Simulating the Rotation Measure Sky from Primordial Magnetic Fields

This paper presents a novel approach to studying Primordial Magnetic Fields (PMFs) by simulating their imprints on the mean rotation measure (RM) originating in the intergalactic medium (IGM). Using cosmological simulations coupled with light-cone analysis, the authors introduce a new method for producing full-sky RMIGM distributions and analyze the autocorrelation of RMIGM on small and large angular scales. The results show that PMF structures indeed exhibit distinct signatures in the RM sky. The large-scale uniform model leads to correlations up to 90 degrees, while correlations for small-scale stochastic PMF models drop significantly at small angular scales. The study also compares the simulated RMIGM redshift dependence with that from the LOFAR Two-metre Sky Survey, showing agreement with previous upper limits' estimates on the PMF strength. These findings suggest that improvements in the modeling of Galactic RM will be necessary to investigate the signature of large-scale correlated PMFs. Future research should focus on refining the simulations and developing new observational techniques to better isolate the signatures of PMFs in the rotation measure sky.

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