). Because the secondary pair distribution resulting from proton-photon interactions is fixed by the observed neutrino spectrum the corresponding synchrotron-supported cascade emission in the optically thin case is expected to be unaffected by a possible anisotropy of the collisions. In the optically thick case, τ γγ 1, the number of ...

Context 2

... Doppler factors lies at ∼ 10 55 erg/s which exceeds the Eddington luminosity of the most massive black holes known by several orders of magnitude. Furthermore, this scenario predicts a proton synchrotron flux at keVs of ∼ 10 4 times larger than the photo-pion induced emission (unless field strengths and/or Doppler factors extremely low; see Fig. 4). This is several orders of magnitude higher than any of the observed X-ray fluxes ever detected from this source. Based on these two arguments we rule out this ...