Robustness across simulations, resolutions, and MHD solvers

Determine whether and to what extent the inferred dependence of the intracluster-medium magnetic power spectrum on local environment and dynamics changes with simulation spatial resolution and with the choice of magnetohydrodynamic solver, using a larger body of simulations.

Background

The study analyzes one snapshot of one simulated, post-merger galaxy cluster produced with a particular adaptive-mesh-refinement cosmological simulation and MHD solver. Consequently, it does not establish whether the reported subbox-to-subbox variation of the magnetic power spectrum and its correlations with local intracluster-medium properties are robust to numerical resolution or to alternative MHD methods. The authors state that addressing this unresolved issue requires a larger set of simulations and defer that analysis to future work; they also note that such studies could include local active-galactic-nucleus contributions to Faraday rotation measures.

References

First, we focused only on a single snapshot of a single cluster, though representative of clusters where the RM observations are most likely (see Sect. \ref{sec:intro}), and did not address whether and how much our findings change with varying spatial resolution of the simulation and different MHD solvers. This requires analysis of a larger body of simulations, possibly including the local contribution of AGN to RM in clusters \citep[e.g.][]{2011ApJ...739...77X,lehle2026A&A...705A..41L}, which we defer to future work.

— Monitoring the power spectrum of magnetic field fluctuations across the simulated intracluster medium  (2609.19307 - Bartalesi et al., 16 Sep 2026) in Section 6, Conclusions