This appendix contains the figures for the synchrotron and IC modelling of all clusters not shown in the main text. For some of these, the IC emission peaks in SXRs or EUV above the CXB and ICM emissions, so we also show the case with γmin = 1000.
Several objects, mainly radio relics, have the peculiarity of very low thermal ICM emission, probably an underestimation by observations pointed to the cluster’s centre or by using the phenomenological model of Zandanel et al. (2014) for the gas density. In some cases (A0781, A2163, MACSJ1149, 5-2223-E and W,
MACSJ1752.0+4440-SW, PLCK G287.0+32.9-N and S), the CXB outweighs the thermal ICM emission, and in addition, the intersection point between the ASTRO-H and CXB emissions is at an energy lower than the rise in the CXB spectrum. The corresponding results for Bdt should be taken with caution, and in fact, in these cases, the signal-to-noise approach gives more conservative and reasonable results.
We also remind the reader that the signal-to-noise approach assumes a straight power law in the 20−80 keV energy band (see Sect. 7). While in most cases the cutoffs are at much lower and higher energies, for A2063 and A0013 this method could give slightly optimistic results.
All figures can be read as explained in the caption of Fig. 2.
Synchrotron and IC modelling for all clusters that are not shown in the main text. Caption as in Fig. 2.
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