Diffuse neutrino flux from relativistic reconnection in AGN coronae

Open Access

Fig. D.1.

Same as Fig. 1 except that lines are color coded based on the bolometric X-ray luminosity (panel a), the redshift z (panel b) and on the magnetic field (panel c) of AGN as indicated by the inset legend. Panel d shows the exact same calculation as in Fig. 1 but for σ_p extending up to 10⁶.

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